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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Strauss%2C+R&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Strauss%2C+R&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Strauss%2C+R&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.04471">arXiv:2501.04471</a> <span> [<a href="https://arxiv.org/pdf/2501.04471">pdf</a>, <a href="https://arxiv.org/format/2501.04471">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Decoupling Pulse Tube Vibrations from a Dry Dilution Refrigerator at milli-Kelvin Temperatures </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=The+NUCLEUS+collaboration"> The NUCLEUS collaboration</a>, <a href="/search/physics?searchtype=author&query=Wex%2C+A">A. Wex</a>, <a href="/search/physics?searchtype=author&query=Rothe%2C+J">J. Rothe</a>, <a href="/search/physics?searchtype=author&query=Peters%2C+L">L. Peters</a>, <a href="/search/physics?searchtype=author&query=Abele%2C+H">H. Abele</a>, <a href="/search/physics?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/physics?searchtype=author&query=Arnold%2C+B">B. Arnold</a>, <a href="/search/physics?searchtype=author&query=Corona%2C+M+A">M. Atzori Corona</a>, <a href="/search/physics?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/physics?searchtype=author&query=Bossio%2C+E">E. Bossio</a>, <a href="/search/physics?searchtype=author&query=Burkhart%2C+J">J. Burkhart</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=Cappella%2C+F">F. Cappella</a>, <a href="/search/physics?searchtype=author&query=Cappelli%2C+M">M. Cappelli</a>, <a href="/search/physics?searchtype=author&query=Casali%2C+N">N. Casali</a>, <a href="/search/physics?searchtype=author&query=Cerulli%2C+R">R. Cerulli</a>, <a href="/search/physics?searchtype=author&query=Cruciani%2C+A">A. Cruciani</a>, <a href="/search/physics?searchtype=author&query=Del+Castello%2C+G">G. Del Castello</a>, <a href="/search/physics?searchtype=author&query=Roccagiovine%2C+M+d+G">M. del Gallo Roccagiovine</a>, <a href="/search/physics?searchtype=author&query=Doblhammer%2C+A">A. Doblhammer</a>, <a href="/search/physics?searchtype=author&query=Dorer%2C+S">S. Dorer</a>, <a href="/search/physics?searchtype=author&query=Erhart%2C+A">A. Erhart</a>, <a href="/search/physics?searchtype=author&query=Friedl%2C+M">M. Friedl</a>, <a href="/search/physics?searchtype=author&query=Fichtinger%2C+S">S. Fichtinger</a>, <a href="/search/physics?searchtype=author&query=Garai%2C+A">A. Garai</a> , et al. (43 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.04471v1-abstract-short" style="display: inline;"> With the rising adoption of dry dilution refrigerators across scientific and industrial domains, there has been a pressing demand for highly efficient vibration decoupling systems capable of operation at cryogenic temperatures in order to achieve the low vibration levels required for operation of sensitive equipment like cryogenic detectors or quantum devices. As part of the NUCLEUS experiment, a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.04471v1-abstract-full').style.display = 'inline'; document.getElementById('2501.04471v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.04471v1-abstract-full" style="display: none;"> With the rising adoption of dry dilution refrigerators across scientific and industrial domains, there has been a pressing demand for highly efficient vibration decoupling systems capable of operation at cryogenic temperatures in order to achieve the low vibration levels required for operation of sensitive equipment like cryogenic detectors or quantum devices. As part of the NUCLEUS experiment, a cryogenic spring pendulum has been engineered to effectively isolate pulse tube vibrations by establishing an autonomous frame of reference for the experimental volume, while sustaining temperatures below 10 mK. Attaining attenuation of up to two orders of magnitude within the region of interest of the NUCLEUS cryogenic detectors, we achieved displacement RMS values in the order of 1 nm in the axial direction and 100 pm radially, thereby reducing vibrations below typical environmental levels. Our successful detector operation across multiple cooldown cycles demonstrated negligible sensitivity to pulse tube induced vibrations, culminating in the achievement of an ultra-low $(6.22 \pm 0.07)$ eV baseline resolution on a gram-scale CaWO$_4$ cryogenic calorimeter during continuous pulse tube operation over the course of several weeks. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.04471v1-abstract-full').style.display = 'none'; document.getElementById('2501.04471v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.13256">arXiv:2411.13256</a> <span> [<a href="https://arxiv.org/pdf/2411.13256">pdf</a>, <a href="https://arxiv.org/ps/2411.13256">ps</a>, <a href="https://arxiv.org/format/2411.13256">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-ph</span> </div> </div> <p class="title is-5 mathjax"> Prevention of resistive wall tearing mode major disruptions with feedback </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Strauss%2C+H+R">H. R. Strauss</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.13256v2-abstract-short" style="display: inline;"> Resistive wall tearing modes (RWTM) can cause major disruptions. A signature of RWTMs is that the rational surface is sufficiently close to the wall. For $(m,n) = (2,1)$ modes, at normalized minor radius $蟻= 0.75$, the value of $q$ is $q_{75} < 2.$ This is confirmed in simulations and theory and in a DIII-D locked mode disruption database. The $q_{75} < 2$ criterion is valid at high $尾$ as well as… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.13256v2-abstract-full').style.display = 'inline'; document.getElementById('2411.13256v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.13256v2-abstract-full" style="display: none;"> Resistive wall tearing modes (RWTM) can cause major disruptions. A signature of RWTMs is that the rational surface is sufficiently close to the wall. For $(m,n) = (2,1)$ modes, at normalized minor radius $蟻= 0.75$, the value of $q$ is $q_{75} < 2.$ This is confirmed in simulations and theory and in a DIII-D locked mode disruption database. The $q_{75} < 2$ criterion is valid at high $尾$ as well as at low $尾.$ A very important feature of RWTMs is that they produce major disruptions only when the $q_{75} < 2$ criterion is satisfied. If it is not satisfied, or if the wall is ideally conducting, then the mode does not produce a major disruption, although it can produce a minor disruption. Feedback, or rotation of the mode at the wall by complex feedback, can emulate an ideal wall, preventing major disruptions. The $q_{75}$ criterion is analyzed in a linear simulations, and a simple geometric model is given. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.13256v2-abstract-full').style.display = 'none'; document.getElementById('2411.13256v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.05765">arXiv:2406.05765</a> <span> [<a href="https://arxiv.org/pdf/2406.05765">pdf</a>, <a href="https://arxiv.org/format/2406.05765">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> A detailed survey of the parallel mean free path of solar energetic particle protons and electrons </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Lang%2C+J+T">J. T. Lang</a>, <a href="/search/physics?searchtype=author&query=Strauss%2C+R+D">R. D. Strauss</a>, <a href="/search/physics?searchtype=author&query=Engelbrecht%2C+N+E">N. E. Engelbrecht</a>, <a href="/search/physics?searchtype=author&query=Berg%2C+J+P+v+d">J. P. van den Berg</a>, <a href="/search/physics?searchtype=author&query=Dresing%2C+N">N. Dresing</a>, <a href="/search/physics?searchtype=author&query=Ruffolo%2C+D">D. Ruffolo</a>, <a href="/search/physics?searchtype=author&query=Bandyopadhyay%2C+R">R. Bandyopadhyay</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.05765v1-abstract-short" style="display: inline;"> In this work, more than a dozen solar energetic particle (SEP) events are identified where the source region is magnetically well-connected to at least one spacecraft at 1~au. The observed intensity-time profiles, for all available proton and electron energy channels, are compared to results computed using a numerical 1D SEP transport model in order to derive the parallel mean free paths (pMFPs) a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05765v1-abstract-full').style.display = 'inline'; document.getElementById('2406.05765v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.05765v1-abstract-full" style="display: none;"> In this work, more than a dozen solar energetic particle (SEP) events are identified where the source region is magnetically well-connected to at least one spacecraft at 1~au. The observed intensity-time profiles, for all available proton and electron energy channels, are compared to results computed using a numerical 1D SEP transport model in order to derive the parallel mean free paths (pMFPs) as a function of energy (or rigidity) at 1~au. These inversion results are then compared to theoretical estimates of the pMFP, using observed turbulence quantities with observationally-motivated variations as input. For protons, a very good comparison between inversion and theoretical results is obtained. It is shown that the observed inter-event variations in the inversion pMFP values can be explained by natural variations in the background turbulence values. For electrons, there is relatively good agreement with pMFPs derived assuming the damping model of dynamical turbulence, although the theoretical values are extremely sensitive to the details of the turbulence dissipation range which themselves display a high level of variation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05765v1-abstract-full').style.display = 'none'; document.getElementById('2406.05765v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.02607">arXiv:2404.02607</a> <span> [<a href="https://arxiv.org/pdf/2404.02607">pdf</a>, <a href="https://arxiv.org/format/2404.02607">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> DoubleTES detectors to investigate the CRESST low energy background: results from above-ground prototypes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/physics?searchtype=author&query=Banik%2C+S">S. Banik</a>, <a href="/search/physics?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/physics?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/physics?searchtype=author&query=Bertolini%2C+A">A. Bertolini</a>, <a href="/search/physics?searchtype=author&query=Breier%2C+R">R. Breier</a>, <a href="/search/physics?searchtype=author&query=Bucci%2C+C">C. Bucci</a>, <a href="/search/physics?searchtype=author&query=Burkhart%2C+J">J. Burkhart</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=D%27Addabbo%2C+A">A. D'Addabbo</a>, <a href="/search/physics?searchtype=author&query=Di+Lorenzo%2C+S">S. Di Lorenzo</a>, <a href="/search/physics?searchtype=author&query=Einfalt%2C+L">L. Einfalt</a>, <a href="/search/physics?searchtype=author&query=Erb%2C+A">A. Erb</a>, <a href="/search/physics?searchtype=author&query=Feilitzsch%2C+F+v">F. v. Feilitzsch</a>, <a href="/search/physics?searchtype=author&query=Fichtinger%2C+S">S. Fichtinger</a>, <a href="/search/physics?searchtype=author&query=Fuchs%2C+D">D. Fuchs</a>, <a href="/search/physics?searchtype=author&query=Garai%2C+A">A. Garai</a>, <a href="/search/physics?searchtype=author&query=Ghete%2C+V+M">V. M. Ghete</a>, <a href="/search/physics?searchtype=author&query=Gorla%2C+P">P. Gorla</a>, <a href="/search/physics?searchtype=author&query=Guillaumon%2C+P+V">P. V. Guillaumon</a>, <a href="/search/physics?searchtype=author&query=Gupta%2C+S">S. Gupta</a>, <a href="/search/physics?searchtype=author&query=Hauff%2C+D">D. Hauff</a>, <a href="/search/physics?searchtype=author&query=Je%C5%A1kovsk%C3%BD%2C+M">M. Je拧kovsk媒</a>, <a href="/search/physics?searchtype=author&query=Jochum%2C+J">J. Jochum</a>, <a href="/search/physics?searchtype=author&query=Kaznacheeva%2C+M">M. Kaznacheeva</a> , et al. (33 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.02607v1-abstract-short" style="display: inline;"> In recent times, the sensitivity of low-mass direct dark matter searches has been limited by unknown low energy backgrounds close to the energy threshold of the experiments known as the low energy excess (LEE). The CRESST experiment utilises advanced cryogenic detectors constructed with different types of crystals equipped with Transition Edge Sensors (TESs) to measure signals of nuclear recoils i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.02607v1-abstract-full').style.display = 'inline'; document.getElementById('2404.02607v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.02607v1-abstract-full" style="display: none;"> In recent times, the sensitivity of low-mass direct dark matter searches has been limited by unknown low energy backgrounds close to the energy threshold of the experiments known as the low energy excess (LEE). The CRESST experiment utilises advanced cryogenic detectors constructed with different types of crystals equipped with Transition Edge Sensors (TESs) to measure signals of nuclear recoils induced by the scattering of dark matter particles in the detector. In CRESST, this low energy background manifests itself as a steeply rising population of events below 200 eV. A novel detector design named doubleTES using two identical TESs on the target crystal was studied to investigate the hypothesis that the events are sensor-related. We present the first results from two such modules, demonstrating their ability to differentiate between events originating from the crystal's bulk and those occurring in the sensor or in its close proximity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.02607v1-abstract-full').style.display = 'none'; document.getElementById('2404.02607v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 13 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.07133">arXiv:2401.07133</a> <span> [<a href="https://arxiv.org/pdf/2401.07133">pdf</a>, <a href="https://arxiv.org/ps/2401.07133">ps</a>, <a href="https://arxiv.org/format/2401.07133">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-ph</span> </div> </div> <p class="title is-5 mathjax"> Resistive Wall Tearing Mode Disruptions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Strauss%2C+H+R">H. R. Strauss</a>, <a href="/search/physics?searchtype=author&query=Chapman%2C+B+E">B. E. Chapman</a>, <a href="/search/physics?searchtype=author&query=Lyons%2C+B+C">B. C. Lyons</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.07133v1-abstract-short" style="display: inline;"> This paper deals with resistive wall tearing mode (RWTM) disruptions. RWTMs are closely related to resistive wall modes (RWMs). The nonlinear behavior of these modes is strongly dependent on the resistive wall outside the plasma. A conducting wall is highly mitigating for RWTM disruptions. The consequence for ITER, which has a highly conducting wall, is that the thermal quench (TQ) time could be m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.07133v1-abstract-full').style.display = 'inline'; document.getElementById('2401.07133v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.07133v1-abstract-full" style="display: none;"> This paper deals with resistive wall tearing mode (RWTM) disruptions. RWTMs are closely related to resistive wall modes (RWMs). The nonlinear behavior of these modes is strongly dependent on the resistive wall outside the plasma. A conducting wall is highly mitigating for RWTM disruptions. The consequence for ITER, which has a highly conducting wall, is that the thermal quench (TQ) time could be much longer than previously conjectured. Active feedback stabilization is another possible way to mitigate or prevent RWTM disruptions. Simulations of disruptions are reviewed for DIII-D and MST. MST has a longer resistive wall time than ITER, and disruptions are not observed experimentally when MST is operated as a standard tokamak. Simulations indicate that the RWTM disruption time scale is longer than the experimental shot time. In general, edge cooling by tearing mode island overlap or by impurity radiation causes contraction of the current profile, which destabilizes RWTMs. The equilibria studied here have a q = 2 rational surface close to the edge of the plasma, and low edge current density. A sequence of low edge current model equilibria hasmajor disruptions only for a resistive, not ideal, wall, and approximately edge q < 3. This is consistent with typical regimes of tokamak disruption avoidance, suggesting that typical tokamak disruptions could be RWTMs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.07133v1-abstract-full').style.display = 'none'; document.getElementById('2401.07133v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.02969">arXiv:2401.02969</a> <span> [<a href="https://arxiv.org/pdf/2401.02969">pdf</a>, <a href="https://arxiv.org/format/2401.02969">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Jovian electrons in the inner heliosphere: Opportunities for Multi-spacecraft Observations and Modeling </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Strauss%2C+R+D">R. D. Strauss</a>, <a href="/search/physics?searchtype=author&query=Dresing%2C+N">N. Dresing</a>, <a href="/search/physics?searchtype=author&query=Engelbrecht%2C+N+E">N. E. Engelbrecht</a>, <a href="/search/physics?searchtype=author&query=Mitchell%2C+J+G">J. G. Mitchell</a>, <a href="/search/physics?searchtype=author&query=K%C3%BChl%2C+P">P. K眉hl</a>, <a href="/search/physics?searchtype=author&query=Jensen%2C+S">S. Jensen</a>, <a href="/search/physics?searchtype=author&query=Fleth%2C+S">S. Fleth</a>, <a href="/search/physics?searchtype=author&query=S%C3%A1nchez-Cano%2C+B">B. S谩nchez-Cano</a>, <a href="/search/physics?searchtype=author&query=Posner%2C+A">A. Posner</a>, <a href="/search/physics?searchtype=author&query=Rankin%2C+J+S">J. S Rankin</a>, <a href="/search/physics?searchtype=author&query=Lee%2C+C+O">C. O. Lee</a>, <a href="/search/physics?searchtype=author&query=Berg%2C+J+P+v+d">J. P. van den Berg</a>, <a href="/search/physics?searchtype=author&query=Ferreira%2C+S+E+S">S. E. S. Ferreira</a>, <a href="/search/physics?searchtype=author&query=Heber%2C+B">B. Heber</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.02969v1-abstract-short" style="display: inline;"> In this paper we explore the idea of using multi-spacecraft observations of Jovian electrons to measure the 3D distribution of these particles in the inner heliosphere. We present simulations of Jovian electron intensities along selected spacecraft trajectories for 2021 and compare these, admittedly qualitatively, to these measurements. Using the data-model comparison we emphasize how such a study… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.02969v1-abstract-full').style.display = 'inline'; document.getElementById('2401.02969v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.02969v1-abstract-full" style="display: none;"> In this paper we explore the idea of using multi-spacecraft observations of Jovian electrons to measure the 3D distribution of these particles in the inner heliosphere. We present simulations of Jovian electron intensities along selected spacecraft trajectories for 2021 and compare these, admittedly qualitatively, to these measurements. Using the data-model comparison we emphasize how such a study can be used to constrain the transport parameters in the inner heliosphere, and how this can lead to additional insight into energetic particle transport. Model results are also shown along the expected trajectories of selected spacecraft, including the off-ecliptic phase of the Solar Orbiter mission from 2025 onward. Lastly, we revisit the use of historical data and discuss upcoming missions that may contribute to Jovian electron measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.02969v1-abstract-full').style.display = 'none'; document.getElementById('2401.02969v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.15147">arXiv:2311.15147</a> <span> [<a href="https://arxiv.org/pdf/2311.15147">pdf</a>, <a href="https://arxiv.org/format/2311.15147">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Optimal operation of cryogenic calorimeters through deep reinforcement learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/physics?searchtype=author&query=Banik%2C+S">S. Banik</a>, <a href="/search/physics?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/physics?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/physics?searchtype=author&query=Bertolini%2C+A">A. Bertolini</a>, <a href="/search/physics?searchtype=author&query=Breier%2C+R">R. Breier</a>, <a href="/search/physics?searchtype=author&query=Bucci%2C+C">C. Bucci</a>, <a href="/search/physics?searchtype=author&query=Burkhart%2C+J">J. Burkhart</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=D%27Addabbo%2C+A">A. D'Addabbo</a>, <a href="/search/physics?searchtype=author&query=Di+Lorenzo%2C+S">S. Di Lorenzo</a>, <a href="/search/physics?searchtype=author&query=Einfalt%2C+L">L. Einfalt</a>, <a href="/search/physics?searchtype=author&query=Erb%2C+A">A. Erb</a>, <a href="/search/physics?searchtype=author&query=Feilitzsch%2C+F+v">F. v. Feilitzsch</a>, <a href="/search/physics?searchtype=author&query=Fichtinger%2C+S">S. Fichtinger</a>, <a href="/search/physics?searchtype=author&query=Fuchs%2C+D">D. Fuchs</a>, <a href="/search/physics?searchtype=author&query=Garai%2C+A">A. Garai</a>, <a href="/search/physics?searchtype=author&query=Ghete%2C+V+M">V. M. Ghete</a>, <a href="/search/physics?searchtype=author&query=Gorla%2C+P">P. Gorla</a>, <a href="/search/physics?searchtype=author&query=Guillaumon%2C+P+V">P. V. Guillaumon</a>, <a href="/search/physics?searchtype=author&query=Gupta%2C+S">S. Gupta</a>, <a href="/search/physics?searchtype=author&query=Hauff%2C+D">D. Hauff</a>, <a href="/search/physics?searchtype=author&query=Je%C5%A1kovsk%C3%BD%2C+M">M. Je拧kovsk媒</a>, <a href="/search/physics?searchtype=author&query=Jochum%2C+J">J. Jochum</a>, <a href="/search/physics?searchtype=author&query=Kaznacheeva%2C+M">M. Kaznacheeva</a> , et al. (37 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.15147v1-abstract-short" style="display: inline;"> Cryogenic phonon detectors with transition-edge sensors achieve the best sensitivity to light dark matter-nucleus scattering in current direct detection dark matter searches. In such devices, the temperature of the thermometer and the bias current in its readout circuit need careful optimization to achieve optimal detector performance. This task is not trivial and is typically done manually by an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.15147v1-abstract-full').style.display = 'inline'; document.getElementById('2311.15147v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.15147v1-abstract-full" style="display: none;"> Cryogenic phonon detectors with transition-edge sensors achieve the best sensitivity to light dark matter-nucleus scattering in current direct detection dark matter searches. In such devices, the temperature of the thermometer and the bias current in its readout circuit need careful optimization to achieve optimal detector performance. This task is not trivial and is typically done manually by an expert. In our work, we automated the procedure with reinforcement learning in two settings. First, we trained on a simulation of the response of three CRESST detectors used as a virtual reinforcement learning environment. Second, we trained live on the same detectors operated in the CRESST underground setup. In both cases, we were able to optimize a standard detector as fast and with comparable results as human experts. Our method enables the tuning of large-scale cryogenic detector setups with minimal manual interventions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.15147v1-abstract-full').style.display = 'none'; document.getElementById('2311.15147v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 14 figures, 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.07318">arXiv:2311.07318</a> <span> [<a href="https://arxiv.org/pdf/2311.07318">pdf</a>, <a href="https://arxiv.org/format/2311.07318">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Detector development for the CRESST experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/physics?searchtype=author&query=Banik%2C+S">S. Banik</a>, <a href="/search/physics?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/physics?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/physics?searchtype=author&query=Bertolini%2C+A">A. Bertolini</a>, <a href="/search/physics?searchtype=author&query=Breier%2C+R">R. Breier</a>, <a href="/search/physics?searchtype=author&query=Bucci%2C+C">C. Bucci</a>, <a href="/search/physics?searchtype=author&query=Burkhart%2C+J">J. Burkhart</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=D%27Addabbo%2C+A">A. D'Addabbo</a>, <a href="/search/physics?searchtype=author&query=Di+Lorenzo%2C+S">S. Di Lorenzo</a>, <a href="/search/physics?searchtype=author&query=Einfalt%2C+L">L. Einfalt</a>, <a href="/search/physics?searchtype=author&query=Erb%2C+A">A. Erb</a>, <a href="/search/physics?searchtype=author&query=Feilitzsch%2C+F+v">F. v. Feilitzsch</a>, <a href="/search/physics?searchtype=author&query=Fichtinger%2C+S">S. Fichtinger</a>, <a href="/search/physics?searchtype=author&query=Fuchs%2C+D">D. Fuchs</a>, <a href="/search/physics?searchtype=author&query=Garai%2C+A">A. Garai</a>, <a href="/search/physics?searchtype=author&query=Ghete%2C+V+M">V. M. Ghete</a>, <a href="/search/physics?searchtype=author&query=Gorla%2C+P">P. Gorla</a>, <a href="/search/physics?searchtype=author&query=Guillaumon%2C+P+V">P. V. Guillaumon</a>, <a href="/search/physics?searchtype=author&query=Gupta%2C+S">S. Gupta</a>, <a href="/search/physics?searchtype=author&query=Hauff%2C+D">D. Hauff</a>, <a href="/search/physics?searchtype=author&query=Je%C5%A1kovsk%C3%BD%2C+M">M. Je拧kovsk媒</a>, <a href="/search/physics?searchtype=author&query=Jochum%2C+J">J. Jochum</a>, <a href="/search/physics?searchtype=author&query=Kaznacheeva%2C+M">M. Kaznacheeva</a> , et al. (33 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.07318v1-abstract-short" style="display: inline;"> Recently low-mass dark matter direct searches have been hindered by a low energy background, drastically reducing the physics reach of the experiments. In the CRESST-III experiment, this signal is characterised by a significant increase of events below 200 eV. As the origin of this background is still unknown, it became necessary to develop new detector designs to reach a better understanding of t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.07318v1-abstract-full').style.display = 'inline'; document.getElementById('2311.07318v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.07318v1-abstract-full" style="display: none;"> Recently low-mass dark matter direct searches have been hindered by a low energy background, drastically reducing the physics reach of the experiments. In the CRESST-III experiment, this signal is characterised by a significant increase of events below 200 eV. As the origin of this background is still unknown, it became necessary to develop new detector designs to reach a better understanding of the observations. Within the CRESST collaboration, three new different detector layouts have been developed and they are presented in this contribution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.07318v1-abstract-full').style.display = 'none'; document.getElementById('2311.07318v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 4 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.08457">arXiv:2310.08457</a> <span> [<a href="https://arxiv.org/pdf/2310.08457">pdf</a>, <a href="https://arxiv.org/format/2310.08457">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> A Plastic Scintillation Muon Veto for Sub-Kelvin Temperatures </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Erhart%2C+A">A. Erhart</a>, <a href="/search/physics?searchtype=author&query=Wagner%2C+V">V. Wagner</a>, <a href="/search/physics?searchtype=author&query=Wex%2C+A">A. Wex</a>, <a href="/search/physics?searchtype=author&query=Goupy%2C+C">C. Goupy</a>, <a href="/search/physics?searchtype=author&query=Lhuillier%2C+D">D. Lhuillier</a>, <a href="/search/physics?searchtype=author&query=Namuth%2C+E">E. Namuth</a>, <a href="/search/physics?searchtype=author&query=Nones%2C+C">C. Nones</a>, <a href="/search/physics?searchtype=author&query=Rogly%2C+R">R. Rogly</a>, <a href="/search/physics?searchtype=author&query=Savu%2C+V">V. Savu</a>, <a href="/search/physics?searchtype=author&query=Schwarz%2C+M">M. Schwarz</a>, <a href="/search/physics?searchtype=author&query=Strauss%2C+R">R. Strauss</a>, <a href="/search/physics?searchtype=author&query=Vivier%2C+M">M. Vivier</a>, <a href="/search/physics?searchtype=author&query=Abele%2C+H">H. Abele</a>, <a href="/search/physics?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/physics?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/physics?searchtype=author&query=Burkhart%2C+J">J. Burkhart</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=Cappella%2C+F">F. Cappella</a>, <a href="/search/physics?searchtype=author&query=Casali%2C+N">N. Casali</a>, <a href="/search/physics?searchtype=author&query=Cerulli%2C+R">R. Cerulli</a>, <a href="/search/physics?searchtype=author&query=Cruciani%2C+A">A. Cruciani</a>, <a href="/search/physics?searchtype=author&query=del+Castello%2C+G">G. del Castello</a>, <a href="/search/physics?searchtype=author&query=Roccagiovine%2C+M+d+G">M. del Gallo Roccagiovine</a>, <a href="/search/physics?searchtype=author&query=Doblhammer%2C+A">A. Doblhammer</a>, <a href="/search/physics?searchtype=author&query=Dorer%2C+S">S. Dorer</a> , et al. (37 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.08457v1-abstract-short" style="display: inline;"> Rare-event search experiments located on-surface, such as short-baseline reactor neutrino experiments, are often limited by muon-induced background events. Highly efficient muon vetos are essential to reduce the detector background and to reach the sensitivity goals. We demonstrate the feasibility of deploying organic plastic scintillators at sub-Kelvin temperatures. For the NUCLEUS experiment, we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.08457v1-abstract-full').style.display = 'inline'; document.getElementById('2310.08457v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.08457v1-abstract-full" style="display: none;"> Rare-event search experiments located on-surface, such as short-baseline reactor neutrino experiments, are often limited by muon-induced background events. Highly efficient muon vetos are essential to reduce the detector background and to reach the sensitivity goals. We demonstrate the feasibility of deploying organic plastic scintillators at sub-Kelvin temperatures. For the NUCLEUS experiment, we developed a cryogenic muon veto equipped with wavelength shifting fibers and a silicon photo multiplier operating inside a dilution refrigerator. The achievable compactness of cryostat-internal integration is a key factor in keeping the muon rate to a minimum while maximizing coverage. The thermal and light output properties of a plastic scintillation detector were examined. We report first data on the thermal conductivity and heat capacity of the polystyrene-based scintillator UPS-923A over a wide range of temperatures extending below one Kelvin. The light output was measured down to 0.8K and observed to increase by a factor of 1.61$\pm$0.05 compared to 300K. The development of an organic plastic scintillation muon veto operating in sub-Kelvin temperature environments opens new perspectives for rare-event searches with cryogenic detectors at sites lacking substantial overburden. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.08457v1-abstract-full').style.display = 'none'; document.getElementById('2310.08457v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.05815">arXiv:2310.05815</a> <span> [<a href="https://arxiv.org/pdf/2310.05815">pdf</a>, <a href="https://arxiv.org/format/2310.05815">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Light Dark Matter Search Using a Diamond Cryogenic Detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=CRESST+Collaboration"> CRESST Collaboration</a>, <a href="/search/physics?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/physics?searchtype=author&query=Banik%2C+S">S. Banik</a>, <a href="/search/physics?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/physics?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/physics?searchtype=author&query=Bertolini%2C+A">A. Bertolini</a>, <a href="/search/physics?searchtype=author&query=Breier%2C+R">R. Breier</a>, <a href="/search/physics?searchtype=author&query=Bucci%2C+C">C. Bucci</a>, <a href="/search/physics?searchtype=author&query=Burkhart%2C+J">J. Burkhart</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=D%27Addabbo%2C+A">A. D'Addabbo</a>, <a href="/search/physics?searchtype=author&query=Di+Lorenzo%2C+S">S. Di Lorenzo</a>, <a href="/search/physics?searchtype=author&query=Einfalt%2C+L">L. Einfalt</a>, <a href="/search/physics?searchtype=author&query=Erb%2C+A">A. Erb</a>, <a href="/search/physics?searchtype=author&query=Feilitzsch%2C+F+v">F. v. Feilitzsch</a>, <a href="/search/physics?searchtype=author&query=Fichtinger%2C+S">S. Fichtinger</a>, <a href="/search/physics?searchtype=author&query=Fuchs%2C+D">D. Fuchs</a>, <a href="/search/physics?searchtype=author&query=Garai%2C+A">A. Garai</a>, <a href="/search/physics?searchtype=author&query=Ghete%2C+V+M">V. M. Ghete</a>, <a href="/search/physics?searchtype=author&query=Gorla%2C+P">P. Gorla</a>, <a href="/search/physics?searchtype=author&query=Guillaumon%2C+P+V">P. V. Guillaumon</a>, <a href="/search/physics?searchtype=author&query=Gupta%2C+S">S. Gupta</a>, <a href="/search/physics?searchtype=author&query=Hauff%2C+D">D. Hauff</a>, <a href="/search/physics?searchtype=author&query=Je%C5%A1kovsk%C3%BD%2C+M">M. Je拧kovsk媒</a>, <a href="/search/physics?searchtype=author&query=Jochum%2C+J">J. Jochum</a> , et al. (34 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.05815v1-abstract-short" style="display: inline;"> Diamond operated as a cryogenic calorimeter is an excellent target for direct detection of low-mass dark matter candidates. Following the realization of the first low-threshold cryogenic detector that uses diamond as absorber for astroparticle physics applications, we now present the resulting exclusion limits on the elastic spin-independent interaction cross-section of dark matter with diamond. W… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.05815v1-abstract-full').style.display = 'inline'; document.getElementById('2310.05815v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.05815v1-abstract-full" style="display: none;"> Diamond operated as a cryogenic calorimeter is an excellent target for direct detection of low-mass dark matter candidates. Following the realization of the first low-threshold cryogenic detector that uses diamond as absorber for astroparticle physics applications, we now present the resulting exclusion limits on the elastic spin-independent interaction cross-section of dark matter with diamond. We measured two 0.175 g CVD (Chemical Vapor Deposition) diamond samples, each instrumented with a W-TES. Thanks to the energy threshold of just 16.8 eV of one of the two detectors, we set exclusion limits on the elastic spin-independent interaction of dark matter particles with carbon nuclei down to dark matter masses as low as 0.122 GeV/c2. This work shows the scientific potential of cryogenic detectors made from diamond and lays the foundation for the use of this material as target for direct detection dark matter experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.05815v1-abstract-full').style.display = 'none'; document.getElementById('2310.05815v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 6 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.07694">arXiv:2308.07694</a> <span> [<a href="https://arxiv.org/pdf/2308.07694">pdf</a>, <a href="https://arxiv.org/ps/2308.07694">ps</a>, <a href="https://arxiv.org/format/2308.07694">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-ph</span> </div> </div> <p class="title is-5 mathjax"> Models of Tokamak Disruptions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Strauss%2C+H+R">H. R. Strauss</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.07694v1-abstract-short" style="display: inline;"> Disruptions are a serious issue in tokamaks. In a disruption, the thermal energy is lost by means of an instability which could be a resistive wall tearing mode (RWTM). During precursors to a disruption, the plasma edge region cools, causing the current to contract. Model sequences of contracted current equilibria are given, and their stability is calculated. A linear stability study shows that th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.07694v1-abstract-full').style.display = 'inline'; document.getElementById('2308.07694v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.07694v1-abstract-full" style="display: none;"> Disruptions are a serious issue in tokamaks. In a disruption, the thermal energy is lost by means of an instability which could be a resistive wall tearing mode (RWTM). During precursors to a disruption, the plasma edge region cools, causing the current to contract. Model sequences of contracted current equilibria are given, and their stability is calculated. A linear stability study shows that there is a maximum value of edge $q_a \approx 3$ for RWTMs to occur. This also implies a minimum rational surface radius normalized to plasma radius from RWTMs to be unstable. Nonlinear simulations are performed using a similar model sequence derived from an equilibrium reconstruction. There is a striking difference in the results, depending on whether the wall is ideal or resistive. With an ideal wall, the perturbations saturate at moderate amplitude, causing a minor disruption without a thermal quench. With a resistive wall, there is a major disruption with a thermal quench, if the edge $q_a \le 3.$ There is a sharp transition in nonlinear behavior at $q_a = 3.$ This is consistent with the linear model and with experiments. If disruptions are caused by RWTMs, then devices with highly conducting walls, such as the International Tokamak Experimental Reactor (ITER) will experience much milder, tolerable, disruptions than presently predicted. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.07694v1-abstract-full').style.display = 'none'; document.getElementById('2308.07694v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">arXiv admin note: text overlap with arXiv:2304.07994</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.12991">arXiv:2307.12991</a> <span> [<a href="https://arxiv.org/pdf/2307.12991">pdf</a>, <a href="https://arxiv.org/format/2307.12991">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/19/11/P11013">10.1088/1748-0221/19/11/P11013 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High-Dimensional Bayesian Likelihood Normalisation for CRESST's Background Model </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/physics?searchtype=author&query=Banik%2C+S">S. Banik</a>, <a href="/search/physics?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/physics?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/physics?searchtype=author&query=Bertolini%2C+A">A. Bertolini</a>, <a href="/search/physics?searchtype=author&query=Breier%2C+R">R. Breier</a>, <a href="/search/physics?searchtype=author&query=Bucci%2C+C">C. Bucci</a>, <a href="/search/physics?searchtype=author&query=Burkhart%2C+J">J. Burkhart</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=D%27Addabbo%2C+A">A. D'Addabbo</a>, <a href="/search/physics?searchtype=author&query=Di+Lorenzo%2C+S">S. Di Lorenzo</a>, <a href="/search/physics?searchtype=author&query=Einfalt%2C+L">L. Einfalt</a>, <a href="/search/physics?searchtype=author&query=Erb%2C+A">A. Erb</a>, <a href="/search/physics?searchtype=author&query=Feilitzsch%2C+F+v">F. v. Feilitzsch</a>, <a href="/search/physics?searchtype=author&query=Fichtinger%2C+S">S. Fichtinger</a>, <a href="/search/physics?searchtype=author&query=Fuchs%2C+D">D. Fuchs</a>, <a href="/search/physics?searchtype=author&query=Garai%2C+A">A. Garai</a>, <a href="/search/physics?searchtype=author&query=Ghete%2C+V+M">V. M. Ghete</a>, <a href="/search/physics?searchtype=author&query=Gorla%2C+P">P. Gorla</a>, <a href="/search/physics?searchtype=author&query=Guillaumon%2C+P+V">P. V. Guillaumon</a>, <a href="/search/physics?searchtype=author&query=Gupta%2C+S">S. Gupta</a>, <a href="/search/physics?searchtype=author&query=Hauff%2C+D">D. Hauff</a>, <a href="/search/physics?searchtype=author&query=Jeskovsky%2C+M">M. Jeskovsky</a>, <a href="/search/physics?searchtype=author&query=Jochum%2C+J">J. Jochum</a>, <a href="/search/physics?searchtype=author&query=Kaznacheeva%2C+M">M. Kaznacheeva</a> , et al. (37 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.12991v2-abstract-short" style="display: inline;"> Using CaWO$_4$ crystals as cryogenic calorimeters, the CRESST experiment searches for nuclear recoils caused by the scattering of potential Dark Matter particles. A reliable identification of a potential signal crucially depends on an accurate background model. In this work we introduce an improved normalisation method for CRESST's model of the electromagnetic backgrounds. Spectral templates, base… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.12991v2-abstract-full').style.display = 'inline'; document.getElementById('2307.12991v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.12991v2-abstract-full" style="display: none;"> Using CaWO$_4$ crystals as cryogenic calorimeters, the CRESST experiment searches for nuclear recoils caused by the scattering of potential Dark Matter particles. A reliable identification of a potential signal crucially depends on an accurate background model. In this work we introduce an improved normalisation method for CRESST's model of the electromagnetic backgrounds. Spectral templates, based on Geant4 simulations, are normalised via a Bayesian likelihood fit to experimental background data. Contrary to our previous work, no assumption of partial secular equilibrium is required, which results in a more robust and versatile applicability. Furthermore, considering the correlation between all background components allows us to explain 82.7% of the experimental background within [1 keV, 40 keV], an improvement of 18.6% compared to our previous method. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.12991v2-abstract-full').style.display = 'none'; document.getElementById('2307.12991v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">38 pages, 15 figures, accepted version to JINST</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2024 JINST 19 P11013 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.10139">arXiv:2305.10139</a> <span> [<a href="https://arxiv.org/pdf/2305.10139">pdf</a>, <a href="https://arxiv.org/format/2305.10139">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Study of collision and $纬$-cascade times following neutron-capture processes in cryogenic detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=CRAB+collaboration"> CRAB collaboration</a>, <a href="/search/physics?searchtype=author&query=Soum-Sidikov%2C+G">G. Soum-Sidikov</a>, <a href="/search/physics?searchtype=author&query=Abele%2C+H">H. Abele</a>, <a href="/search/physics?searchtype=author&query=Burkhart%2C+J">J. Burkhart</a>, <a href="/search/physics?searchtype=author&query=Cappella%2C+F">F. Cappella</a>, <a href="/search/physics?searchtype=author&query=Casali%2C+N">N. Casali</a>, <a href="/search/physics?searchtype=author&query=Cerulli%2C+R">R. Cerulli</a>, <a href="/search/physics?searchtype=author&query=Chalil%2C+A">A. Chalil</a>, <a href="/search/physics?searchtype=author&query=Chebboubi%2C+A">A. Chebboubi</a>, <a href="/search/physics?searchtype=author&query=Crocombette%2C+J">J-P. Crocombette</a>, <a href="/search/physics?searchtype=author&query=del+Castello%2C+G">G. del Castello</a>, <a href="/search/physics?searchtype=author&query=Roccagiovine%2C+M+d+G">M. del Gallo Roccagiovine</a>, <a href="/search/physics?searchtype=author&query=Doblhammer%2C+A">A. Doblhammer</a>, <a href="/search/physics?searchtype=author&query=Dorer%2C+S">S. Dorer</a>, <a href="/search/physics?searchtype=author&query=Dumonteil%2C+E">E. Dumonteil</a>, <a href="/search/physics?searchtype=author&query=Erhart%2C+A">A. Erhart</a>, <a href="/search/physics?searchtype=author&query=Giuliani%2C+A">A. Giuliani</a>, <a href="/search/physics?searchtype=author&query=Goupy%2C+C">C. Goupy</a>, <a href="/search/physics?searchtype=author&query=Gunsing%2C+F">F. Gunsing</a>, <a href="/search/physics?searchtype=author&query=Jericha%2C+E">E. Jericha</a>, <a href="/search/physics?searchtype=author&query=Kaznacheeva%2C+M">M. Kaznacheeva</a>, <a href="/search/physics?searchtype=author&query=Kinast%2C+A">A. Kinast</a>, <a href="/search/physics?searchtype=author&query=Kluck%2C+H">H. Kluck</a>, <a href="/search/physics?searchtype=author&query=Langenk%C3%A4mper%2C+A">A. Langenk盲mper</a>, <a href="/search/physics?searchtype=author&query=Lasserre%2C+T">T. Lasserre</a> , et al. (25 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.10139v1-abstract-short" style="display: inline;"> The emission of $纬$-rays after a neutron capture in a cryogenic detector can generate mono-energetic nuclear recoils in the sub-keV regime, of direct interest for the calibration of Dark Matter and Coherent Elastic Neutrino Nucleus Scattering experiments. Here we show that accurate predictions of the nuclear recoil spectra induced by neutron captures require taking into account the interplay betwe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.10139v1-abstract-full').style.display = 'inline'; document.getElementById('2305.10139v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.10139v1-abstract-full" style="display: none;"> The emission of $纬$-rays after a neutron capture in a cryogenic detector can generate mono-energetic nuclear recoils in the sub-keV regime, of direct interest for the calibration of Dark Matter and Coherent Elastic Neutrino Nucleus Scattering experiments. Here we show that accurate predictions of the nuclear recoil spectra induced by neutron captures require taking into account the interplay between the development in time of the de-excitation $纬$-cascade of the target nucleus and that of the associated atomic collisions in matter. We present detailed simulations coupling the FIFRELIN code for the description of the $纬$-cascades and the IRADINA code for the modelling of the fast atomic movements in matter. Nuclear recoil spectra are predicted, and made available to the community, for concrete cases of Al$_2$O$_3$, Si, Ge and CaWO$_4$ crystals exposed to a low intensity beam of thermal neutrons. We find that timing effects cause new calibration peaks to emerge in the recoil spectra and also impact the shape of the continuous recoil distribution. We discuss how they could give access to a rich physics program, spanning the accurate study of the response of cryogenic detectors in the sub-keV range, tests of solid state physics simulations and tests of nuclear models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.10139v1-abstract-full').style.display = 'none'; document.getElementById('2305.10139v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.05347">arXiv:2305.05347</a> <span> [<a href="https://arxiv.org/pdf/2305.05347">pdf</a>, <a href="https://arxiv.org/format/2305.05347">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acd3ef">10.3847/1538-4357/acd3ef <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On the onset delays of solar energetic electrons and protons: Evidence for a common accelerator </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Strauss%2C+R+D">R. D. Strauss</a>, <a href="/search/physics?searchtype=author&query=Dresing%2C+N">N. Dresing</a>, <a href="/search/physics?searchtype=author&query=Richardson%2C+I+G">I. G. Richardson</a>, <a href="/search/physics?searchtype=author&query=Berg%2C+J+P+v+d">J. P. van den Berg</a>, <a href="/search/physics?searchtype=author&query=Steyn%2C+P+J">P. J. Steyn</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.05347v1-abstract-short" style="display: inline;"> The processes responsible for the acceleration of solar energetic particles (SEPs) are still not well understood, including whether SEP electrons and protons are accelerated by common or separate processes. Using a numerical particle transport model that includes both pitch-angle and perpendicular spatial diffusion, we simulate, amongst other quantities, the onset delay for MeV electrons and proto… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.05347v1-abstract-full').style.display = 'inline'; document.getElementById('2305.05347v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.05347v1-abstract-full" style="display: none;"> The processes responsible for the acceleration of solar energetic particles (SEPs) are still not well understood, including whether SEP electrons and protons are accelerated by common or separate processes. Using a numerical particle transport model that includes both pitch-angle and perpendicular spatial diffusion, we simulate, amongst other quantities, the onset delay for MeV electrons and protons and compare the results to observations of SEPs from widely-separated spacecraft. Such observations have previously been interpreted, in a simple scenario assuming no perpendicular diffusion, as evidence for different electron and proton sources. We show that, by assuming a common particle source together with perpendicular diffusion, we are able to simultaneously reproduce the onset delays for both electrons and protons. We argue that this points towards a common accelerator for these particles. Moreover, a relatively broad particle source is required in the model to correctly describe the observations. This is suggestive of diffusive shock acceleration occurring at large shock structures playing a significant role in the acceleration of these SEPs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.05347v1-abstract-full').style.display = 'none'; document.getElementById('2305.05347v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.07994">arXiv:2304.07994</a> <span> [<a href="https://arxiv.org/pdf/2304.07994">pdf</a>, <a href="https://arxiv.org/ps/2304.07994">ps</a>, <a href="https://arxiv.org/format/2304.07994">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-ph</span> </div> </div> <p class="title is-5 mathjax"> A Model of Tokamak Locked Mode Disruptions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Strauss%2C+H+R">H. R. Strauss</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.07994v1-abstract-short" style="display: inline;"> Locked modes are precursors to major disruptions. During locked modes, the temperature decreases in the plasma edge region. This causes the current to contract. A model is given to analyze the MHD stability of contracted current equilibria. If there is sufficient current contraction, resistive wall tearing modes are destabilized. This requires that the q = 2 surface be sufficiently close to the wa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.07994v1-abstract-full').style.display = 'inline'; document.getElementById('2304.07994v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.07994v1-abstract-full" style="display: none;"> Locked modes are precursors to major disruptions. During locked modes, the temperature decreases in the plasma edge region. This causes the current to contract. A model is given to analyze the MHD stability of contracted current equilibria. If there is sufficient current contraction, resistive wall tearing modes are destabilized. This requires that the q = 2 surface be sufficiently close to the wall. The threshold conditions obtained in the model are consistent with experimental observations of the conditions for a thermal quench in a disruption. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.07994v1-abstract-full').style.display = 'none'; document.getElementById('2304.07994v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 3 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.15452">arXiv:2303.15452</a> <span> [<a href="https://arxiv.org/pdf/2303.15452">pdf</a>, <a href="https://arxiv.org/format/2303.15452">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Geophysics">physics.geo-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Atmospheric and Oceanic Physics">physics.ao-ph</span> </div> </div> <p class="title is-5 mathjax"> The radiation environment over the African continent at aviation altitudes: First results of the RPiRENA-based dosimeter </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Mosotho%2C+M+G">M. G. Mosotho</a>, <a href="/search/physics?searchtype=author&query=Strauss%2C+R+D">R. D. Strauss</a>, <a href="/search/physics?searchtype=author&query=Bottcher%2C+S">S. Bottcher</a>, <a href="/search/physics?searchtype=author&query=Diedericks%2C+C">C. Diedericks</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.15452v1-abstract-short" style="display: inline;"> The radiation environment over the African continent, at aviation altitudes, remains mostly uncharacterized and unregulated. In this paper we present initial measurements made by a newly developed active dosimeter on-board long-haul flights between South Africa and Germany. Based on these initial tests, we believe that this low-cost and open-source dosimeter is suitable for continued operation ove… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15452v1-abstract-full').style.display = 'inline'; document.getElementById('2303.15452v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.15452v1-abstract-full" style="display: none;"> The radiation environment over the African continent, at aviation altitudes, remains mostly uncharacterized and unregulated. In this paper we present initial measurements made by a newly developed active dosimeter on-board long-haul flights between South Africa and Germany. Based on these initial tests, we believe that this low-cost and open-source dosimeter is suitable for continued operation over the Africa continent and can provide valuable long-term measurements to test dosimteric models and inform aviation policy <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15452v1-abstract-full').style.display = 'none'; document.getElementById('2303.15452v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to appear in Journal of Space Weather and Space Climate</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.15315">arXiv:2303.15315</a> <span> [<a href="https://arxiv.org/pdf/2303.15315">pdf</a>, <a href="https://arxiv.org/format/2303.15315">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.108.022005">10.1103/PhysRevD.108.022005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observation of a low energy nuclear recoil peak in the neutron calibration data of the CRESST-III Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=CRESST+Collaboration"> CRESST Collaboration</a>, <a href="/search/physics?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/physics?searchtype=author&query=Banik%2C+S">S. Banik</a>, <a href="/search/physics?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/physics?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/physics?searchtype=author&query=Bertolini%2C+A">A. Bertolini</a>, <a href="/search/physics?searchtype=author&query=Breier%2C+R">R. Breier</a>, <a href="/search/physics?searchtype=author&query=Bucci%2C+C">C. Bucci</a>, <a href="/search/physics?searchtype=author&query=Burkhart%2C+J">J. Burkhart</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=D%27Addabbo%2C+A">A. D'Addabbo</a>, <a href="/search/physics?searchtype=author&query=Di+Lorenzo%2C+S">S. Di Lorenzo</a>, <a href="/search/physics?searchtype=author&query=Einfalt%2C+L">L. Einfalt</a>, <a href="/search/physics?searchtype=author&query=Erb%2C+A">A. Erb</a>, <a href="/search/physics?searchtype=author&query=Feilitzsch%2C+F+v">F. v. Feilitzsch</a>, <a href="/search/physics?searchtype=author&query=Fichtinger%2C+S">S. Fichtinger</a>, <a href="/search/physics?searchtype=author&query=Fuchs%2C+D">D. Fuchs</a>, <a href="/search/physics?searchtype=author&query=Fuss%2C+A">A. Fuss</a>, <a href="/search/physics?searchtype=author&query=Garai%2C+A">A. Garai</a>, <a href="/search/physics?searchtype=author&query=Ghete%2C+V+M">V. M. Ghete</a>, <a href="/search/physics?searchtype=author&query=Gerster%2C+S">S. Gerster</a>, <a href="/search/physics?searchtype=author&query=Gorla%2C+P">P. Gorla</a>, <a href="/search/physics?searchtype=author&query=Guillaumon%2C+P+V">P. V. Guillaumon</a>, <a href="/search/physics?searchtype=author&query=Gupta%2C+S">S. Gupta</a>, <a href="/search/physics?searchtype=author&query=Hauff%2C+D">D. Hauff</a> , et al. (36 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.15315v2-abstract-short" style="display: inline;"> New-generation direct searches for low mass dark matter feature detection thresholds at energies well below 100 eV, much lower than the energies of commonly used X-ray calibration sources. This requires new calibration sources with sub-keV energies. When searching for nuclear recoil signals, the calibration source should ideally cause mono-energetic nuclear recoils in the relevant energy range. Re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15315v2-abstract-full').style.display = 'inline'; document.getElementById('2303.15315v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.15315v2-abstract-full" style="display: none;"> New-generation direct searches for low mass dark matter feature detection thresholds at energies well below 100 eV, much lower than the energies of commonly used X-ray calibration sources. This requires new calibration sources with sub-keV energies. When searching for nuclear recoil signals, the calibration source should ideally cause mono-energetic nuclear recoils in the relevant energy range. Recently, a new calibration method based on the radiative neutron capture on $^{182}$W with subsequent de-excitation via single $纬$-emission leading to a nuclear recoil peak at 112 eV was proposed. The CRESST-III dark matter search operated several CaWO$_{4}$-based detector modules with detection thresholds below 100 eV in the past years. We report the observation of a peak around the expected energy of 112 eV in the data of three different detector modules recorded while irradiated with neutrons from different AmBe calibration sources. We compare the properties of the observed peaks with Geant-4 simulations and assess the prospects of using this for the energy calibration of CRESST-III detectors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15315v2-abstract-full').style.display = 'none'; document.getElementById('2303.15315v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 4 figures; submitted to Phys. Rev. D</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 108, 022005 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.10969">arXiv:2303.10969</a> <span> [<a href="https://arxiv.org/pdf/2303.10969">pdf</a>, <a href="https://arxiv.org/format/2303.10969">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202345938">10.1051/0004-6361/202345938 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The 17 April 2021 widespread solar energetic particle event </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Dresing%2C+N">N. Dresing</a>, <a href="/search/physics?searchtype=author&query=Rodr%C3%ADguez-Garc%C3%ADa%2C+L">L. Rodr铆guez-Garc铆a</a>, <a href="/search/physics?searchtype=author&query=Jebaraj%2C+I+C">I. C. Jebaraj</a>, <a href="/search/physics?searchtype=author&query=Warmuth%2C+A">A. Warmuth</a>, <a href="/search/physics?searchtype=author&query=Wallace%2C+S">S. Wallace</a>, <a href="/search/physics?searchtype=author&query=Balmaceda%2C+L">L. Balmaceda</a>, <a href="/search/physics?searchtype=author&query=Podladchikova%2C+T">T. Podladchikova</a>, <a href="/search/physics?searchtype=author&query=Strauss%2C+R+D">R. D. Strauss</a>, <a href="/search/physics?searchtype=author&query=Kouloumvakos%2C+A">A. Kouloumvakos</a>, <a href="/search/physics?searchtype=author&query=Palmroos%2C+C">C. Palmroos</a>, <a href="/search/physics?searchtype=author&query=Krupar%2C+V">V. Krupar</a>, <a href="/search/physics?searchtype=author&query=Gieseler%2C+J">J. Gieseler</a>, <a href="/search/physics?searchtype=author&query=Xu%2C+Z">Z. Xu</a>, <a href="/search/physics?searchtype=author&query=Mitchell%2C+J+G">J. G. Mitchell</a>, <a href="/search/physics?searchtype=author&query=Cohen%2C+C+M+S">C. M. S. Cohen</a>, <a href="/search/physics?searchtype=author&query=de+Nolfo%2C+G+A">G. A. de Nolfo</a>, <a href="/search/physics?searchtype=author&query=Palmerio%2C+E">E. Palmerio</a>, <a href="/search/physics?searchtype=author&query=Carcaboso%2C+F">F. Carcaboso</a>, <a href="/search/physics?searchtype=author&query=Kilpua%2C+E+K+J">E. K. J. Kilpua</a>, <a href="/search/physics?searchtype=author&query=Trotta%2C+D">D. Trotta</a>, <a href="/search/physics?searchtype=author&query=Auster%2C+U">U. Auster</a>, <a href="/search/physics?searchtype=author&query=Asvestari%2C+E">E. Asvestari</a>, <a href="/search/physics?searchtype=author&query=da+Silva%2C+D">D. da Silva</a>, <a href="/search/physics?searchtype=author&query=Dr%C3%B6ge%2C+W">W. Dr枚ge</a>, <a href="/search/physics?searchtype=author&query=Getachew%2C+T">T. Getachew</a> , et al. (24 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.10969v1-abstract-short" style="display: inline;"> Context. A solar eruption on 17 April 2021 produced a widespread Solar Energetic Particle (SEP) event that was observed by five longitudinally well-separated observers in the inner heliosphere at heliocentric distances of 0.42 to 1 au: BepiColombo, Parker Solar Probe, Solar Orbiter, STEREO A, and near-Earth spacecraft. The event produced relativistic electrons and protons. It was associated with a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.10969v1-abstract-full').style.display = 'inline'; document.getElementById('2303.10969v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.10969v1-abstract-full" style="display: none;"> Context. A solar eruption on 17 April 2021 produced a widespread Solar Energetic Particle (SEP) event that was observed by five longitudinally well-separated observers in the inner heliosphere at heliocentric distances of 0.42 to 1 au: BepiColombo, Parker Solar Probe, Solar Orbiter, STEREO A, and near-Earth spacecraft. The event produced relativistic electrons and protons. It was associated with a long-lasting solar hard X-ray flare and a medium fast Coronal Mass Ejection (CME) with a speed of 880 km/s driving a shock, an EUV wave as well as long-lasting radio burst activity showing four distinct type III burst. Methods. A multi-spacecraft analysis of remote-sensing and in-situ observations is applied to attribute the SEP observations at the different locations to the various potential source regions at the Sun. An ENLIL simulation is used to characterize the interplanetary state and its role for the energetic particle transport. The magnetic connection between each spacecraft and the Sun is determined. Based on a reconstruction of the coronal shock front we determine the times when the shock establishes magnetic connections with the different observers. Radio observations are used to characterize the directivity of the four main injection episodes, which are then employed in a 2D SEP transport simulation. Results. Timing analysis of the inferred SEP solar injection suggests different source processes being important for the electron and the proton event. Comparison among the characteristics and timing of the potential particle sources, such as the CME-driven shock or the flare, suggests a stronger shock contribution for the proton event and a more likely flare-related source of the electron event. Conclusions. We find that in this event an important ingredient for the wide SEP spread was the wide longitudinal range of about 110 degrees covered by distinct SEP injections. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.10969v1-abstract-full').style.display = 'none'; document.getElementById('2303.10969v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A105 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.11926">arXiv:2302.11926</a> <span> [<a href="https://arxiv.org/pdf/2302.11926">pdf</a>, <a href="https://arxiv.org/ps/2302.11926">ps</a>, <a href="https://arxiv.org/format/2302.11926">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1361-6587/acdff8">10.1088/1361-6587/acdff8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MST Resistive Wall Tearing Mode Simulations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Strauss%2C+H+R">H. R. Strauss</a>, <a href="/search/physics?searchtype=author&query=Chapman%2C+B+E">B. E. Chapman</a>, <a href="/search/physics?searchtype=author&query=Hurst%2C+N+C">N. C. Hurst</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.11926v1-abstract-short" style="display: inline;"> The Madison Symmetric Torus (MST) is a toroidal device that, when operated as a tokamak, is resistant to disruptions. Unlike most tokamaks, the MST plasma is surrounded by a close fitting highly conducting wall, with a resistive wall penetration time two orders of magnitude longer than in JET or DIII-D, and three times longer than in ITER. The MST can operate with edge q_a < 2, unlike standard tok… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.11926v1-abstract-full').style.display = 'inline'; document.getElementById('2302.11926v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.11926v1-abstract-full" style="display: none;"> The Madison Symmetric Torus (MST) is a toroidal device that, when operated as a tokamak, is resistant to disruptions. Unlike most tokamaks, the MST plasma is surrounded by a close fitting highly conducting wall, with a resistive wall penetration time two orders of magnitude longer than in JET or DIII-D, and three times longer than in ITER. The MST can operate with edge q_a < 2, unlike standard tokamaks. Simulations presented here indicate that the MST is unstable to resistive wall tearing modes (RWTMs) and resistive wall modes (RWMs). They could in principle cause disruptions, but the predicted thermal quench time is much longer than the experimental pulse time. If the MST thermal quench time were comparable to measurements in JET and DIII-D, theory and simulations predict that disruptions would have been observed in MST. This is consistent with the modeling herein, predicting that disruptions are caused by RWTMs and RWMs. In the low q_a regime of MST, the RWTM asymptotically satisfies the RWM dispersion relation. The transition from RWTM to RWM occurs smoothly at q_a = m/n, where m,n are poloidal and toroidal mode numbers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.11926v1-abstract-full').style.display = 'none'; document.getElementById('2302.11926v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.02816">arXiv:2302.02816</a> <span> [<a href="https://arxiv.org/pdf/2302.02816">pdf</a>, <a href="https://arxiv.org/format/2302.02816">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acb53d">10.3847/1538-4357/acb53d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The modulation of anomalous and galactic cosmic ray oxygen over successive solar cycle minima </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Strauss%2C+R+D">R. D. Strauss</a>, <a href="/search/physics?searchtype=author&query=Leske%2C+R+A">R. A. Leske</a>, <a href="/search/physics?searchtype=author&query=Rankin%2C+J+S">J. S. Rankin</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.02816v1-abstract-short" style="display: inline;"> Both the recent 2009 and 2020 solar minima were classified as unusually quiet and characterized with unusually high galactic cosmic ray (GCR) levels. However, unlike the trends from previous decades in which anomalous cosmic ray (ACR) and GCR levels strongly agreed, the ACR intensities did not reach such high record-setting levels.This discrepancy between the behaviour of GCRs and ACRs is investig… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.02816v1-abstract-full').style.display = 'inline'; document.getElementById('2302.02816v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.02816v1-abstract-full" style="display: none;"> Both the recent 2009 and 2020 solar minima were classified as unusually quiet and characterized with unusually high galactic cosmic ray (GCR) levels. However, unlike the trends from previous decades in which anomalous cosmic ray (ACR) and GCR levels strongly agreed, the ACR intensities did not reach such high record-setting levels.This discrepancy between the behaviour of GCRs and ACRs is investigated in this work by simulating the acceleration and transport of GCR and ACR oxygen under different transport conditions. After using recent observations to constrain any remaining free parameters present in the model, we show that less turbulent conditions are characterized by higher GCR fluxes and low ACR fluxes due to less efficient ACR acceleration at the solar wind termination shock. We offer this as an explanation for the ACR/GCR discrepancy observed during 2009 and 2020, when compared to previous solar cycles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.02816v1-abstract-full').style.display = 'none'; document.getElementById('2302.02816v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.02441">arXiv:2212.02441</a> <span> [<a href="https://arxiv.org/pdf/2212.02441">pdf</a>, <a href="https://arxiv.org/format/2212.02441">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aca903">10.3847/1538-4357/aca903 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The radial variation of the solar wind turbulence spectra near the kinetic break scale from Parker Solar Probe measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Lotz%2C+S">S. Lotz</a>, <a href="/search/physics?searchtype=author&query=Nel%2C+A+E">A. E. Nel</a>, <a href="/search/physics?searchtype=author&query=Wicks%2C+R+T">R. T. Wicks</a>, <a href="/search/physics?searchtype=author&query=Roberts%2C+O+W">O. W. Roberts</a>, <a href="/search/physics?searchtype=author&query=Engelbrecht%2C+N+E">N. E. Engelbrecht</a>, <a href="/search/physics?searchtype=author&query=Strauss%2C+R+D">R. D. Strauss</a>, <a href="/search/physics?searchtype=author&query=Botha%2C+G+J+J">G. J. J. Botha</a>, <a href="/search/physics?searchtype=author&query=Kontar%2C+E+P">E. P. Kontar</a>, <a href="/search/physics?searchtype=author&query=Pitna%2C+A">A. Pitna</a>, <a href="/search/physics?searchtype=author&query=Bale%2C+S+D">S. D. Bale</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.02441v1-abstract-short" style="display: inline;"> In this study we examine the radial dependence of the inertial and dissipation range indices, as well as the spectral break separating the inertial and dissipation range in power density spectra of interplanetary magnetic field fluctuations using {\it Parker Solar Probe} data from the fifth solar encounter between $\sim$0.1 and $\sim$0.7 au. The derived break wavenumber compares reasonably well wi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.02441v1-abstract-full').style.display = 'inline'; document.getElementById('2212.02441v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.02441v1-abstract-full" style="display: none;"> In this study we examine the radial dependence of the inertial and dissipation range indices, as well as the spectral break separating the inertial and dissipation range in power density spectra of interplanetary magnetic field fluctuations using {\it Parker Solar Probe} data from the fifth solar encounter between $\sim$0.1 and $\sim$0.7 au. The derived break wavenumber compares reasonably well with previous estimates at larger radial distances and is consistent with gyro-resonant damping of Alfv茅nic fluctuations by thermal protons. We find that the inertial scale power law index varies between approximately -1.65 and -1.45. This is consistent with either the Kolmogorov (-5/3) or Iroshnikov-Kraichnan (-3/2) values, has a very weak radial dependence with a possible hint that the spectrum becomes steeper closer to the Sun. The dissipation range power law index, however, has a clear dependence on radial distance (and turbulence age), decreasing from -3 near 0.7 au (4 days) to -4 [$\pm$0.3] at 0.1 au (0.75 days) closer to the Sun. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.02441v1-abstract-full').style.display = 'none'; document.getElementById('2212.02441v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.09669">arXiv:2211.09669</a> <span> [<a href="https://arxiv.org/pdf/2211.09669">pdf</a>, <a href="https://arxiv.org/format/2211.09669">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> SNOWMASS Neutrino Frontier NF10 Topical Group Report: Neutrino Detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Klein%2C+J+R">Joshua R. Klein</a>, <a href="/search/physics?searchtype=author&query=Machado%2C+A">Ana Machado</a>, <a href="/search/physics?searchtype=author&query=Schmitz%2C+D">David Schmitz</a>, <a href="/search/physics?searchtype=author&query=Strauss%2C+R">Raimund Strauss</a>, <a href="/search/physics?searchtype=author&query=Diwan%2C+M">Milind Diwan</a>, <a href="/search/physics?searchtype=author&query=Jackson%2C+C">Christopher Jackson</a>, <a href="/search/physics?searchtype=author&query=Maneira%2C+J">Jose Maneira</a>, <a href="/search/physics?searchtype=author&query=Mavrokoridis%2C+K">Kostantinos Mavrokoridis</a>, <a href="/search/physics?searchtype=author&query=McConkey%2C+N">Nicola McConkey</a>, <a href="/search/physics?searchtype=author&query=Mohai%2C+T">Tanaz Mohai</a>, <a href="/search/physics?searchtype=author&query=Petrillo%2C+G">Gianluca Petrillo</a>, <a href="/search/physics?searchtype=author&query=Zennamo%2C+J">Joseph Zennamo</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.09669v1-abstract-short" style="display: inline;"> We discuss here future neutrino detectors with physics goals ranging from the eV to the EeV scale. The focus is on future enabling technologies for such detectors, rather than existing detectors or those under construction. The report includes methodologies across the broad spectrum of neutrino physics: liquid noble and other cryogenic detectors, includin LAr and LXe TPCs; photon-based detectors i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.09669v1-abstract-full').style.display = 'inline'; document.getElementById('2211.09669v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.09669v1-abstract-full" style="display: none;"> We discuss here future neutrino detectors with physics goals ranging from the eV to the EeV scale. The focus is on future enabling technologies for such detectors, rather than existing detectors or those under construction. The report includes methodologies across the broad spectrum of neutrino physics: liquid noble and other cryogenic detectors, includin LAr and LXe TPCs; photon-based detectors including technologies enabling hybrid Cherenkov/scintillation detectors; low-threshold detectors which use a wide variety of technologies to probe physics like coherent neutrino-nucleus scattering or detection of cosmic background neutrinos; and ultra-high energy detectors including optical and radio detectors, as well as tracking detectors for use at the forward physics facility of the LHC <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.09669v1-abstract-full').style.display = 'none'; document.getElementById('2211.09669v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.04189">arXiv:2211.04189</a> <span> [<a href="https://arxiv.org/pdf/2211.04189">pdf</a>, <a href="https://arxiv.org/format/2211.04189">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Exploring coherent elastic neutrino-nucleus scattering of reactor neutrinos with the NUCLEUS experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=The+NUCLEUS+collaboration"> The NUCLEUS collaboration</a>, <a href="/search/physics?searchtype=author&query=Goupy%2C+C">C. Goupy</a>, <a href="/search/physics?searchtype=author&query=Abele%2C+H">H. Abele</a>, <a href="/search/physics?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/physics?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=Cappella%2C+F">F. Cappella</a>, <a href="/search/physics?searchtype=author&query=Cardani%2C+L">L. Cardani</a>, <a href="/search/physics?searchtype=author&query=Casali%2C+N">N. Casali</a>, <a href="/search/physics?searchtype=author&query=Cerulli%2C+R">R. Cerulli</a>, <a href="/search/physics?searchtype=author&query=Colantoni%2C+I">I. Colantoni</a>, <a href="/search/physics?searchtype=author&query=Cruciani%2C+A">A. Cruciani</a>, <a href="/search/physics?searchtype=author&query=Del+Castello%2C+G">G. Del Castello</a>, <a href="/search/physics?searchtype=author&query=Roccagiovine%2C+M+d+G">M. del Gallo Roccagiovine</a>, <a href="/search/physics?searchtype=author&query=Doblhammer%2C+A">A. Doblhammer</a>, <a href="/search/physics?searchtype=author&query=Dorer%2C+S">S. Dorer</a>, <a href="/search/physics?searchtype=author&query=Erhart%2C+A">A. Erhart</a>, <a href="/search/physics?searchtype=author&query=Friendl%2C+M">M. Friendl</a>, <a href="/search/physics?searchtype=author&query=Garai%2C+A">A. Garai</a>, <a href="/search/physics?searchtype=author&query=Ghete%2C+V+M">V. M. Ghete</a>, <a href="/search/physics?searchtype=author&query=Hauff%2C+D">D. Hauff</a>, <a href="/search/physics?searchtype=author&query=Jeanneau%2C+F">F. Jeanneau</a>, <a href="/search/physics?searchtype=author&query=Jericha%2C+E">E. Jericha</a>, <a href="/search/physics?searchtype=author&query=Kaznacheeva%2C+M">M. Kaznacheeva</a>, <a href="/search/physics?searchtype=author&query=Kinast%2C+A">A. Kinast</a> , et al. (37 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.04189v2-abstract-short" style="display: inline;"> The NUCLEUS experiment aims to perform a high-precision measurement of Coherent Elastic Neutrino-Nucleus Scattering (CEvNS) at the EdF Chooz B nuclear power plant in France. CEvNS is a unique process to study neutrino properties and to search for physics beyond the Standard Model. The study of CEvNS is also important for light Dark-Matter searches. It could be a possible irreducible background for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.04189v2-abstract-full').style.display = 'inline'; document.getElementById('2211.04189v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.04189v2-abstract-full" style="display: none;"> The NUCLEUS experiment aims to perform a high-precision measurement of Coherent Elastic Neutrino-Nucleus Scattering (CEvNS) at the EdF Chooz B nuclear power plant in France. CEvNS is a unique process to study neutrino properties and to search for physics beyond the Standard Model. The study of CEvNS is also important for light Dark-Matter searches. It could be a possible irreducible background for high-sensitivity Dark-Matter searches. NUCLEUS is an experiment under construction based on ultra-low threshold (20 eVnr) cryogenic calorimeters, operated at tens-of-mK temperatures. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.04189v2-abstract-full').style.display = 'none'; document.getElementById('2211.04189v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Procceding for 14th International Conference on Identification of Dark Matter Vienna, Austria, 18-22 July 2022 - Submitted to SciPost</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.03631">arXiv:2211.03631</a> <span> [<a href="https://arxiv.org/pdf/2211.03631">pdf</a>, <a href="https://arxiv.org/format/2211.03631">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.130.211802">10.1103/PhysRevLett.130.211802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observation of a nuclear recoil peak at the 100 eV scale induced by neutron capture </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=CRAB+Collaboration"> CRAB Collaboration</a>, <a href="/search/physics?searchtype=author&query=NUCLEUS+Collaboration"> NUCLEUS Collaboration</a>, <a href="/search/physics?searchtype=author&query=Abele%2C+H">H. Abele</a>, <a href="/search/physics?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/physics?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=Cappella%2C+F">F. Cappella</a>, <a href="/search/physics?searchtype=author&query=Cardani%2C+L">L. Cardani</a>, <a href="/search/physics?searchtype=author&query=Casali%2C+N">N. Casali</a>, <a href="/search/physics?searchtype=author&query=Cerulli%2C+R">R. Cerulli</a>, <a href="/search/physics?searchtype=author&query=Chalil%2C+A">A. Chalil</a>, <a href="/search/physics?searchtype=author&query=Chebboubi%2C+A">A. Chebboubi</a>, <a href="/search/physics?searchtype=author&query=Colantoni%2C+I">I. Colantoni</a>, <a href="/search/physics?searchtype=author&query=Crocombette%2C+J+-">J. -P. Crocombette</a>, <a href="/search/physics?searchtype=author&query=Cruciani%2C+A">A. Cruciani</a>, <a href="/search/physics?searchtype=author&query=Del+Castello%2C+G">G. Del Castello</a>, <a href="/search/physics?searchtype=author&query=Roccagiovine%2C+M+d+G">M. del Gallo Roccagiovine</a>, <a href="/search/physics?searchtype=author&query=Desforge%2C+D">D. Desforge</a>, <a href="/search/physics?searchtype=author&query=Doblhammer%2C+A">A. Doblhammer</a>, <a href="/search/physics?searchtype=author&query=Dumonteil%2C+E">E. Dumonteil</a>, <a href="/search/physics?searchtype=author&query=Dorer%2C+S">S. Dorer</a>, <a href="/search/physics?searchtype=author&query=Erhart%2C+A">A. Erhart</a>, <a href="/search/physics?searchtype=author&query=Fuss%2C+A">A. Fuss</a>, <a href="/search/physics?searchtype=author&query=Friedl%2C+M">M. Friedl</a>, <a href="/search/physics?searchtype=author&query=Garai%2C+A">A. Garai</a> , et al. (53 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.03631v2-abstract-short" style="display: inline;"> Coherent elastic neutrino-nucleus scattering and low-mass Dark Matter detectors rely crucially on the understanding of their response to nuclear recoils. We report the first observation of a nuclear recoil peak at around 112 eV induced by neutron capture. The measurement was performed with a CaWO$_4$ cryogenic detector from the NUCLEUS experiment exposed to a $^{252}$Cf source placed in a compact… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.03631v2-abstract-full').style.display = 'inline'; document.getElementById('2211.03631v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.03631v2-abstract-full" style="display: none;"> Coherent elastic neutrino-nucleus scattering and low-mass Dark Matter detectors rely crucially on the understanding of their response to nuclear recoils. We report the first observation of a nuclear recoil peak at around 112 eV induced by neutron capture. The measurement was performed with a CaWO$_4$ cryogenic detector from the NUCLEUS experiment exposed to a $^{252}$Cf source placed in a compact moderator. The measured spectrum is found in agreement with simulations and the expected peak structure from the single-$纬$ de-excitation of $^{183}$W is identified with 3 $蟽$ significance. This result demonstrates a new method for precise, in-situ, and non-intrusive calibration of low-threshold experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.03631v2-abstract-full').style.display = 'none'; document.getElementById('2211.03631v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 130, 211802 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.00564">arXiv:2211.00564</a> <span> [<a href="https://arxiv.org/pdf/2211.00564">pdf</a>, <a href="https://arxiv.org/format/2211.00564">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjp/s13360-023-03674-2">10.1140/epjp/s13360-023-03674-2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Towards an automated data cleaning with deep learning in CRESST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/physics?searchtype=author&query=Banik%2C+S">S. Banik</a>, <a href="/search/physics?searchtype=author&query=Bartolot%2C+D">D. Bartolot</a>, <a href="/search/physics?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/physics?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/physics?searchtype=author&query=Bertolini%2C+A">A. Bertolini</a>, <a href="/search/physics?searchtype=author&query=Breier%2C+R">R. Breier</a>, <a href="/search/physics?searchtype=author&query=Bucci%2C+C">C. Bucci</a>, <a href="/search/physics?searchtype=author&query=Burkhart%2C+J">J. Burkhart</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=D%27Addabbo%2C+A">A. D'Addabbo</a>, <a href="/search/physics?searchtype=author&query=Di+Lorenzo%2C+S">S. Di Lorenzo</a>, <a href="/search/physics?searchtype=author&query=Einfalt%2C+L">L. Einfalt</a>, <a href="/search/physics?searchtype=author&query=Erb%2C+A">A. Erb</a>, <a href="/search/physics?searchtype=author&query=Feilitzsch%2C+F+v">F. v. Feilitzsch</a>, <a href="/search/physics?searchtype=author&query=Iachellini%2C+N+F">N. Ferreiro Iachellini</a>, <a href="/search/physics?searchtype=author&query=Fichtinger%2C+S">S. Fichtinger</a>, <a href="/search/physics?searchtype=author&query=Fuchs%2C+D">D. Fuchs</a>, <a href="/search/physics?searchtype=author&query=Fuss%2C+A">A. Fuss</a>, <a href="/search/physics?searchtype=author&query=Garai%2C+A">A. Garai</a>, <a href="/search/physics?searchtype=author&query=Ghete%2C+V+M">V. M. Ghete</a>, <a href="/search/physics?searchtype=author&query=Gerster%2C+S">S. Gerster</a>, <a href="/search/physics?searchtype=author&query=Gorla%2C+P">P. Gorla</a>, <a href="/search/physics?searchtype=author&query=Guillaumon%2C+P+V">P. V. Guillaumon</a>, <a href="/search/physics?searchtype=author&query=Gupta%2C+S">S. Gupta</a> , et al. (40 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.00564v2-abstract-short" style="display: inline;"> The CRESST experiment employs cryogenic calorimeters for the sensitive measurement of nuclear recoils induced by dark matter particles. The recorded signals need to undergo a careful cleaning process to avoid wrongly reconstructed recoil energies caused by pile-up and read-out artefacts. We frame this process as a time series classification task and propose to automate it with neural networks. Wit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.00564v2-abstract-full').style.display = 'inline'; document.getElementById('2211.00564v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.00564v2-abstract-full" style="display: none;"> The CRESST experiment employs cryogenic calorimeters for the sensitive measurement of nuclear recoils induced by dark matter particles. The recorded signals need to undergo a careful cleaning process to avoid wrongly reconstructed recoil energies caused by pile-up and read-out artefacts. We frame this process as a time series classification task and propose to automate it with neural networks. With a data set of over one million labeled records from 68 detectors, recorded between 2013 and 2019 by CRESST, we test the capability of four commonly used neural network architectures to learn the data cleaning task. Our best performing model achieves a balanced accuracy of 0.932 on our test set. We show on an exemplary detector that about half of the wrongly predicted events are in fact wrongly labeled events, and a large share of the remaining ones have a context-dependent ground truth. We furthermore evaluate the recall and selectivity of our classifiers with simulated data. The results confirm that the trained classifiers are well suited for the data cleaning task. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.00564v2-abstract-full').style.display = 'none'; document.getElementById('2211.00564v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 8 figures, 6 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. Plus 138, 100 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.00461">arXiv:2209.00461</a> <span> [<a href="https://arxiv.org/pdf/2209.00461">pdf</a>, <a href="https://arxiv.org/format/2209.00461">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.apradiso.2023.110670">10.1016/j.apradiso.2023.110670 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Secular Equilibrium Assessment in a $\mathrm{CaWO}_4$ Target Crystal from the Dark Matter Experiment CRESST using Bayesian Likelihood Normalisation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/physics?searchtype=author&query=Banik%2C+S">S. Banik</a>, <a href="/search/physics?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/physics?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/physics?searchtype=author&query=Bertolini%2C+A">A. Bertolini</a>, <a href="/search/physics?searchtype=author&query=Breier%2C+R">R. Breier</a>, <a href="/search/physics?searchtype=author&query=Bucci%2C+C">C. Bucci</a>, <a href="/search/physics?searchtype=author&query=Burkhart%2C+J">J. Burkhart</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=D%27Addabbo%2C+A">A. D'Addabbo</a>, <a href="/search/physics?searchtype=author&query=Di+Lorenzo%2C+S">S. Di Lorenzo</a>, <a href="/search/physics?searchtype=author&query=Einfalt%2C+L">L. Einfalt</a>, <a href="/search/physics?searchtype=author&query=Erb%2C+A">A. Erb</a>, <a href="/search/physics?searchtype=author&query=Feilitzsch%2C+F+v">F. v. Feilitzsch</a>, <a href="/search/physics?searchtype=author&query=Iachellini%2C+N+F">N. Ferreiro Iachellini</a>, <a href="/search/physics?searchtype=author&query=Fichtinger%2C+S">S. Fichtinger</a>, <a href="/search/physics?searchtype=author&query=Fuchs%2C+D">D. Fuchs</a>, <a href="/search/physics?searchtype=author&query=Fuss%2C+A">A. Fuss</a>, <a href="/search/physics?searchtype=author&query=Garai%2C+A">A. Garai</a>, <a href="/search/physics?searchtype=author&query=Ghete%2C+V+M">V. M. Ghete</a>, <a href="/search/physics?searchtype=author&query=Gorla%2C+P">P. Gorla</a>, <a href="/search/physics?searchtype=author&query=Gupta%2C+S">S. Gupta</a>, <a href="/search/physics?searchtype=author&query=Hauff%2C+D">D. Hauff</a>, <a href="/search/physics?searchtype=author&query=Je%C5%A1kovsk%C3%BD%2C+M">M. Je拧kovsk媒</a>, <a href="/search/physics?searchtype=author&query=Jochum%2C+J">J. Jochum</a> , et al. (36 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.00461v2-abstract-short" style="display: inline;"> CRESST is a leading direct detection sub-$\mathrm{GeVc}^{-2}$ dark matter experiment. During its second phase, cryogenic bolometers were used to detect nuclear recoils off the $\mathrm{CaWO}_4$ target crystal nuclei. The previously established electromagnetic background model relies on secular equilibrium (SE) assumptions. In this work, a validation of SE is attempted by comparing two likelihood-b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.00461v2-abstract-full').style.display = 'inline'; document.getElementById('2209.00461v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.00461v2-abstract-full" style="display: none;"> CRESST is a leading direct detection sub-$\mathrm{GeVc}^{-2}$ dark matter experiment. During its second phase, cryogenic bolometers were used to detect nuclear recoils off the $\mathrm{CaWO}_4$ target crystal nuclei. The previously established electromagnetic background model relies on secular equilibrium (SE) assumptions. In this work, a validation of SE is attempted by comparing two likelihood-based normalisation results using a recently developed spectral template normalisation method based on Bayesian likelihood. We find deviations from SE; further investigations are necessary to determine their origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.00461v2-abstract-full').style.display = 'none'; document.getElementById('2209.00461v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Part of special issue: ICRM-LLRMT22 8th International Conference on Radionuclide Metrology - Low Level Radioactivity Measurement and Techniques, 6 pages, 3 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Applied Radiation and Isotopes, 194 (2023) 110670 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.05116">arXiv:2206.05116</a> <span> [<a href="https://arxiv.org/pdf/2206.05116">pdf</a>, <a href="https://arxiv.org/format/2206.05116">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Characterization of a kg-scale archaeological lead-based cryogenic detectors for the RES-NOVA experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Beeman%2C+J+W">J. W. Beeman</a>, <a href="/search/physics?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/physics?searchtype=author&query=Bucci%2C+C">C. Bucci</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=Carniti%2C+P">P. Carniti</a>, <a href="/search/physics?searchtype=author&query=Celi%2C+E">E. Celi</a>, <a href="/search/physics?searchtype=author&query=Clemenza%2C+M">M. Clemenza</a>, <a href="/search/physics?searchtype=author&query=D%27Addabbo%2C+A">A. D'Addabbo</a>, <a href="/search/physics?searchtype=author&query=Danevich%2C+F+A">F. A. Danevich</a>, <a href="/search/physics?searchtype=author&query=Di+Domizio%2C+S">S. Di Domizio</a>, <a href="/search/physics?searchtype=author&query=Di+Lorenzo%2C+S">S. Di Lorenzo</a>, <a href="/search/physics?searchtype=author&query=Dubovik%2C+O+M">O. M. Dubovik</a>, <a href="/search/physics?searchtype=author&query=Iachellini%2C+N+F">N. Ferreiro Iachellini</a>, <a href="/search/physics?searchtype=author&query=Ferroni%2C+F">F. Ferroni</a>, <a href="/search/physics?searchtype=author&query=Fiorini%2C+E">E. Fiorini</a>, <a href="/search/physics?searchtype=author&query=Fu%2C+S">S. Fu</a>, <a href="/search/physics?searchtype=author&query=Garai%2C+A">A. Garai</a>, <a href="/search/physics?searchtype=author&query=Ghislandi%2C+S">S. Ghislandi</a>, <a href="/search/physics?searchtype=author&query=Gironi%2C+L">L. Gironi</a>, <a href="/search/physics?searchtype=author&query=Gorla%2C+P">P. Gorla</a>, <a href="/search/physics?searchtype=author&query=Gotti%2C+C">C. Gotti</a>, <a href="/search/physics?searchtype=author&query=Guillaumon%2C+P+V">P. V. Guillaumon</a>, <a href="/search/physics?searchtype=author&query=Helis%2C+D+L">D. L. Helis</a>, <a href="/search/physics?searchtype=author&query=Kovtun%2C+G+P">G. P. Kovtun</a>, <a href="/search/physics?searchtype=author&query=Mancuso%2C+M">M. Mancuso</a> , et al. (19 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.05116v2-abstract-short" style="display: inline;"> One of the most energetic events in the Universe are core-collapse Supernovae (SNe), where almost all the star's binding energy is released as neutrinos. These particles are direct probes of the processes occurring in the stellar core and provide unique insights into the gravitational collapse. RES-NOVA will revolutionize how we detect neutrinos from astrophysical sources, by deploying the first t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05116v2-abstract-full').style.display = 'inline'; document.getElementById('2206.05116v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.05116v2-abstract-full" style="display: none;"> One of the most energetic events in the Universe are core-collapse Supernovae (SNe), where almost all the star's binding energy is released as neutrinos. These particles are direct probes of the processes occurring in the stellar core and provide unique insights into the gravitational collapse. RES-NOVA will revolutionize how we detect neutrinos from astrophysical sources, by deploying the first ton-scale array of cryogenic detectors made from archaeological lead. Pb offers the highest neutrino interaction cross-section via coherent elastic neutrino-nucleus scattering (CE$谓$NS). Such process will enable RES-NOVA to be equally sensitive to all neutrino flavors. For the first time, we propose to use archaeological Pb as sensitive target material in order to achieve an ultra-low background level in the region of interest (\textit{O}(1keV)). All these features make possible the deployment of the first cm-scale neutrino telescope for the investigation of astrophysical sources. In this contribution, we will characterize the radiopurity level and the performance of a small-scale proof-of-principle detector of RES-NOVA, consisting in a PbWO$_4$ crystal made from archaeological-Pb operated as cryogenic detector. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05116v2-abstract-full').style.display = 'none'; document.getElementById('2206.05116v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.02154">arXiv:2205.02154</a> <span> [<a href="https://arxiv.org/pdf/2205.02154">pdf</a>, <a href="https://arxiv.org/format/2205.02154">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.asr.2022.05.016">10.1016/j.asr.2022.05.016 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First results from the ENTOTO neutron monitor: Quantifying the waiting time distribution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Strauss%2C+R+D">R. D. Strauss</a>, <a href="/search/physics?searchtype=author&query=Giday%2C+N+M">Nigussie M. Giday</a>, <a href="/search/physics?searchtype=author&query=Seba%2C+E+B">Ephrem B. Seba</a>, <a href="/search/physics?searchtype=author&query=Chekole%2C+D+A">Daniel A. Chekole</a>, <a href="/search/physics?searchtype=author&query=Garuma%2C+G+F">Gemechu F. Garuma</a>, <a href="/search/physics?searchtype=author&query=Kassa%2C+B+H">Bereket H. Kassa</a>, <a href="/search/physics?searchtype=author&query=Dugassa%2C+T">Teshome Dugassa</a>, <a href="/search/physics?searchtype=author&query=Diedericks%2C+C">C. Diedericks</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2205.02154v1-abstract-short" style="display: inline;"> We discuss a newly established neutron monitor station installed at the ENTOTO Observatory Research Center outside of Addis Ababa, Ethiopia. This is a version of a mini-neutron monitor, recently upgraded to detect individual neutrons and able to calculate the waiting time distribution between neutron pulses down to $\sim 1 $ $渭$s. From the waiting time distribution we define and calculate a new qu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.02154v1-abstract-full').style.display = 'inline'; document.getElementById('2205.02154v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.02154v1-abstract-full" style="display: none;"> We discuss a newly established neutron monitor station installed at the ENTOTO Observatory Research Center outside of Addis Ababa, Ethiopia. This is a version of a mini-neutron monitor, recently upgraded to detect individual neutrons and able to calculate the waiting time distribution between neutron pulses down to $\sim 1 $ $渭$s. From the waiting time distribution we define and calculate a new quantity, the correlation ratio, as the ratio of correlated to uncorrelated neutrons measured inside the monitor. We propose that this quantity can, in future, be used as a proxy for spectral index of atmospheric particles incident on the monitor and show that this quantity has a weak pressure dependence. We believe that future measurements from the ENTOTO mini-neutron monitor will contribute towards the understanding of cosmic ray acceleration and transport in the heliosphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.02154v1-abstract-full').style.display = 'none'; document.getElementById('2205.02154v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to Advances in Space Research spacial issue: Space and Geophysical Observations and Recent Results related to the African Continent</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.07441">arXiv:2203.07441</a> <span> [<a href="https://arxiv.org/pdf/2203.07441">pdf</a>, <a href="https://arxiv.org/format/2203.07441">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-022-10656-8">10.1140/epjc/s10052-022-10656-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radiopurity of a kg-scale PbWO$_4$ cryogenic detector produced from archaeological Pb for the RES-NOVA experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Beeman%2C+J+W">J. W. Beeman</a>, <a href="/search/physics?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/physics?searchtype=author&query=Bucci%2C+C">C. Bucci</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=Carniti%2C+P">P. Carniti</a>, <a href="/search/physics?searchtype=author&query=Celi%2C+E">E. Celi</a>, <a href="/search/physics?searchtype=author&query=Clemenza%2C+M">M. Clemenza</a>, <a href="/search/physics?searchtype=author&query=D%27Addabbo%2C+A">A. D'Addabbo</a>, <a href="/search/physics?searchtype=author&query=Danevich%2C+F+A">F. A. Danevich</a>, <a href="/search/physics?searchtype=author&query=Di+Domizio%2C+S">S. Di Domizio</a>, <a href="/search/physics?searchtype=author&query=Di+Lorenzo%2C+S">S. Di Lorenzo</a>, <a href="/search/physics?searchtype=author&query=Dubovik%2C+O+M">O. M. Dubovik</a>, <a href="/search/physics?searchtype=author&query=Iachellini%2C+N+F">N. Ferreiro Iachellini</a>, <a href="/search/physics?searchtype=author&query=Ferroni%2C+F">F. Ferroni</a>, <a href="/search/physics?searchtype=author&query=Fiorini%2C+E">E. Fiorini</a>, <a href="/search/physics?searchtype=author&query=Fu%2C+S">S. Fu</a>, <a href="/search/physics?searchtype=author&query=Garai%2C+A">A. Garai</a>, <a href="/search/physics?searchtype=author&query=Ghislandi%2C+S">S. Ghislandi</a>, <a href="/search/physics?searchtype=author&query=Gironi%2C+L">L. Gironi</a>, <a href="/search/physics?searchtype=author&query=Gorla%2C+P">P. Gorla</a>, <a href="/search/physics?searchtype=author&query=Gotti%2C+C">C. Gotti</a>, <a href="/search/physics?searchtype=author&query=Guillaumon%2C+P+V">P. V. Guillaumon</a>, <a href="/search/physics?searchtype=author&query=Helis%2C+D+L">D. L. Helis</a>, <a href="/search/physics?searchtype=author&query=Kovtun%2C+G+P">G. P. Kovtun</a>, <a href="/search/physics?searchtype=author&query=Mancuso%2C+M">M. Mancuso</a> , et al. (19 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.07441v2-abstract-short" style="display: inline;"> RES-NOVA is a newly proposed experiment for the detection of neutrinos from astrophysical sources, mainly Supernovae, using an array of cryogenic detectors made of PbWO$_4$ crystals produced from archaeological Pb. This unconventional material, characterized by intrinsic high radiopurity, enables to achieve low-background levels in the region of interest for the neutrino detection via Coherent Ela… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07441v2-abstract-full').style.display = 'inline'; document.getElementById('2203.07441v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.07441v2-abstract-full" style="display: none;"> RES-NOVA is a newly proposed experiment for the detection of neutrinos from astrophysical sources, mainly Supernovae, using an array of cryogenic detectors made of PbWO$_4$ crystals produced from archaeological Pb. This unconventional material, characterized by intrinsic high radiopurity, enables to achieve low-background levels in the region of interest for the neutrino detection via Coherent Elastic neutrino-Nucleus Scattering (CE$谓$NS). This signal lies at the detector energy threshold, O(1 keV), and it is expected to be hidden by naturally occurring radioactive contaminants of the crystal absorber. Here, we present the results of a radiopurity assay on a 0.84 kg PbWO$_4$ crystal produced from archaeological Pb operated as a cryogenic detector. The crystal internal radioactive contaminations are: $^{232}$Th $<$40 $渭$Bq/kg, $^{238}$U $<$30 $渭$Bq/kg, $^{226}$Ra 1.3 mBq/kg and $^{210}$Pb 22.5 mBq/kg. We present also a background projection for the final experiment and possible mitigation strategies for further background suppression. The achieved results demonstrate the feasibility of realizing this new class of detectors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07441v2-abstract-full').style.display = 'none'; document.getElementById('2203.07441v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">New analysis with high statistic</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C (2022) 82:692 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.11320">arXiv:2202.11320</a> <span> [<a href="https://arxiv.org/pdf/2202.11320">pdf</a>, <a href="https://arxiv.org/format/2202.11320">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac582a">10.3847/1538-4357/ac582a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmic ray transport near the Sun </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Strauss%2C+R+D">R. D. Strauss</a>, <a href="/search/physics?searchtype=author&query=Berg%2C+J+P+v+d">J. P. van den Berg</a>, <a href="/search/physics?searchtype=author&query=Rankin%2C+J+S">J. S. Rankin</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2202.11320v1-abstract-short" style="display: inline;"> The strongly diverging magnetic field lines in the very inner heliosphere, through the associated magnetic focusing/mirroring forces, can, potentially, lead to highly anisotropic galactic cosmic ray distributions close to the Sun. Using a simplified analytical approach, validated by numerical simulations, we study the behaviour of the galactic cosmic ray distribution in this newly explored region… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.11320v1-abstract-full').style.display = 'inline'; document.getElementById('2202.11320v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.11320v1-abstract-full" style="display: none;"> The strongly diverging magnetic field lines in the very inner heliosphere, through the associated magnetic focusing/mirroring forces, can, potentially, lead to highly anisotropic galactic cosmic ray distributions close to the Sun. Using a simplified analytical approach, validated by numerical simulations, we study the behaviour of the galactic cosmic ray distribution in this newly explored region of the heliosphere and find that significant anisotropies can be expected inside 0.2 au. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.11320v1-abstract-full').style.display = 'none'; document.getElementById('2202.11320v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.05097">arXiv:2202.05097</a> <span> [<a href="https://arxiv.org/pdf/2202.05097">pdf</a>, <a href="https://arxiv.org/format/2202.05097">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.21468/SciPostPhysProc.9.001">10.21468/SciPostPhysProc.9.001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> EXCESS workshop: Descriptions of rising low-energy spectra </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adari%2C+P">P. Adari</a>, <a href="/search/physics?searchtype=author&query=Aguilar-Arevalo%2C+A">A. Aguilar-Arevalo</a>, <a href="/search/physics?searchtype=author&query=Amidei%2C+D">D. Amidei</a>, <a href="/search/physics?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/physics?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/physics?searchtype=author&query=Augier%2C+C">C. Augier</a>, <a href="/search/physics?searchtype=author&query=Balogh%2C+L">L. Balogh</a>, <a href="/search/physics?searchtype=author&query=Banik%2C+S">S. Banik</a>, <a href="/search/physics?searchtype=author&query=Baxter%2C+D">D. Baxter</a>, <a href="/search/physics?searchtype=author&query=Beaufort%2C+C">C. Beaufort</a>, <a href="/search/physics?searchtype=author&query=Beaulieu%2C+G">G. Beaulieu</a>, <a href="/search/physics?searchtype=author&query=Belov%2C+V">V. Belov</a>, <a href="/search/physics?searchtype=author&query=Gal%2C+Y+B">Y. Ben Gal</a>, <a href="/search/physics?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/physics?searchtype=author&query=Beno%C3%AEt%2C+A">A. Beno卯t</a>, <a href="/search/physics?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/physics?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/physics?searchtype=author&query=Bertolini%2C+A">A. Bertolini</a>, <a href="/search/physics?searchtype=author&query=Bhattacharyya%2C+R">R. Bhattacharyya</a>, <a href="/search/physics?searchtype=author&query=Billard%2C+J">J. Billard</a>, <a href="/search/physics?searchtype=author&query=Bloch%2C+I+M">I. M. Bloch</a>, <a href="/search/physics?searchtype=author&query=Botti%2C+A">A. Botti</a>, <a href="/search/physics?searchtype=author&query=Breier%2C+R">R. Breier</a>, <a href="/search/physics?searchtype=author&query=Bres%2C+G">G. Bres</a>, <a href="/search/physics?searchtype=author&query=Bret%2C+J+L">J-. L. Bret</a> , et al. (281 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2202.05097v2-abstract-short" style="display: inline;"> Many low-threshold experiments observe sharply rising event rates of yet unknown origins below a few hundred eV, and larger than expected from known backgrounds. Due to the significant impact of this excess on the dark matter or neutrino sensitivity of these experiments, a collective effort has been started to share the knowledge about the individual observations. For this, the EXCESS Workshop was… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.05097v2-abstract-full').style.display = 'inline'; document.getElementById('2202.05097v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.05097v2-abstract-full" style="display: none;"> Many low-threshold experiments observe sharply rising event rates of yet unknown origins below a few hundred eV, and larger than expected from known backgrounds. Due to the significant impact of this excess on the dark matter or neutrino sensitivity of these experiments, a collective effort has been started to share the knowledge about the individual observations. For this, the EXCESS Workshop was initiated. In its first iteration in June 2021, ten rare event search collaborations contributed to this initiative via talks and discussions. The contributing collaborations were CONNIE, CRESST, DAMIC, EDELWEISS, MINER, NEWS-G, NUCLEUS, RICOCHET, SENSEI and SuperCDMS. They presented data about their observed energy spectra and known backgrounds together with details about the respective measurements. In this paper, we summarize the presented information and give a comprehensive overview of the similarities and differences between the distinct measurements. The provided data is furthermore publicly available on the workshop's data repository together with a plotting tool for visualization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.05097v2-abstract-full').style.display = 'none'; document.getElementById('2202.05097v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">44 pages, 20 figures; Editors: A. Fuss, M. Kaznacheeva, F. Reindl, F. Wagner; updated copyright statements and funding information</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> SciPost Phys. Proc. 9, 001 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.03991">arXiv:2202.03991</a> <span> [<a href="https://arxiv.org/pdf/2202.03991">pdf</a>, <a href="https://arxiv.org/format/2202.03991">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/17/05/T05020">10.1088/1748-0221/17/05/T05020 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Development of a compact muon veto for the NUCLEUS experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Wagner%2C+V">V. Wagner</a>, <a href="/search/physics?searchtype=author&query=Rogly%2C+R">R. Rogly</a>, <a href="/search/physics?searchtype=author&query=Erhart%2C+A">A. Erhart</a>, <a href="/search/physics?searchtype=author&query=Savu%2C+V">V. Savu</a>, <a href="/search/physics?searchtype=author&query=Goupy%2C+C">C. Goupy</a>, <a href="/search/physics?searchtype=author&query=Lhuillier%2C+D">D. Lhuillier</a>, <a href="/search/physics?searchtype=author&query=Vivier%2C+M">M. Vivier</a>, <a href="/search/physics?searchtype=author&query=Klinkenberg%2C+L">L. Klinkenberg</a>, <a href="/search/physics?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/physics?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=Cappella%2C+F">F. Cappella</a>, <a href="/search/physics?searchtype=author&query=Cardani%2C+L">L. Cardani</a>, <a href="/search/physics?searchtype=author&query=Casali%2C+N">N. Casali</a>, <a href="/search/physics?searchtype=author&query=Cerulli%2C+R">R. Cerulli</a>, <a href="/search/physics?searchtype=author&query=Colantoni%2C+I">I. Colantoni</a>, <a href="/search/physics?searchtype=author&query=Cruciani%2C+A">A. Cruciani</a>, <a href="/search/physics?searchtype=author&query=del+Castello%2C+G">G. del Castello</a>, <a href="/search/physics?searchtype=author&query=Friedl%2C+M">M. Friedl</a>, <a href="/search/physics?searchtype=author&query=Garai%2C+A">A. Garai</a>, <a href="/search/physics?searchtype=author&query=Ghete%2C+V+M">V. M. Ghete</a>, <a href="/search/physics?searchtype=author&query=Guidi%2C+V">V. Guidi</a>, <a href="/search/physics?searchtype=author&query=Hauff%2C+D">D. Hauff</a>, <a href="/search/physics?searchtype=author&query=Kaznacheeva%2C+M">M. Kaznacheeva</a>, <a href="/search/physics?searchtype=author&query=Kinast%2C+A">A. Kinast</a> , et al. (30 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2202.03991v2-abstract-short" style="display: inline;"> The NUCLEUS experiment aims to measure coherent elastic neutrino nucleus scattering of reactor anti-neutrinos using cryogenic calorimeters. Operating at an overburden of 3 m.w.e., muon-induced backgrounds are expected to be one of the dominant background contributions. Besides a high efficiency to identify muon events passing the experimental setup, the NUCLEUS muon veto has to fulfill tight spati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.03991v2-abstract-full').style.display = 'inline'; document.getElementById('2202.03991v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.03991v2-abstract-full" style="display: none;"> The NUCLEUS experiment aims to measure coherent elastic neutrino nucleus scattering of reactor anti-neutrinos using cryogenic calorimeters. Operating at an overburden of 3 m.w.e., muon-induced backgrounds are expected to be one of the dominant background contributions. Besides a high efficiency to identify muon events passing the experimental setup, the NUCLEUS muon veto has to fulfill tight spatial requirements to fit the constraints given by the experimental site and to minimize the induced detector dead-time. We developed highly efficient and compact muon veto modules based on plastic scintillators equipped with wavelength shifting fibers and silicon photo multipliers to collect and detect the scintillation light. In this paper, we present the full characterization of a prototype module with different light read-out configurations. We conclude that an efficient and compact muon veto system can be built for the NUCLEUS experiment from a cube assembly of the developed modules. Simulations show that an efficiency for muon identification of >99 % and an associated rate of 325 Hz is achievable, matching the requirements of the NUCLEUS experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.03991v2-abstract-full').style.display = 'none'; document.getElementById('2202.03991v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.03863">arXiv:2201.03863</a> <span> [<a href="https://arxiv.org/pdf/2201.03863">pdf</a>, <a href="https://arxiv.org/format/2201.03863">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-022-10140-3">10.1140/epjc/s10052-022-10140-3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing spin-dependent dark matter interactions with $^6$Li </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/physics?searchtype=author&query=Benato%2C+G">G. Benato</a>, <a href="/search/physics?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/physics?searchtype=author&query=Bertoldo%2C+E">E. Bertoldo</a>, <a href="/search/physics?searchtype=author&query=Bertolini%2C+A">A. Bertolini</a>, <a href="/search/physics?searchtype=author&query=Breier%2C+R">R. Breier</a>, <a href="/search/physics?searchtype=author&query=Bucci%2C+C">C. Bucci</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=D%27Addabbo%2C+A">A. D'Addabbo</a>, <a href="/search/physics?searchtype=author&query=Di+Lorenzo%2C+S">S. Di Lorenzo</a>, <a href="/search/physics?searchtype=author&query=Einfalt%2C+L">L. Einfalt</a>, <a href="/search/physics?searchtype=author&query=Erb%2C+A">A. Erb</a>, <a href="/search/physics?searchtype=author&query=Feilitzsch%2C+F+v">F. v. Feilitzsch</a>, <a href="/search/physics?searchtype=author&query=Iachellini%2C+N+F">N. Ferreiro Iachellini</a>, <a href="/search/physics?searchtype=author&query=Fichtinger%2C+S">S. Fichtinger</a>, <a href="/search/physics?searchtype=author&query=Fuchs%2C+D">D. Fuchs</a>, <a href="/search/physics?searchtype=author&query=Fuss%2C+A">A. Fuss</a>, <a href="/search/physics?searchtype=author&query=Garai%2C+A">A. Garai</a>, <a href="/search/physics?searchtype=author&query=Ghete%2C+V+M">V. M. Ghete</a>, <a href="/search/physics?searchtype=author&query=Gorla%2C+P">P. Gorla</a>, <a href="/search/physics?searchtype=author&query=Gupta%2C+S">S. Gupta</a>, <a href="/search/physics?searchtype=author&query=Hauff%2C+D">D. Hauff</a>, <a href="/search/physics?searchtype=author&query=Je%C5%A1kovsk%C3%BD%2C+M">M. Je拧kovsk媒</a>, <a href="/search/physics?searchtype=author&query=Jochum%2C+J">J. Jochum</a>, <a href="/search/physics?searchtype=author&query=Kaznacheeva%2C+M">M. Kaznacheeva</a> , et al. (33 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.03863v1-abstract-short" style="display: inline;"> CRESST is one of the most prominent direct detection experiments for dark matter particles with sub-GeV/c$^2$ mass. One of the advantages of the CRESST experiment is the possibility to include a large variety of nuclides in the target material used to probe dark matter interactions. In this work, we discuss in particular the interactions of dark matter particles with protons and neutrons of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.03863v1-abstract-full').style.display = 'inline'; document.getElementById('2201.03863v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.03863v1-abstract-full" style="display: none;"> CRESST is one of the most prominent direct detection experiments for dark matter particles with sub-GeV/c$^2$ mass. One of the advantages of the CRESST experiment is the possibility to include a large variety of nuclides in the target material used to probe dark matter interactions. In this work, we discuss in particular the interactions of dark matter particles with protons and neutrons of $^{6}$Li. This is now possible thanks to new calculations on nuclear matrix elements of this specific isotope of Li. To show the potential of using this particular nuclide for probing dark matter interactions, we used the data collected previously by a CRESST prototype based on LiAlO$_2$ and operated in an above ground test-facility at Max-Planck-Institut f眉r Physik in Munich, Germany. In particular, the inclusion of $^{6}$Li in the limit calculation drastically improves the result obtained for spin-dependent interactions with neutrons in the whole mass range. The improvement is significant, greater than two order of magnitude for dark matter masses below 1 GeV/c$^2$, compared to the limit previously published with the same data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.03863v1-abstract-full').style.display = 'none'; document.getElementById('2201.03863v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.03601">arXiv:2110.03601</a> <span> [<a href="https://arxiv.org/pdf/2110.03601">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac348f">10.3847/1538-4357/ac348f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Anomalous Cosmic Ray Oxygen Observations in to 0.1 au </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Rankin%2C+J+S">Jamie S. Rankin</a>, <a href="/search/physics?searchtype=author&query=McComas%2C+D+J">David J. McComas</a>, <a href="/search/physics?searchtype=author&query=Leske%2C+R+A">Richard A. Leske</a>, <a href="/search/physics?searchtype=author&query=Christian%2C+E+R">Eric R. Christian</a>, <a href="/search/physics?searchtype=author&query=Cohen%2C+C+M+S">Christina M. S. Cohen</a>, <a href="/search/physics?searchtype=author&query=Cummings%2C+A+C">Alan C. Cummings</a>, <a href="/search/physics?searchtype=author&query=Joyce%2C+C+J">Colin J. Joyce</a>, <a href="/search/physics?searchtype=author&query=Labrador%2C+A+W">Allan W. Labrador</a>, <a href="/search/physics?searchtype=author&query=Mewaldt%2C+R+A">Richard A. Mewaldt</a>, <a href="/search/physics?searchtype=author&query=Schwadron%2C+N+A">Nathan A. Schwadron</a>, <a href="/search/physics?searchtype=author&query=Stone%2C+E+C">Edward C. Stone</a>, <a href="/search/physics?searchtype=author&query=Strauss%2C+R+D+T">R. Du Toit Strauss</a>, <a href="/search/physics?searchtype=author&query=Wiedenbeck%2C+M+E">Mark E. Wiedenbeck</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.03601v1-abstract-short" style="display: inline;"> The Integrated Science Investigation of the Sun instrument suite onboard NASA's Parker Solar Probe mission continues to measure solar energetic particles and cosmic rays closer to the Sun than ever before. Here, we present the first observations of cosmic rays into 0.1 au (21.5 solar radii), focusing specifically on oxygen from ~2018.7 to ~2021.2. Our energy spectra reveal an anomalous cosmic ray-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.03601v1-abstract-full').style.display = 'inline'; document.getElementById('2110.03601v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.03601v1-abstract-full" style="display: none;"> The Integrated Science Investigation of the Sun instrument suite onboard NASA's Parker Solar Probe mission continues to measure solar energetic particles and cosmic rays closer to the Sun than ever before. Here, we present the first observations of cosmic rays into 0.1 au (21.5 solar radii), focusing specifically on oxygen from ~2018.7 to ~2021.2. Our energy spectra reveal an anomalous cosmic ray-dominated profile that is comparable to that at 1 au, across multiple solar cycle minima. The galactic cosmic ray-dominated component is similar to that of the previous solar minimum (Solar Cycle 24/25 compared to 23/24) but elevated compared to the past (Solar Cycle 20/21). The findings are generally consistent with the current trend of unusually weak solar modulation that originated during the previous solar minimum and continues today. We also find a strong radial intensity gradient: 49.4 +/- 8.0 %/au from 0.1 to 0.94 au, for energies of 6.9 to 27 MeV/nuc. This value agrees with that measured by Helios nearly 45 years ago from 0.3 to 1.0 au (48 +/- 12 %/au; 9 to 29 MeV/nuc) and is larger than predicted by models. The large ACR gradients observed close to the Sun by the Parker Solar Probe Integrated Science Investigation of the Sun instrument suite found here suggest that intermediate-scale variations in the magnetic field's structure strongly influences cosmic ray drifts, well inside 1 au. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.03601v1-abstract-full').style.display = 'none'; document.getElementById('2110.03601v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.08376">arXiv:2109.08376</a> <span> [<a href="https://arxiv.org/pdf/2109.08376">pdf</a>, <a href="https://arxiv.org/format/2109.08376">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac2736">10.3847/1538-4357/ac2736 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On the Turbulent Reduction of Drifts for Solar Energetic Particles </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Berg%2C+J+P+v+d">J. P. van den Berg</a>, <a href="/search/physics?searchtype=author&query=Engelbrecht%2C+N+E">N. E. Engelbrecht</a>, <a href="/search/physics?searchtype=author&query=Wijsen%2C+N">N. Wijsen</a>, <a href="/search/physics?searchtype=author&query=Strauss%2C+R+D">R. D. Strauss</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.08376v1-abstract-short" style="display: inline;"> Particle drifts perpendicular to the background magnetic field have been proposed by some authors as an explanation for the very efficient perpendicular transport of solar energetic particles (SEPs). This process, however, competes with perpendicular diffusion caused by magnetic turbulence, which can also disrupt the drift patterns and reduce the efficiency of drift effects. The latter phenomenon… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.08376v1-abstract-full').style.display = 'inline'; document.getElementById('2109.08376v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.08376v1-abstract-full" style="display: none;"> Particle drifts perpendicular to the background magnetic field have been proposed by some authors as an explanation for the very efficient perpendicular transport of solar energetic particles (SEPs). This process, however, competes with perpendicular diffusion caused by magnetic turbulence, which can also disrupt the drift patterns and reduce the efficiency of drift effects. The latter phenomenon is well known in cosmic ray studies, but not yet considered in SEP models. Additionally, SEP models which do not include drifts, especially for electrons, use turbulent drift reduction as a justification of this omission, without critically evaluating or testing this assumption. This article presents the first theoretical step for a theory of drift suppression in SEP transport. This is done by deriving the turbulence-dependent drift reduction function with a pitch-angle dependence, as applicable for anisotropic particle distributions, and by investigating to what extent drifts will be reduced in the inner heliosphere for realistic turbulence conditions and different pitch-angle dependencies of the perpendicular diffusion coefficient. The influence of the derived turbulent drift reduction factors on the transport of SEPs are tested, using a state-of-the-art SEP transport code, for several expressions of theoretically-derived perpendicular diffusion coefficients. It is found, for realistic turbulence conditions in the inner heliosphere, that cross-field diffusion will have the largest influence on the perpendicular transport of SEPs, as opposed to particle drifts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.08376v1-abstract-full').style.display = 'none'; document.getElementById('2109.08376v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">This is a pre-print of an article accepted for publication in The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.14289">arXiv:2107.14289</a> <span> [<a href="https://arxiv.org/pdf/2107.14289">pdf</a>, <a href="https://arxiv.org/format/2107.14289">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.asr.2021.05.032">10.1016/j.asr.2021.05.032 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The updated SANAE neutron monitor </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Strauss%2C+R+D">R. D. Strauss</a>, <a href="/search/physics?searchtype=author&query=van+der+Merwe%2C+C">C. van der Merwe</a>, <a href="/search/physics?searchtype=author&query=Diedericks%2C+C">C. Diedericks</a>, <a href="/search/physics?searchtype=author&query=Kruger%2C+H">H. Kruger</a>, <a href="/search/physics?searchtype=author&query=Kruger%2C+H+G">H. G. Kruger</a>, <a href="/search/physics?searchtype=author&query=Moloto%2C+K+D">K. D. Moloto</a>, <a href="/search/physics?searchtype=author&query=Lotz%2C+S">S. Lotz</a>, <a href="/search/physics?searchtype=author&query=Mosotho%2C+G+M">G. M. Mosotho</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.14289v1-abstract-short" style="display: inline;"> Neutron monitors have been the premier ground-based instruments for monitoring the near-Earth cosmic ray flux for more than 70 years. It is essential to continue with such measurements in order to extend this unique long-term time series. Moreover, with the recent interest of the aviation industry to space weather effects, and especially the radiation risk posed by solar energetic particles and ga… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.14289v1-abstract-full').style.display = 'inline'; document.getElementById('2107.14289v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.14289v1-abstract-full" style="display: none;"> Neutron monitors have been the premier ground-based instruments for monitoring the near-Earth cosmic ray flux for more than 70 years. It is essential to continue with such measurements in order to extend this unique long-term time series. Moreover, with the recent interest of the aviation industry to space weather effects, and especially the radiation risk posed by solar energetic particles and galactic cosmic rays, it is vital to extend the current neutron monitor network in order to provide near-real-time measurements to the space weather community. In this paper we discuss a new electronics system that was retrofitted to the SANAE neutron monitor in Antarctica. We present initial results from this system, featuring very high temporal resolution and discuss the techniques applied to the data analysis. Based on these successful upgrades, we are confident that this system can be used to rejuvenate the aligning neutron monitor network, and even possibly to revive some of the decommissioned instruments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.14289v1-abstract-full').style.display = 'none'; document.getElementById('2107.14289v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to Advances in Space Research</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.01186">arXiv:2105.01186</a> <span> [<a href="https://arxiv.org/pdf/2105.01186">pdf</a>, <a href="https://arxiv.org/format/2105.01186">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1741-4326/ac0b35">10.1088/1741-4326/ac0b35 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Approach to nonlinear magnetohydrodynamic simulations in stellarator geometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Zhou%2C+Y">Yao Zhou</a>, <a href="/search/physics?searchtype=author&query=Ferraro%2C+N+M">N. M. Ferraro</a>, <a href="/search/physics?searchtype=author&query=Jardin%2C+S+C">S. C. Jardin</a>, <a href="/search/physics?searchtype=author&query=Strauss%2C+H+R">H. R. Strauss</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2105.01186v2-abstract-short" style="display: inline;"> The capability to model the nonlinear magnetohydrodynamic (MHD) evolution of stellarator plasmas is developed by extending the M3D-$C^1$ code to allow non-axisymmetric domain geometry. We introduce a set of logical coordinates, in which the computational domain is axisymmetric, to utilize the existing finite-element framework of M3D-$C^1$. A $C^1$ coordinate mapping connects the logical domain to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.01186v2-abstract-full').style.display = 'inline'; document.getElementById('2105.01186v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.01186v2-abstract-full" style="display: none;"> The capability to model the nonlinear magnetohydrodynamic (MHD) evolution of stellarator plasmas is developed by extending the M3D-$C^1$ code to allow non-axisymmetric domain geometry. We introduce a set of logical coordinates, in which the computational domain is axisymmetric, to utilize the existing finite-element framework of M3D-$C^1$. A $C^1$ coordinate mapping connects the logical domain to the non-axisymmetric physical domain, where we use the M3D-$C^1$ extended MHD models essentially without modifications. We present several numerical verifications on the implementation of this approach, including simulations of the heating, destabilization, and equilibration of stellarator plasmas with strongly anisotropic thermal conductivity, and of the relaxation of stellarator equilibria to integrable and non-integrable magnetic field configurations in realistic geometries. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.01186v2-abstract-full').style.display = 'none'; document.getElementById('2105.01186v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 6 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl. Fusion 61, 086015 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.08672">arXiv:2103.08672</a> <span> [<a href="https://arxiv.org/pdf/2103.08672">pdf</a>, <a href="https://arxiv.org/format/2103.08672">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2021/10/064">10.1088/1475-7516/2021/10/064 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> RES-NOVA sensitivity to core-collapse and failed core-collapse supernova neutrinos </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Pattavina%2C+L">L. Pattavina</a>, <a href="/search/physics?searchtype=author&query=Iachellini%2C+N+F">N. Ferreiro Iachellini</a>, <a href="/search/physics?searchtype=author&query=Pagnanini%2C+L">L. Pagnanini</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=Celi%2C+E">E. Celi</a>, <a href="/search/physics?searchtype=author&query=Clemenza%2C+M">M. Clemenza</a>, <a href="/search/physics?searchtype=author&query=Ferroni%2C+F">F. Ferroni</a>, <a href="/search/physics?searchtype=author&query=Fiorini%2C+E">E. Fiorini</a>, <a href="/search/physics?searchtype=author&query=Garai%2C+A">A. Garai</a>, <a href="/search/physics?searchtype=author&query=Gironi%2C+L">L. Gironi</a>, <a href="/search/physics?searchtype=author&query=Mancuso%2C+M">M. Mancuso</a>, <a href="/search/physics?searchtype=author&query=Nisi%2C+S">S. Nisi</a>, <a href="/search/physics?searchtype=author&query=Petricca%2C+F">F. Petricca</a>, <a href="/search/physics?searchtype=author&query=Pirro%2C+S">S. Pirro</a>, <a href="/search/physics?searchtype=author&query=Pozzi%2C+S">S. Pozzi</a>, <a href="/search/physics?searchtype=author&query=Puiu%2C+A">A. Puiu</a>, <a href="/search/physics?searchtype=author&query=Rothe%2C+J">J. Rothe</a>, <a href="/search/physics?searchtype=author&query=Schoenert%2C+S">S. Schoenert</a>, <a href="/search/physics?searchtype=author&query=Shtembari%2C+L">L. Shtembari</a>, <a href="/search/physics?searchtype=author&query=Strauss%2C+R">R. Strauss</a>, <a href="/search/physics?searchtype=author&query=Wagner%2C+V">V. Wagner</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2103.08672v3-abstract-short" style="display: inline;"> RES-NOVA is a new proposed experiment for the investigation of astrophysical neutrino sources with archaeological Pb-based cryogenic detectors. RES-NOVA will exploit Coherent Elastic neutrino-Nucleus Scattering (CE$谓$NS) as detection channel, thus it will be equally sensitive to all neutrino flavors produced by Supernovae (SNe). RES-NOVA with only a total active volume of (60 cm)$^3$ and an energy… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.08672v3-abstract-full').style.display = 'inline'; document.getElementById('2103.08672v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.08672v3-abstract-full" style="display: none;"> RES-NOVA is a new proposed experiment for the investigation of astrophysical neutrino sources with archaeological Pb-based cryogenic detectors. RES-NOVA will exploit Coherent Elastic neutrino-Nucleus Scattering (CE$谓$NS) as detection channel, thus it will be equally sensitive to all neutrino flavors produced by Supernovae (SNe). RES-NOVA with only a total active volume of (60 cm)$^3$ and an energy threshold of 1 keV will probe the entire Milky Way Galaxy for (failed) core-collapse SNe with $> 3 蟽$ detection significance. The high detector modularity makes RES-NOVA ideal also for reconstructing the main parameters (e.g. average neutrino energy, star binding energy) of SNe occurring in our vicinity, without deterioration of the detector performance caused by the high neutrino interaction rate. For the first time, distances $<3$ kpc can be surveyed, similarly to the ones where all known past galactic SNe happened. We discuss the RES-NOVA potential, accounting for a realistic setup, considering the detector geometry, modularity and background level in the region of interest. We report on the RES-NOVA background model and on the sensitivity to SN neutrinos as a function of the distance travelled by neutrinos. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.08672v3-abstract-full').style.display = 'none'; document.getElementById('2103.08672v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 10 (2021) 064 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.07570">arXiv:2012.07570</a> <span> [<a href="https://arxiv.org/pdf/2012.07570">pdf</a>, <a href="https://arxiv.org/format/2012.07570">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s11214-020-00771-x">10.1007/s11214-020-00771-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Primer on Focused Solar Energetic Particle Transport: Basic physics and recent modelling results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Berg%2C+J+P+v+d">J. P. van den Berg</a>, <a href="/search/physics?searchtype=author&query=Strauss%2C+R+D">R. D. Strauss</a>, <a href="/search/physics?searchtype=author&query=Effenberger%2C+F">F. Effenberger</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.07570v1-abstract-short" style="display: inline;"> The basics of focused transport as applied to solar energetic particles are reviewed, paying special attention to areas of common misconception. The micro-physics of charged particles interacting with slab turbulence are investigated to illustrate the concept of pitch-angle scattering, where after the distribution function and focused transport equation are introduced as theoretical tools to descr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.07570v1-abstract-full').style.display = 'inline'; document.getElementById('2012.07570v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.07570v1-abstract-full" style="display: none;"> The basics of focused transport as applied to solar energetic particles are reviewed, paying special attention to areas of common misconception. The micro-physics of charged particles interacting with slab turbulence are investigated to illustrate the concept of pitch-angle scattering, where after the distribution function and focused transport equation are introduced as theoretical tools to describe the transport processes and it is discussed how observable quantities can be calculated from the distribution function. In particular, two approximations, the diffusion-advection and the telegraph equation, are compared in simplified situations to the full solution of the focused transport equation describing particle motion along a magnetic field line. It is shown that these approximations are insufficient to capture the complexity of the physical processes involved. To overcome such limitations, a finite-difference model, which is open for use by the public, is introduced to solve the focused transport equation. The use of the model is briefly discussed and it is shown how the model can be applied to reproduce an observed solar energetic electron event, providing insights into the acceleration and transport processes involved. Past work and literature on the application of these concepts are also reviewed, starting with the most basic models and building up to more complex models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.07570v1-abstract-full').style.display = 'none'; document.getElementById('2012.07570v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">This is a pre-print of an article published in Space Science Reviews. The final authenticated version is available online at: https://doi.org/10.1007/s11214-020-00771-x</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Space Science Reviews 216, 146 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.13803">arXiv:2011.13803</a> <span> [<a href="https://arxiv.org/pdf/2011.13803">pdf</a>, <a href="https://arxiv.org/format/2011.13803">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/16/07/P07032">10.1088/1748-0221/16/07/P07032 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Calibration of nuclear recoils at the 100 eV scale using neutron capture </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Thulliez%2C+L">L. Thulliez</a>, <a href="/search/physics?searchtype=author&query=Lhuillier%2C+D">D. Lhuillier</a>, <a href="/search/physics?searchtype=author&query=Cappella%2C+F">F. Cappella</a>, <a href="/search/physics?searchtype=author&query=Casali%2C+N">N. Casali</a>, <a href="/search/physics?searchtype=author&query=Cerulli%2C+R">R. Cerulli</a>, <a href="/search/physics?searchtype=author&query=Chalil%2C+A">A. Chalil</a>, <a href="/search/physics?searchtype=author&query=Chebboubi%2C+A">A. Chebboubi</a>, <a href="/search/physics?searchtype=author&query=Dumonteil%2C+E">E. Dumonteil</a>, <a href="/search/physics?searchtype=author&query=Erhart%2C+A">A. Erhart</a>, <a href="/search/physics?searchtype=author&query=Giuliani%2C+A">A. Giuliani</a>, <a href="/search/physics?searchtype=author&query=Gunsing%2C+F">F. Gunsing</a>, <a href="/search/physics?searchtype=author&query=Jericha%2C+E">E. Jericha</a>, <a href="/search/physics?searchtype=author&query=Kaznacheeva%2C+M">M. Kaznacheeva</a>, <a href="/search/physics?searchtype=author&query=Kinast%2C+A">A. Kinast</a>, <a href="/search/physics?searchtype=author&query=Langenk%C3%A4mper%2C+A">A. Langenk盲mper</a>, <a href="/search/physics?searchtype=author&query=Lasserre%2C+T">T. Lasserre</a>, <a href="/search/physics?searchtype=author&query=Letourneau%2C+A">A. Letourneau</a>, <a href="/search/physics?searchtype=author&query=Litaize%2C+O">O. Litaize</a>, <a href="/search/physics?searchtype=author&query=de+Marcillac%2C+P">P. de Marcillac</a>, <a href="/search/physics?searchtype=author&query=Marnieros%2C+S">S. Marnieros</a>, <a href="/search/physics?searchtype=author&query=Materna%2C+T">T. Materna</a>, <a href="/search/physics?searchtype=author&query=Mauri%2C+B">B. Mauri</a>, <a href="/search/physics?searchtype=author&query=Mazzucato%2C+E">E. Mazzucato</a>, <a href="/search/physics?searchtype=author&query=Nones%2C+C">C. Nones</a>, <a href="/search/physics?searchtype=author&query=Ortmann%2C+T">T. Ortmann</a> , et al. (12 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2011.13803v3-abstract-short" style="display: inline;"> The development of low-threshold detectors for the study of coherent elastic neutrino-nucleus scattering and for the search for light dark matter necessitates methods of low-energy calibration. We suggest this can be provided by the nuclear recoils resulting from the $纬$ emission following thermal neutron capture. In particular, several MeV-scale single-$纬$ transitions induce well-defined nuclear… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.13803v3-abstract-full').style.display = 'inline'; document.getElementById('2011.13803v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.13803v3-abstract-full" style="display: none;"> The development of low-threshold detectors for the study of coherent elastic neutrino-nucleus scattering and for the search for light dark matter necessitates methods of low-energy calibration. We suggest this can be provided by the nuclear recoils resulting from the $纬$ emission following thermal neutron capture. In particular, several MeV-scale single-$纬$ transitions induce well-defined nuclear recoil peaks in the 100 eV range. Using the FIFRELIN code, complete schemes of $纬$-cascades for various isotopes can be predicted with high accuracy to determine the continuous background of nuclear recoils below the calibration peaks. We present a comprehensive experimental concept for the calibration of CaWO$_4$ and Ge cryogenic detectors at a research reactor. For CaWO$_4$ the simulations show that two nuclear recoil peaks at 112.5 eV and 160.3 eV should be visible above background simply in the spectrum of the cryogenic detector. Then we discuss how the additional tagging for the associated $纬$ increases the sensitivity of the method and extends its application to a wider energy range and to Ge cryogenic detectors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.13803v3-abstract-full').style.display = 'none'; document.getElementById('2011.13803v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 8 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.08226">arXiv:2008.08226</a> <span> [<a href="https://arxiv.org/pdf/2008.08226">pdf</a>, <a href="https://arxiv.org/format/2008.08226">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Neurons and Cognition">q-bio.NC</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">cs.LG</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computational Physics">physics.comp-ph</span> </div> </div> <p class="title is-5 mathjax"> Augmenting Neural Differential Equations to Model Unknown Dynamical Systems with Incomplete State Information </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Strauss%2C+R">Robert Strauss</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2008.08226v3-abstract-short" style="display: inline;"> Neural Ordinary Differential Equations replace the right-hand side of a conventional ODE with a neural net, which by virtue of the universal approximation theorem, can be trained to the representation of any function. When we do not know the function itself, but have state trajectories (time evolution) of the ODE system we can still train the neural net to learn the representation of the underlyin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.08226v3-abstract-full').style.display = 'inline'; document.getElementById('2008.08226v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.08226v3-abstract-full" style="display: none;"> Neural Ordinary Differential Equations replace the right-hand side of a conventional ODE with a neural net, which by virtue of the universal approximation theorem, can be trained to the representation of any function. When we do not know the function itself, but have state trajectories (time evolution) of the ODE system we can still train the neural net to learn the representation of the underlying but unknown ODE. However if the state of the system is incompletely known then the right-hand side of the ODE cannot be calculated. The derivatives to propagate the system are unavailable. We show that a specially augmented Neural ODE can learn the system when given incomplete state information. As a worked example we apply neural ODEs to the Lotka-Voltera problem of 3 species, rabbits, wolves, and bears. We show that even when the data for the bear time series is removed the remaining time series of the rabbits and wolves is sufficient to learn the dynamical system despite the missing the incomplete state information. This is surprising since a conventional ODE system cannot output the correct derivatives without the full state as the input. We implement augmented neural ODEs and differential equation solvers in the julia programming language. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.08226v3-abstract-full').style.display = 'none'; document.getElementById('2008.08226v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.16768">arXiv:2006.16768</a> <span> [<a href="https://arxiv.org/pdf/2006.16768">pdf</a>, <a href="https://arxiv.org/format/2006.16768">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201936897">10.1051/0004-6361/201936897 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On the residence-time of Jovian electrons in the inner heliosphere </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Vogt%2C+A">A. Vogt</a>, <a href="/search/physics?searchtype=author&query=Engelbrecht%2C+N+E">N. E. Engelbrecht</a>, <a href="/search/physics?searchtype=author&query=Strauss%2C+R+D">R. D. Strauss</a>, <a href="/search/physics?searchtype=author&query=Heber%2C+B">B. Heber</a>, <a href="/search/physics?searchtype=author&query=Kopp%2C+A">A. Kopp</a>, <a href="/search/physics?searchtype=author&query=Herbst%2C+K">K. Herbst</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2006.16768v1-abstract-short" style="display: inline;"> Jovian electrons serve as an important test-particle distribution in the inner heliosphere and have been used extensively in the past to study the (diffusive) transport of cosmic rays in the inner heliosphere. With new limits on the Jovian source function (i.e. the particle intensity just outside the Jovian magnetosphere), and a new set of in-situ observations at 1 AU for both cases of good and po… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.16768v1-abstract-full').style.display = 'inline'; document.getElementById('2006.16768v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.16768v1-abstract-full" style="display: none;"> Jovian electrons serve as an important test-particle distribution in the inner heliosphere and have been used extensively in the past to study the (diffusive) transport of cosmic rays in the inner heliosphere. With new limits on the Jovian source function (i.e. the particle intensity just outside the Jovian magnetosphere), and a new set of in-situ observations at 1 AU for both cases of good and poor magnetic connection between the source and observer, we revisit some of these earlier simulations. We aim to find the optimal numerical set-up that can be used to simulate the propagation of 6 MeV Jovian electrons in the inner heliosphere. Using such a set-up, we further aim to study the residence (propagation) times of these particles for different levels of magnetic connection between Jupiter and an observer at Earth (1 AU). Using an advanced Jovian electron propagation model based on the stochastic differential equation (SDE) approach, we calculate the Jovian electron intensity for different model parameters. A comparison with observations leads to an optimal numerical set-up, which is then used to calculate the so-called residence (propagation) times of these particles. Comparing to in-situ observations, we are able to derive transport parameters that are appropriate to study the propagation of 6 MeV Jovian electrons in the inner heliosphere. Moreover, using these values, we show that the method of calculating the residence time applied in former literature is not suited to being interpreted as the propagation time of physical particles. This is due to an incorrect weighting of the probability distribution. We propose and apply a new method, where the results from each pseudo-particle are weighted by its resulting phase-space density (i.e. the number of physical particles that it represents). Thereby we obtain more reliable estimates for the propagation time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.16768v1-abstract-full').style.display = 'none'; document.getElementById('2006.16768v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 642, A170 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.03486">arXiv:2005.03486</a> <span> [<a href="https://arxiv.org/pdf/2005.03486">pdf</a>, <a href="https://arxiv.org/format/2005.03486">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> On the shape of SEP electron spectra: The role of interplanetary transport </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Strauss%2C+R+D+T">R. Du Toit Strauss</a>, <a href="/search/physics?searchtype=author&query=Dresing%2C+N">Nina Dresing</a>, <a href="/search/physics?searchtype=author&query=Kollhoff%2C+A">Alexander Kollhoff</a>, <a href="/search/physics?searchtype=author&query=Br%C3%BCdern%2C+M">Maximillian Br眉dern</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2005.03486v1-abstract-short" style="display: inline;"> We address the effect of particle scattering on the energy spectra of solar energetic electron events using i) an observational and ii) a modeling approach. i) We statistically study observations of the STEREO spacecraft making use of directional electron measurements made with the SEPT instrument in the range of 45 -- 425 keV. We compare the energy spectra of the anti-sunward propagating beam wit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.03486v1-abstract-full').style.display = 'inline'; document.getElementById('2005.03486v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.03486v1-abstract-full" style="display: none;"> We address the effect of particle scattering on the energy spectra of solar energetic electron events using i) an observational and ii) a modeling approach. i) We statistically study observations of the STEREO spacecraft making use of directional electron measurements made with the SEPT instrument in the range of 45 -- 425 keV. We compare the energy spectra of the anti-sunward propagating beam with that one of the backward scattered population and find that, on average, the backward scattered population shows a harder spectrum with the effect being stronger at higher energies. ii) We use a numerical SEP transport model to simulate the effect of particle scattering (both in terms of pitch-angle and perpendicular to the mean field) on the spectrum. We find that pitch-angle scattering can lead to spectral changes at higher energies (E $>100$ keV) and further away from the Sun (r $> 1$ au) which are also often observed. At lower energies, and closer to the Sun the effect of pitch-angle scattering is much reduced so that the simulated energy spectra still resemble the injected power-law functions. When examining pitch-angle dependent spectra, we find, in agreement with the observational results, that the spectra of the backward propagating electrons are harder than that of the forward (from the Sun) propagating population. {We conclude that {\it Solar Orbiter} and {\it Parker Solar Probe} will be able to observe the unmodulated omni-directional SEP electron spectrum close to the Sun at higher energies, giving a direct indication of the accelerated spectrum. } <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.03486v1-abstract-full').style.display = 'none'; document.getElementById('2005.03486v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.02692">arXiv:2005.02692</a> <span> [<a href="https://arxiv.org/pdf/2005.02692">pdf</a>, <a href="https://arxiv.org/format/2005.02692">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-020-8329-4">10.1140/epjc/s10052-020-8329-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cryogenic characterization of a LiAlO$_{2}$ crystal and new results on spin-dependent dark matter interactions with ordinary matter </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Abdelhameed%2C+A+H">A. H. Abdelhameed</a>, <a href="/search/physics?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/physics?searchtype=author&query=Bauer%2C+P">P. Bauer</a>, <a href="/search/physics?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/physics?searchtype=author&query=Bertoldo%2C+E">E. Bertoldo</a>, <a href="/search/physics?searchtype=author&query=Breier%2C+R">R. Breier</a>, <a href="/search/physics?searchtype=author&query=Bucci%2C+C">C. Bucci</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=D%27Addabbo%2C+A">A. D'Addabbo</a>, <a href="/search/physics?searchtype=author&query=Di+Lorenzo%2C+S">S. Di Lorenzo</a>, <a href="/search/physics?searchtype=author&query=Erb%2C+A">A. Erb</a>, <a href="/search/physics?searchtype=author&query=Feilitzsch%2C+F+v">F. v. Feilitzsch</a>, <a href="/search/physics?searchtype=author&query=Iachellini%2C+N+F">N. Ferreiro Iachellini</a>, <a href="/search/physics?searchtype=author&query=Fichtinger%2C+S">S. Fichtinger</a>, <a href="/search/physics?searchtype=author&query=Fuchs%2C+D">D. Fuchs</a>, <a href="/search/physics?searchtype=author&query=Fuss%2C+A">A. Fuss</a>, <a href="/search/physics?searchtype=author&query=Ghete%2C+V+M">V. M. Ghete</a>, <a href="/search/physics?searchtype=author&query=Garai%2C+A">A. Garai</a>, <a href="/search/physics?searchtype=author&query=Gorla%2C+P">P. Gorla</a>, <a href="/search/physics?searchtype=author&query=Hauff%2C+D">D. Hauff</a>, <a href="/search/physics?searchtype=author&query=Je%C5%A1kovsk%C3%BD%2C+M">M. Je拧kovsk媒</a>, <a href="/search/physics?searchtype=author&query=Jochum%2C+J">J. Jochum</a>, <a href="/search/physics?searchtype=author&query=Kaizer%2C+J">J. Kaizer</a>, <a href="/search/physics?searchtype=author&query=Kaznacheeva%2C+M">M. Kaznacheeva</a>, <a href="/search/physics?searchtype=author&query=Kinast%2C+A">A. Kinast</a> , et al. (34 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2005.02692v3-abstract-short" style="display: inline;"> In this work, a first cryogenic characterization of a scintillating LiAlO$_{2}$ single crystal is presented. The results achieved show that this material holds great potential as a target for direct dark matter search experiments. Three different detector modules obtained from one crystal grown at the Leibniz-Institut f眉r Kristallz眉chtung (IKZ) have been tested to study different properties at cry… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.02692v3-abstract-full').style.display = 'inline'; document.getElementById('2005.02692v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.02692v3-abstract-full" style="display: none;"> In this work, a first cryogenic characterization of a scintillating LiAlO$_{2}$ single crystal is presented. The results achieved show that this material holds great potential as a target for direct dark matter search experiments. Three different detector modules obtained from one crystal grown at the Leibniz-Institut f眉r Kristallz眉chtung (IKZ) have been tested to study different properties at cryogenic temperatures. Firstly, two 2.8 g twin crystals were used to build different detector modules which were operated in an above-ground laboratory at the Max Planck Institute for Physics (MPP) in Munich, Germany. The first detector module was used to study the scintillation properties of LiAlO$_{2}$ at cryogenic temperatures. The second achieved an energy threshold of (213.02$\pm$1.48) eV which allows setting a competitive limit on the spin-dependent dark matter particle-proton scattering cross section for dark matter particle masses between 350 MeV/c$^{2}$ and 1.50 GeV/c$^{2}$. Secondly, a detector module with a 373 g LiAlO$_{2}$ crystal as the main absorber was tested in an underground facility at the Laboratori Nazionali del Gran Sasso (LNGS): from this measurement it was possible to determine the radiopurity of the crystal and study the feasibility of using this material as a neutron flux monitor for low-background experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.02692v3-abstract-full').style.display = 'none'; document.getElementById('2005.02692v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur.Phys.J. C80 (2020) no.9, 834 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1912.02476">arXiv:1912.02476</a> <span> [<a href="https://arxiv.org/pdf/1912.02476">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41550-019-0942-5">10.1038/s41550-019-0942-5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Voyager 2 enters interstellar space </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Strauss%2C+R+D+T">R. Du Toit Strauss</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1912.02476v1-abstract-short" style="display: inline;"> After 41 years of travel, the Voyager 2 spacecraft joins its twin in interstellar space. A suite of papers report Voyager 2's experience of its transition through the heliosheath and heliopause to what lies beyond. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1912.02476v1-abstract-full" style="display: none;"> After 41 years of travel, the Voyager 2 spacecraft joins its twin in interstellar space. A suite of papers report Voyager 2's experience of its transition through the heliosheath and heliopause to what lies beyond. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.02476v1-abstract-full').style.display = 'none'; document.getElementById('1912.02476v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature Astronomy volume 3, pages 963-964(2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.07450">arXiv:1910.07450</a> <span> [<a href="https://arxiv.org/pdf/1910.07450">pdf</a>, <a href="https://arxiv.org/format/1910.07450">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.5281/zenodo.3489190">10.5281/zenodo.3489190 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Proceedings of The Magnificent CE$谓$NS Workshop 2018 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Sierra%2C+D+A">D. Aristizabal Sierra</a>, <a href="/search/physics?searchtype=author&query=Balantekin%2C+A+B">A. B. Balantekin</a>, <a href="/search/physics?searchtype=author&query=Caratelli%2C+D">D. Caratelli</a>, <a href="/search/physics?searchtype=author&query=Cogswell%2C+B">B. Cogswell</a>, <a href="/search/physics?searchtype=author&query=Collar%2C+J+I">J. I. Collar</a>, <a href="/search/physics?searchtype=author&query=Dahl%2C+C+E">C. E. Dahl</a>, <a href="/search/physics?searchtype=author&query=Dent%2C+J">J. Dent</a>, <a href="/search/physics?searchtype=author&query=Dutta%2C+B">B. Dutta</a>, <a href="/search/physics?searchtype=author&query=Engel%2C+J">J. Engel</a>, <a href="/search/physics?searchtype=author&query=Estrada%2C+J">J. Estrada</a>, <a href="/search/physics?searchtype=author&query=Formaggio%2C+J">J. Formaggio</a>, <a href="/search/physics?searchtype=author&query=Gariazzo%2C+S">S. Gariazzo</a>, <a href="/search/physics?searchtype=author&query=Han%2C+R">R. Han</a>, <a href="/search/physics?searchtype=author&query=Hedges%2C+S">S. Hedges</a>, <a href="/search/physics?searchtype=author&query=Huber%2C+P">P. Huber</a>, <a href="/search/physics?searchtype=author&query=Konovalov%2C+A">A. Konovalov</a>, <a href="/search/physics?searchtype=author&query=Lang%2C+R+F">R. F. Lang</a>, <a href="/search/physics?searchtype=author&query=Liao%2C+S">S. Liao</a>, <a href="/search/physics?searchtype=author&query=Lindner%2C+M">M. Lindner</a>, <a href="/search/physics?searchtype=author&query=Machado%2C+P">P. Machado</a>, <a href="/search/physics?searchtype=author&query=Mahapatra%2C+R">R. Mahapatra</a>, <a href="/search/physics?searchtype=author&query=Marfatia%2C+D">D. Marfatia</a>, <a href="/search/physics?searchtype=author&query=Martinez-Soler%2C+I">I. Martinez-Soler</a>, <a href="/search/physics?searchtype=author&query=Miranda%2C+O">O. Miranda</a>, <a href="/search/physics?searchtype=author&query=Misiak%2C+D">D. Misiak</a> , et al. (20 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1910.07450v1-abstract-short" style="display: inline;"> The Magnificent CE$谓$NS Workshop (2018) was held November 2 & 3 of 2018 on the University of Chicago campus and brought together theorists, phenomenologists, and experimentalists working in numerous areas but sharing a common interest in the process of coherent elastic neutrino-nucleus scattering (CE$谓$NS). This is a collection of abstract-like summaries of the talks given at the meeting, includin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.07450v1-abstract-full').style.display = 'inline'; document.getElementById('1910.07450v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.07450v1-abstract-full" style="display: none;"> The Magnificent CE$谓$NS Workshop (2018) was held November 2 & 3 of 2018 on the University of Chicago campus and brought together theorists, phenomenologists, and experimentalists working in numerous areas but sharing a common interest in the process of coherent elastic neutrino-nucleus scattering (CE$谓$NS). This is a collection of abstract-like summaries of the talks given at the meeting, including links to the slides presented. This document and the slides from the meeting provide an overview of the field and a snapshot of the robust CE$谓$NS-related efforts both planned and underway. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.07450v1-abstract-full').style.display = 'none'; document.getElementById('1910.07450v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">The Magnificent CEvNS Workshop (2018), Nov 2-3, 2018; Chicago, IL, USA; 44 contributions</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1905.10258">arXiv:1905.10258</a> <span> [<a href="https://arxiv.org/pdf/1905.10258">pdf</a>, <a href="https://arxiv.org/format/1905.10258">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-019-7454-4">10.1140/epjc/s10052-019-7454-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exploring CEvNS with NUCLEUS at the Chooz Nuclear Power Plant </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/physics?searchtype=author&query=Ardellier-Desages%2C+F">F. Ardellier-Desages</a>, <a href="/search/physics?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=Erhart%2C+A">A. Erhart</a>, <a href="/search/physics?searchtype=author&query=Ferreiro%2C+N">N. Ferreiro</a>, <a href="/search/physics?searchtype=author&query=Friedl%2C+M">M. Friedl</a>, <a href="/search/physics?searchtype=author&query=Ghete%2C+V+M">V. M. Ghete</a>, <a href="/search/physics?searchtype=author&query=Hauff%2C+D">D. Hauff</a>, <a href="/search/physics?searchtype=author&query=Kluck%2C+H">H. Kluck</a>, <a href="/search/physics?searchtype=author&query=Langenk%C3%A4mper%2C+A">A. Langenk盲mper</a>, <a href="/search/physics?searchtype=author&query=Lasserre%2C+T">T. Lasserre</a>, <a href="/search/physics?searchtype=author&query=Lhuillier%2C+D">D. Lhuillier</a>, <a href="/search/physics?searchtype=author&query=Kinast%2C+A">A. Kinast</a>, <a href="/search/physics?searchtype=author&query=Mancuso%2C+M">M. Mancuso</a>, <a href="/search/physics?searchtype=author&query=Rubiales%2C+J+M">J. Molina Rubiales</a>, <a href="/search/physics?searchtype=author&query=Mondragon%2C+E">E. Mondragon</a>, <a href="/search/physics?searchtype=author&query=Munch%2C+G">G. Munch</a>, <a href="/search/physics?searchtype=author&query=Nones%2C+C">C. Nones</a>, <a href="/search/physics?searchtype=author&query=Oberauer%2C+L">L. Oberauer</a>, <a href="/search/physics?searchtype=author&query=Onillon%2C+A">A. Onillon</a>, <a href="/search/physics?searchtype=author&query=Ortmann%2C+T">T. Ortmann</a>, <a href="/search/physics?searchtype=author&query=Pattavina%2C+L">L. Pattavina</a>, <a href="/search/physics?searchtype=author&query=Petricca%2C+F">F. Petricca</a>, <a href="/search/physics?searchtype=author&query=Potzel%2C+W">W. Potzel</a> , et al. (12 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1905.10258v1-abstract-short" style="display: inline;"> Coherent elastic neutrino-nucleus scattering (CE$谓$NS) offers a unique way to study neutrino properties and to search for new physics beyond the Standard Model. Nuclear reactors are promising sources to explore this process at low energies since they deliver large fluxes of (anti-)neutrinos with typical energies of a few MeV. In this paper, a new-generation experiment to study CE$谓$NS is described… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.10258v1-abstract-full').style.display = 'inline'; document.getElementById('1905.10258v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.10258v1-abstract-full" style="display: none;"> Coherent elastic neutrino-nucleus scattering (CE$谓$NS) offers a unique way to study neutrino properties and to search for new physics beyond the Standard Model. Nuclear reactors are promising sources to explore this process at low energies since they deliver large fluxes of (anti-)neutrinos with typical energies of a few MeV. In this paper, a new-generation experiment to study CE$谓$NS is described. The NUCLEUS experiment will use cryogenic detectors which feature an unprecedentedly low energy threshold and a time response fast enough to be operated in above-ground conditions. Both sensitivity to low-energy nuclear recoils and a high event rate tolerance are stringent requirements to measure CE$谓$NS of reactor antineutrinos. A new experimental site, denoted the Very-Near-Site (VNS) at the Chooz nuclear power plant in France is described. The VNS is located between the two 4.25 GW$_{\mathrm{th}}$ reactor cores and matches the requirements of NUCLEUS. First results of on-site measurements of neutron and muon backgrounds, the expected dominant background contributions, are given. In this paper a preliminary experimental setup with dedicated active and passive background reduction techniques is presented. Furthermore, the feasibility to operate the NUCLEUS detectors in coincidence with an active muon-veto at shallow overburden is studied. The paper concludes with a sensitivity study pointing out the promising physics potential of NUCLEUS at the Chooz nuclear power plant. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.10258v1-abstract-full').style.display = 'none'; document.getElementById('1905.10258v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1905.08458">arXiv:1905.08458</a> <span> [<a href="https://arxiv.org/pdf/1905.08458">pdf</a>, <a href="https://arxiv.org/format/1905.08458">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab211b">10.3847/1538-4357/ab211b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Acceleration of solar wind particles by traveling interplanetary shocks </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Prinsloo%2C+P+L">P. L. Prinsloo</a>, <a href="/search/physics?searchtype=author&query=Strauss%2C+R+D">R. D. Strauss</a>, <a href="/search/physics?searchtype=author&query=Roux%2C+J+A+l">J. A. le Roux</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1905.08458v1-abstract-short" style="display: inline;"> The acceleration of thermal solar wind protons at spherical interplanetary shocks driven by coronal mass ejections is investigated. The solar wind velocity distribution is represented using $魏$-functions, which are transformed in response to simulated shock transitions in the fixed-frame flow speed, plasma number density, and temperature. These heated solar wind distributions are specified as sour… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.08458v1-abstract-full').style.display = 'inline'; document.getElementById('1905.08458v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.08458v1-abstract-full" style="display: none;"> The acceleration of thermal solar wind protons at spherical interplanetary shocks driven by coronal mass ejections is investigated. The solar wind velocity distribution is represented using $魏$-functions, which are transformed in response to simulated shock transitions in the fixed-frame flow speed, plasma number density, and temperature. These heated solar wind distributions are specified as source spectra at the shock from which particles with sufficient energy can be injected into the diffusive shock acceleration process. It is shown that for shock-accelerated spectra to display the classically expected power-law indices associated with the compression ratio, diffusion length scales must exceed the width of the compression region. The maximum attainable energies of shock-accelerated spectra are found to be limited by the transit times of interplanetary shocks, while spectra may be accelerated to higher energies in the presence of higher levels of magnetic turbulence or at faster-moving shocks. Indeed, simulations suggest fast-moving shocks are more likely to produce very high-energy particles, while strong shocks, associated with harder shock-accelerated spectra, are linked to higher intensities of energetic particles. The prior heating of the solar wind distribution is found to complement shock acceleration in reproducing the intensities of typical energetic storm particle events, especially where injection energies are high. Moreover, simulations of $\sim$0.2 to 1 MeV proton intensities are presented that naturally reproduce the observed flat energy spectra prior to shock passages. Energetic particles accelerated from the solar wind, aided by its prior heating, are shown to contribute substantially to intensities during energetic storm particle events. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.08458v1-abstract-full').style.display = 'none'; document.getElementById('1905.08458v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 21 figures, 5 tables. Accepted for publication in the Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1902.07587">arXiv:1902.07587</a> <span> [<a href="https://arxiv.org/pdf/1902.07587">pdf</a>, <a href="https://arxiv.org/format/1902.07587">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-019-7126-4">10.1140/epjc/s10052-019-7126-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First results on sub-GeV spin-dependent dark matter interactions with $^{7}$Li </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Abdelhameed%2C+A+H">A. H. Abdelhameed</a>, <a href="/search/physics?searchtype=author&query=Angloher%2C+G">G. Angloher</a>, <a href="/search/physics?searchtype=author&query=Bauer%2C+P">P. Bauer</a>, <a href="/search/physics?searchtype=author&query=Bento%2C+A">A. Bento</a>, <a href="/search/physics?searchtype=author&query=Bertoldo%2C+E">E. Bertoldo</a>, <a href="/search/physics?searchtype=author&query=Bucci%2C+C">C. Bucci</a>, <a href="/search/physics?searchtype=author&query=Canonica%2C+L">L. Canonica</a>, <a href="/search/physics?searchtype=author&query=D%27Addabbo%2C+A">A. D'Addabbo</a>, <a href="/search/physics?searchtype=author&query=Defay%2C+X">X. Defay</a>, <a href="/search/physics?searchtype=author&query=Di+Lorenzo%2C+S">S. Di Lorenzo</a>, <a href="/search/physics?searchtype=author&query=Erb%2C+A">A. Erb</a>, <a href="/search/physics?searchtype=author&query=Feilitzsch%2C+F+v">F. v. Feilitzsch</a>, <a href="/search/physics?searchtype=author&query=Iachellini%2C+N+F">N. Ferreiro Iachellini</a>, <a href="/search/physics?searchtype=author&query=Fichtinger%2C+S">S. Fichtinger</a>, <a href="/search/physics?searchtype=author&query=Fuss%2C+A">A. Fuss</a>, <a href="/search/physics?searchtype=author&query=Gorla%2C+P">P. Gorla</a>, <a href="/search/physics?searchtype=author&query=Hauff%2C+D">D. Hauff</a>, <a href="/search/physics?searchtype=author&query=Jochum%2C+J">J. Jochum</a>, <a href="/search/physics?searchtype=author&query=Kinast%2C+A">A. Kinast</a>, <a href="/search/physics?searchtype=author&query=Kluck%2C+H">H. Kluck</a>, <a href="/search/physics?searchtype=author&query=Kraus%2C+H">H. Kraus</a>, <a href="/search/physics?searchtype=author&query=Langenk%C3%A4mper%2C+A">A. Langenk盲mper</a>, <a href="/search/physics?searchtype=author&query=Mancuso%2C+M">M. Mancuso</a>, <a href="/search/physics?searchtype=author&query=Mokina%2C+V">V. Mokina</a>, <a href="/search/physics?searchtype=author&query=Mondragon%2C+E">E. Mondragon</a> , et al. (31 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1902.07587v3-abstract-short" style="display: inline;"> In this work, we want to highlight the potential of lithium as a target for spin-dependent dark matter search in cryogenic experiments, with a special focus on the low-mass region of the parameter space. We operated a prototype detector module based on a Li$_2$MoO$_4$ target crystal in an above-ground laboratory. Despite the high background environment, the detector sets competitive limits on spin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.07587v3-abstract-full').style.display = 'inline'; document.getElementById('1902.07587v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1902.07587v3-abstract-full" style="display: none;"> In this work, we want to highlight the potential of lithium as a target for spin-dependent dark matter search in cryogenic experiments, with a special focus on the low-mass region of the parameter space. We operated a prototype detector module based on a Li$_2$MoO$_4$ target crystal in an above-ground laboratory. Despite the high background environment, the detector sets competitive limits on spin-dependent interactions of dark matter particles with protons and neutrons for masses between 0.8 GeV/c$^2$ and 1.5 GeV/c$^2$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.07587v3-abstract-full').style.display = 'none'; document.getElementById('1902.07587v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C, 79 7 (2019) 630 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1902.02038">arXiv:1902.02038</a> <span> [<a href="https://arxiv.org/pdf/1902.02038">pdf</a>, <a href="https://arxiv.org/format/1902.02038">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aafe02">10.3847/1538-4357/aafe02 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Solar energetic particle propagation in wave turbulence and the possibility of wave generation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Strauss%2C+R+D">R. D. Strauss</a>, <a href="/search/physics?searchtype=author&query=Roux%2C+J+A+l">J. A. le Roux</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1902.02038v1-abstract-short" style="display: inline;"> A complete theory for the complex interaction between solar energetic particles and the turbulent interplanetary magnetic field remains elusive. In this work we aim to contribute towards such a theory by modelling the propagation of solar energetic particle electrons in plasma wave turbulence. We specify a background turbulence spectrum, as constrained through observations, calculate the transport… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.02038v1-abstract-full').style.display = 'inline'; document.getElementById('1902.02038v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1902.02038v1-abstract-full" style="display: none;"> A complete theory for the complex interaction between solar energetic particles and the turbulent interplanetary magnetic field remains elusive. In this work we aim to contribute towards such a theory by modelling the propagation of solar energetic particle electrons in plasma wave turbulence. We specify a background turbulence spectrum, as constrained through observations, calculate the transport coefficients from first principles, and simulate the propagation of these electrons in the inner heliosphere. We have also, for the first time, included dynamical effects into the perpendicular diffusion coefficient. We show that such a "physics-first" approach can lead to reasonable results, when compared qualitatively to observations. In addition, we include the effect of wave growth/damping due to streaming electrons and show that these particles can significantly alter the turbulence levels close to the Sun for the largest events. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.02038v1-abstract-full').style.display = 'none'; document.getElementById('1902.02038v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to ApJ</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous 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