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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <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/2412.13124">arXiv:2412.13124</a> <span> [<a href="https://arxiv.org/pdf/2412.13124">pdf</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="Applied Physics">physics.app-ph</span> </div> </div> <p class="title is-5 mathjax"> Proton irradiation on Hydrogenated Amorphous Silicon flexible devices </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Menichelli%2C+M">M. Menichelli</a>, <a href="/search/physics?searchtype=author&query=Aziz%2C+S">S. Aziz</a>, <a href="/search/physics?searchtype=author&query=Bashiri%2C+A">A. Bashiri</a>, <a href="/search/physics?searchtype=author&query=Bizzarri%2C+M">M. Bizzarri</a>, <a href="/search/physics?searchtype=author&query=Buti%2C+C">C. Buti</a>, <a href="/search/physics?searchtype=author&query=Calcagnile%2C+L">L. Calcagnile</a>, <a href="/search/physics?searchtype=author&query=Calvo%2C+D">D. Calvo</a>, <a href="/search/physics?searchtype=author&query=Caprai%2C+M">M. Caprai</a>, <a href="/search/physics?searchtype=author&query=Caputo%2C+D">D. Caputo</a>, <a href="/search/physics?searchtype=author&query=Caricato%2C+A+P">A. P. Caricato</a>, <a href="/search/physics?searchtype=author&query=Catalano%2C+R">R. Catalano</a>, <a href="/search/physics?searchtype=author&query=Cazzanelli%2C+M">M. Cazzanelli</a>, <a href="/search/physics?searchtype=author&query=Cirio%2C+R">R. Cirio</a>, <a href="/search/physics?searchtype=author&query=Cirrone%2C+G+A+P">G. A. P. Cirrone</a>, <a href="/search/physics?searchtype=author&query=Cittadini%2C+F">F. Cittadini</a>, <a href="/search/physics?searchtype=author&query=Croci%2C+T">T. Croci</a>, <a href="/search/physics?searchtype=author&query=Cuttone%2C+G">G. Cuttone</a>, <a href="/search/physics?searchtype=author&query=de+Cesare%2C+G">G. de Cesare</a>, <a href="/search/physics?searchtype=author&query=De+Remigis%2C+P">P. De Remigis</a>, <a href="/search/physics?searchtype=author&query=Dunand%2C+S">S. Dunand</a>, <a href="/search/physics?searchtype=author&query=Fabi%2C+M">M. Fabi</a>, <a href="/search/physics?searchtype=author&query=Frontini%2C+L">L. Frontini</a>, <a href="/search/physics?searchtype=author&query=Grimani%2C+C">C. Grimani</a>, <a href="/search/physics?searchtype=author&query=Guarrera%2C+M">M. Guarrera</a>, <a href="/search/physics?searchtype=author&query=Hasnaoui%2C+H">H. Hasnaoui</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="2412.13124v1-abstract-short" style="display: inline;"> Radiation damage tests in hydrogenated amorphous silicon (a-Si:H) flexible flux and dose-measuring devices have been performed with a 3 MeV proton beam, to evaluate combined displacement and total ionizing dose damage. The tested devices had two different configurations and thicknesses. The first device was a 2 um thick n-i-p diode having a 5 mm x 5 mm area. The second device was a 5 um thick char… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.13124v1-abstract-full').style.display = 'inline'; document.getElementById('2412.13124v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.13124v1-abstract-full" style="display: none;"> Radiation damage tests in hydrogenated amorphous silicon (a-Si:H) flexible flux and dose-measuring devices have been performed with a 3 MeV proton beam, to evaluate combined displacement and total ionizing dose damage. The tested devices had two different configurations and thicknesses. The first device was a 2 um thick n-i-p diode having a 5 mm x 5 mm area. The second device was a 5 um thick charge selective contact detector having the same area. Both the devices were deposited on a flexible polyimide substrate and were irradiated up to the fluence of 1016 neq/cm2. The response to different proton fluxes has been measured before irradiation and after irradiation at 1016 neq/cm2 for charge-selective contacts and n-i-p devices. The effect of annealing for partial performance recovery at 100掳C for 12 hours was also studied and a final characterization on annealed devices was performed. This test is the first combined displacement and total ionizing dose test on flexible a-Si:H devices. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.13124v1-abstract-full').style.display = 'none'; document.getElementById('2412.13124v1-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">This paper was presented at the IEEE-RTSD2024 in Tampa (USA) with presentation number: R08-04</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.00495">arXiv:2310.00495</a> <span> [<a href="https://arxiv.org/pdf/2310.00495">pdf</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="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Characterization of hydrogenated amorphous silicon sensors on polyimide flexible substrate </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Menichelli%2C+M">M. Menichelli</a>, <a href="/search/physics?searchtype=author&query=Antognini%2C+L">L. Antognini</a>, <a href="/search/physics?searchtype=author&query=Aziz%2C+S">S. Aziz</a>, <a href="/search/physics?searchtype=author&query=Bashiri%2C+A">A. Bashiri</a>, <a href="/search/physics?searchtype=author&query=Bizzarri%2C+M">M. Bizzarri</a>, <a href="/search/physics?searchtype=author&query=Calcagnile%2C+L">L. Calcagnile</a>, <a href="/search/physics?searchtype=author&query=Caprai%2C+M">M. Caprai</a>, <a href="/search/physics?searchtype=author&query=Caputo%2C+D">D. Caputo</a>, <a href="/search/physics?searchtype=author&query=Caricato%2C+A+P">A. P. Caricato</a>, <a href="/search/physics?searchtype=author&query=Catalano%2C+R">R. Catalano</a>, <a href="/search/physics?searchtype=author&query=Chil%C3%A0%2C+D">D. Chil脿</a>, <a href="/search/physics?searchtype=author&query=Cirrone%2C+G+A+P">G. A. P. Cirrone</a>, <a href="/search/physics?searchtype=author&query=Croci%2C+T">T. Croci</a>, <a href="/search/physics?searchtype=author&query=Cuttone%2C+G">G. Cuttone</a>, <a href="/search/physics?searchtype=author&query=De+Cesare%2C+G">G. De Cesare</a>, <a href="/search/physics?searchtype=author&query=Dunand%2C+S">S. Dunand</a>, <a href="/search/physics?searchtype=author&query=Fabi%2C+M">M. Fabi</a>, <a href="/search/physics?searchtype=author&query=Frontini%2C+L">L. Frontini</a>, <a href="/search/physics?searchtype=author&query=Grimani%2C+C">C. Grimani</a>, <a href="/search/physics?searchtype=author&query=Ionica%2C+M">M. Ionica</a>, <a href="/search/physics?searchtype=author&query=Kanxheri%2C+K">K. Kanxheri</a>, <a href="/search/physics?searchtype=author&query=Large%2C+M">M. Large</a>, <a href="/search/physics?searchtype=author&query=Liberali%2C+V">V. Liberali</a>, <a href="/search/physics?searchtype=author&query=Lovecchio%2C+N">N. Lovecchio</a>, <a href="/search/physics?searchtype=author&query=Martino%2C+M">M. Martino</a> , et al. (28 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="2310.00495v1-abstract-short" style="display: inline;"> Hydrogenated amorphous silicon (a-Si:H) is a material having an intrinsically high radiation hardness that can be deposited on flexible substrates like Polyimide. For these properties a-Si:H can be used for the production of flexible sensors. a-Si:H sensors can be successfully utilized in dosimetry, beam monitoring for particle physics (x-ray, electron, gamma-ray and proton detection) and radiothe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.00495v1-abstract-full').style.display = 'inline'; document.getElementById('2310.00495v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.00495v1-abstract-full" style="display: none;"> Hydrogenated amorphous silicon (a-Si:H) is a material having an intrinsically high radiation hardness that can be deposited on flexible substrates like Polyimide. For these properties a-Si:H can be used for the production of flexible sensors. a-Si:H sensors can be successfully utilized in dosimetry, beam monitoring for particle physics (x-ray, electron, gamma-ray and proton detection) and radiotherapy, radiation flux measurement for space applications (study of solar energetic particles and stellar events) and neutron flux measurements. In this paper we have studied the dosimetric x-ray response of n-i-p diodes deposited on Polyimide. We measured the linearity of the photocurrent response to x-rays versus dose-rate from which we have extracted the dosimetric x-ray sensitivity at various bias voltages. In particular low bias voltage operation has been studied to assess the high energy efficiency of these kind of sensor. A measurement of stability of x-ray response versus time has been shown. The effect of detectors annealing has been studied. Operation under bending at various bending radii is also shown. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.00495v1-abstract-full').style.display = 'none'; document.getElementById('2310.00495v1-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> 30 September, 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/2307.11598">arXiv:2307.11598</a> <span> [<a href="https://arxiv.org/pdf/2307.11598">pdf</a>, <a href="https://arxiv.org/format/2307.11598">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="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> <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/10.1051/0004-6361/202346679">10.1051/0004-6361/202346679 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Particle monitoring capability of the Solar Orbiter Metis coronagraph through the increasing phase of solar cycle 25 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Grimani%2C+C">Catia Grimani</a>, <a href="/search/physics?searchtype=author&query=Andretta%2C+V">Vincenzo Andretta</a>, <a href="/search/physics?searchtype=author&query=Antonucci%2C+E">Ester Antonucci</a>, <a href="/search/physics?searchtype=author&query=Chioetto%2C+P">Paolo Chioetto</a>, <a href="/search/physics?searchtype=author&query=Da+Deppo%2C+V">Vania Da Deppo</a>, <a href="/search/physics?searchtype=author&query=Fabi%2C+M">Michele Fabi</a>, <a href="/search/physics?searchtype=author&query=Gissot%2C+S">Samuel Gissot</a>, <a href="/search/physics?searchtype=author&query=Jerse%2C+G">Giovanna Jerse</a>, <a href="/search/physics?searchtype=author&query=Messerotti%2C+M">Mauro Messerotti</a>, <a href="/search/physics?searchtype=author&query=Naletto%2C+G">Giampiero Naletto</a>, <a href="/search/physics?searchtype=author&query=Pancrazzi%2C+M">Maurizio Pancrazzi</a>, <a href="/search/physics?searchtype=author&query=Persici%2C+A">Andrea Persici</a>, <a href="/search/physics?searchtype=author&query=Plainaki%2C+C">Christina Plainaki</a>, <a href="/search/physics?searchtype=author&query=Romoli%2C+M">Marco Romoli</a>, <a href="/search/physics?searchtype=author&query=Sabbatini%2C+F">Federico Sabbatini</a>, <a href="/search/physics?searchtype=author&query=Spadaro%2C+D">Daniele Spadaro</a>, <a href="/search/physics?searchtype=author&query=Stangalini%2C+M">Marco Stangalini</a>, <a href="/search/physics?searchtype=author&query=Telloni%2C+D">Daniele Telloni</a>, <a href="/search/physics?searchtype=author&query=Teriaca%2C+L">Luca Teriaca</a>, <a href="/search/physics?searchtype=author&query=Uslenghi%2C+M">Michela Uslenghi</a>, <a href="/search/physics?searchtype=author&query=Villani%2C+M">Mattia Villani</a>, <a href="/search/physics?searchtype=author&query=Abbo%2C+L">Lucia Abbo</a>, <a href="/search/physics?searchtype=author&query=Burtovoi%2C+A">Aleksandr Burtovoi</a>, <a href="/search/physics?searchtype=author&query=Frassati%2C+F">Federica Frassati</a>, <a href="/search/physics?searchtype=author&query=Landini%2C+F">Federico Landini</a> , et al. (4 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="2307.11598v2-abstract-short" style="display: inline;"> Context. Galactic cosmic rays (GCRs) and solar particles with energies greater than tens of MeV penetrate spacecraft and instruments hosted aboard space missions. The Solar Orbiter Metis coronagraph is aimed at observing the solar corona in both visible (VL) and ultraviolet (UV) light. Particle tracks are observed in the Metis images of the corona. An algorithm has been implemented in the Metis pr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.11598v2-abstract-full').style.display = 'inline'; document.getElementById('2307.11598v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.11598v2-abstract-full" style="display: none;"> Context. Galactic cosmic rays (GCRs) and solar particles with energies greater than tens of MeV penetrate spacecraft and instruments hosted aboard space missions. The Solar Orbiter Metis coronagraph is aimed at observing the solar corona in both visible (VL) and ultraviolet (UV) light. Particle tracks are observed in the Metis images of the corona. An algorithm has been implemented in the Metis processing electronics to detect the VL image pixels crossed by cosmic rays. This algorithm was initially enabled for the VL instrument only, since the process of separating the particle tracks in the UV images has proven to be very challenging. Aims. We study the impact of the overall bulk of particles of galactic and solar origin on the Metis coronagraph images. We discuss the effects of the increasing solar activity after the Solar Orbiter mission launch on the secondary particle production in the spacecraft. Methods. We compared Monte Carlo simulations of GCRs crossing or interacting in the Metis VL CMOS sensor to observations gathered in 2020 and 2022. We also evaluated the impact of solar energetic particle events of different intensities on the Metis images. Results. The study of the role of abundant and rare cosmic rays in firing pixels in the Metis VL images of the corona allows us to estimate the efficiency of the algorithm applied for cosmic-ray track removal from the images and to demonstrate that the instrument performance had remained unchanged during the first two years of the Solar Orbiter operations. The outcome of this work can be used to estimate the Solar Orbiter instrument's deep charging and the order of magnitude for energetic particles crossing the images of Metis and other instruments such as STIX and EUI. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.11598v2-abstract-full').style.display = 'none'; document.getElementById('2307.11598v2-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 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">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> A&A 677, A45 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.10819">arXiv:2306.10819</a> <span> [<a href="https://arxiv.org/pdf/2306.10819">pdf</a>, <a href="https://arxiv.org/format/2306.10819">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> <p class="title is-5 mathjax"> Coronal Heating Rate in the Slow Solar Wind </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Telloni%2C+D">Daniele Telloni</a>, <a href="/search/physics?searchtype=author&query=Romoli%2C+M">Marco Romoli</a>, <a href="/search/physics?searchtype=author&query=Velli%2C+M">Marco Velli</a>, <a href="/search/physics?searchtype=author&query=Zank%2C+G+P">Gary P. Zank</a>, <a href="/search/physics?searchtype=author&query=Adhikari%2C+L">Laxman Adhikari</a>, <a href="/search/physics?searchtype=author&query=Downs%2C+C">Cooper Downs</a>, <a href="/search/physics?searchtype=author&query=Burtovoi%2C+A">Aleksandr Burtovoi</a>, <a href="/search/physics?searchtype=author&query=Susino%2C+R">Roberto Susino</a>, <a href="/search/physics?searchtype=author&query=Spadaro%2C+D">Daniele Spadaro</a>, <a href="/search/physics?searchtype=author&query=Zhao%2C+L">Lingling Zhao</a>, <a href="/search/physics?searchtype=author&query=Liberatore%2C+A">Alessandro Liberatore</a>, <a href="/search/physics?searchtype=author&query=Shi%2C+C">Chen Shi</a>, <a href="/search/physics?searchtype=author&query=De+Leo%2C+Y">Yara De Leo</a>, <a href="/search/physics?searchtype=author&query=Abbo%2C+L">Lucia Abbo</a>, <a href="/search/physics?searchtype=author&query=Frassati%2C+F">Federica Frassati</a>, <a href="/search/physics?searchtype=author&query=Jerse%2C+G">Giovanna Jerse</a>, <a href="/search/physics?searchtype=author&query=Landini%2C+F">Federico Landini</a>, <a href="/search/physics?searchtype=author&query=Nicolini%2C+G">Gianalfredo Nicolini</a>, <a href="/search/physics?searchtype=author&query=Pancrazzi%2C+M">Maurizio Pancrazzi</a>, <a href="/search/physics?searchtype=author&query=Russano%2C+G">Giuliana Russano</a>, <a href="/search/physics?searchtype=author&query=Sasso%2C+C">Clementina Sasso</a>, <a href="/search/physics?searchtype=author&query=Andretta%2C+V">Vincenzo Andretta</a>, <a href="/search/physics?searchtype=author&query=Da+Deppo%2C+V">Vania Da Deppo</a>, <a href="/search/physics?searchtype=author&query=Fineschi%2C+S">Silvano Fineschi</a>, <a href="/search/physics?searchtype=author&query=Grimani%2C+C">Catia Grimani</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="2306.10819v1-abstract-short" style="display: inline;"> This Letter reports the first observational estimate of the heating rate in the slowly expanding solar corona. The analysis exploits the simultaneous remote and local observations of the same coronal plasma volume with the Solar Orbiter/Metis and the Parker Solar Probe instruments, respectively, and relies on the basic solar wind magnetohydrodynamic equations. As expected, energy losses are a mino… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.10819v1-abstract-full').style.display = 'inline'; document.getElementById('2306.10819v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.10819v1-abstract-full" style="display: none;"> This Letter reports the first observational estimate of the heating rate in the slowly expanding solar corona. The analysis exploits the simultaneous remote and local observations of the same coronal plasma volume with the Solar Orbiter/Metis and the Parker Solar Probe instruments, respectively, and relies on the basic solar wind magnetohydrodynamic equations. As expected, energy losses are a minor fraction of the solar wind energy flux, since most of the energy dissipation that feeds the heating and acceleration of the coronal flow occurs much closer to the Sun than the heights probed in the present study, which range from 6.3 to 13.3 solar radii. The energy deposited to the supersonic wind is then used to explain the observed slight residual wind acceleration and to maintain the plasma in a non-adiabatic state. As derived in the Wentzel-Kramers-Brillouin limit, the present energy transfer rate estimates provide a lower limit, which can be very useful in refining the turbulence-based modeling of coronal heating and subsequent solar wind acceleration. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.10819v1-abstract-full').style.display = 'none'; document.getElementById('2306.10819v1-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> 19 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.06740">arXiv:2302.06740</a> <span> [<a href="https://arxiv.org/pdf/2302.06740">pdf</a>, <a href="https://arxiv.org/format/2302.06740">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 Astrophysical Phenomena">astro-ph.HE</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="Machine Learning">cs.LG</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"> Solar Wind Speed Estimate with Machine Learning Ensemble Models for LISA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Sabbatini%2C+F">Federico Sabbatini</a>, <a href="/search/physics?searchtype=author&query=Grimani%2C+C">Catia Grimani</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="2302.06740v1-abstract-short" style="display: inline;"> In this work we study the potentialities of machine learning models in reconstructing the solar wind speed observations gathered in the first Lagrangian point by the ACE satellite in 2016--2017 using as input data galactic cosmic-ray flux variations measured with particle detectors hosted onboard the LISA Pathfinder mission also orbiting around L1 during the same years. We show that ensemble model… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.06740v1-abstract-full').style.display = 'inline'; document.getElementById('2302.06740v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.06740v1-abstract-full" style="display: none;"> In this work we study the potentialities of machine learning models in reconstructing the solar wind speed observations gathered in the first Lagrangian point by the ACE satellite in 2016--2017 using as input data galactic cosmic-ray flux variations measured with particle detectors hosted onboard the LISA Pathfinder mission also orbiting around L1 during the same years. We show that ensemble models composed of heterogeneous weak regressors are able to outperform weak regressors in terms of predictive accuracy. Machine learning and other powerful predictive algorithms open a window on the possibility of substituting dedicated instrumentation with software models acting as surrogates for diagnostics of space missions such as LISA and space weather science. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.06740v1-abstract-full').style.display = 'none'; document.getElementById('2302.06740v1-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 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">Submitted to Environmental Modelling & Software</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.00339">arXiv:2302.00339</a> <span> [<a href="https://arxiv.org/pdf/2302.00339">pdf</a>, <a href="https://arxiv.org/format/2302.00339">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="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> <p class="title is-5 mathjax"> A Hydrogenated amorphous silicon detector for Space Weather Applications </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Grimani%2C+C">Catia Grimani</a>, <a href="/search/physics?searchtype=author&query=Fabi%2C+M">Michele Fabi</a>, <a href="/search/physics?searchtype=author&query=Sabbatini%2C+F">Federico Sabbatini</a>, <a href="/search/physics?searchtype=author&query=Villani%2C+M">Mattia Villani</a>, <a href="/search/physics?searchtype=author&query=Calcagnile%2C+L">Lucio Calcagnile</a>, <a href="/search/physics?searchtype=author&query=Caricato%2C+A+P">Anna Paola Caricato</a>, <a href="/search/physics?searchtype=author&query=Catalano%2C+R">Roberto Catalano</a>, <a href="/search/physics?searchtype=author&query=Cirrone%2C+G+A+P">Giuseppe Antonio Pablo Cirrone</a>, <a href="/search/physics?searchtype=author&query=Croci%2C+T">Tommaso Croci</a>, <a href="/search/physics?searchtype=author&query=Cuttone%2C+G">Giacomo Cuttone</a>, <a href="/search/physics?searchtype=author&query=Dunand%2C+S">Sylvain Dunand</a>, <a href="/search/physics?searchtype=author&query=Frontini%2C+L">Luca Frontini</a>, <a href="/search/physics?searchtype=author&query=Ionica%2C+M">Maria Ionica</a>, <a href="/search/physics?searchtype=author&query=Kanxheri%2C+K">Keida Kanxheri</a>, <a href="/search/physics?searchtype=author&query=Large%2C+M">Matthew Large</a>, <a href="/search/physics?searchtype=author&query=Liberali%2C+V">Valentino Liberali</a>, <a href="/search/physics?searchtype=author&query=Martino%2C+M">Maurizio Martino</a>, <a href="/search/physics?searchtype=author&query=Maruccio%2C+G">Giuseppe Maruccio</a>, <a href="/search/physics?searchtype=author&query=Mazza%2C+G">Giovanni Mazza</a>, <a href="/search/physics?searchtype=author&query=Menichelli%2C+M">Mauro Menichelli</a>, <a href="/search/physics?searchtype=author&query=Monteduro%2C+A+G">Anna Grazia Monteduro</a>, <a href="/search/physics?searchtype=author&query=Morozzi%2C+A">Arianna Morozzi</a>, <a href="/search/physics?searchtype=author&query=Moscatelli%2C+F">Francesco Moscatelli</a>, <a href="/search/physics?searchtype=author&query=Pallotta%2C+S">Stefania Pallotta</a>, <a href="/search/physics?searchtype=author&query=Passeri%2C+D">Daniele Passeri</a> , et al. (13 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="2302.00339v2-abstract-short" style="display: inline;"> The characteristics of a hydrogenated amorphous silicon (a-Si:H) detector are presented here for monitoring in space solar flares and the evolution of large energetic proton events up to hundreds of MeV. The a-Si:H presents an excellent radiation hardness and finds application in harsh radiation environments for medical purposes, for particle beam characterization and in space weather science and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.00339v2-abstract-full').style.display = 'inline'; document.getElementById('2302.00339v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.00339v2-abstract-full" style="display: none;"> The characteristics of a hydrogenated amorphous silicon (a-Si:H) detector are presented here for monitoring in space solar flares and the evolution of large energetic proton events up to hundreds of MeV. The a-Si:H presents an excellent radiation hardness and finds application in harsh radiation environments for medical purposes, for particle beam characterization and in space weather science and applications. The critical flux detection threshold for solar X rays, soft gamma rays, electrons and protons is discussed in detail. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.00339v2-abstract-full').style.display = 'none'; document.getElementById('2302.00339v2-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> 1 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 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">32 pages, 13 figures, submitted to Experimental Astronomy</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.17114">arXiv:2211.17114</a> <span> [<a href="https://arxiv.org/pdf/2211.17114">pdf</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="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Development of thin hydrogenated amorphous silicon detectors on a flexible substrate </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Menichelli%2C+M">M. Menichelli</a>, <a href="/search/physics?searchtype=author&query=Bizzarri%2C+M">M. Bizzarri</a>, <a href="/search/physics?searchtype=author&query=Calcagnile%2C+L">L. Calcagnile</a>, <a href="/search/physics?searchtype=author&query=Caprai%2C+M">M. Caprai</a>, <a href="/search/physics?searchtype=author&query=Caricato%2C+A+P">A. P. Caricato</a>, <a href="/search/physics?searchtype=author&query=Catalano%2C+R">R. Catalano</a>, <a href="/search/physics?searchtype=author&query=Cirrone%2C+G+A+P">G. A. P. Cirrone</a>, <a href="/search/physics?searchtype=author&query=Croci%2C+T">T. Croci</a>, <a href="/search/physics?searchtype=author&query=Cuttone%2C+G">G. Cuttone</a>, <a href="/search/physics?searchtype=author&query=Dunand%2C+S">S. Dunand</a>, <a href="/search/physics?searchtype=author&query=Fabi%2C+M">M. Fabi</a>, <a href="/search/physics?searchtype=author&query=Frontini%2C+L">L. Frontini</a>, <a href="/search/physics?searchtype=author&query=Gianfelici%2C+B">B. Gianfelici</a>, <a href="/search/physics?searchtype=author&query=Grimani%2C+C">C. Grimani</a>, <a href="/search/physics?searchtype=author&query=Ionica%2C+M">M. Ionica</a>, <a href="/search/physics?searchtype=author&query=Kanxheri%2C+K">K. Kanxheri</a>, <a href="/search/physics?searchtype=author&query=Large%2C+M">M. Large</a>, <a href="/search/physics?searchtype=author&query=Liberali%2C+V">V. Liberali</a>, <a href="/search/physics?searchtype=author&query=Martino%2C+M">M. Martino</a>, <a href="/search/physics?searchtype=author&query=Maruccio%2C+G">G. Maruccio</a>, <a href="/search/physics?searchtype=author&query=Mazza%2C+G">G. Mazza</a>, <a href="/search/physics?searchtype=author&query=Monteduro%2C+A+G">A. G. Monteduro</a>, <a href="/search/physics?searchtype=author&query=Morozzi%2C+A">A. Morozzi</a>, <a href="/search/physics?searchtype=author&query=Moscatelli%2C+F">F. Moscatelli</a>, <a href="/search/physics?searchtype=author&query=Pallotta%2C+S">S. Pallotta</a> , et al. (18 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="2211.17114v1-abstract-short" style="display: inline;"> The HASPIDE (Hydrogenated Amorphous Silicon PIxels DEtectors) project aims at the development of thin hydrogenated amorphous silicon (a-Si:H) detectors on flexible substrates (mostly Polyimide) for beam monitoring, neutron detection and space applications. Since a-Si:H is a material with superior radiation hardness, the benefit for the above-mentioned applications can be appreciated mostly in radi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.17114v1-abstract-full').style.display = 'inline'; document.getElementById('2211.17114v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.17114v1-abstract-full" style="display: none;"> The HASPIDE (Hydrogenated Amorphous Silicon PIxels DEtectors) project aims at the development of thin hydrogenated amorphous silicon (a-Si:H) detectors on flexible substrates (mostly Polyimide) for beam monitoring, neutron detection and space applications. Since a-Si:H is a material with superior radiation hardness, the benefit for the above-mentioned applications can be appreciated mostly in radiation harsh environments. Furthermore, the possibility to deposit this material on flexible substrates like Polyimide (PI), polyethylene naphthalate (PEN) or polyethylene terephthalate (PET) facilitates the usage of these detectors in medical dosimetry, beam flux and beam profile measurements. Particularly interesting is its use when positioned directly on the flange of the vacuum-to-air separation interface in a beam line, as well as other applications where a thin self-standing radiation flux detector is envisaged. In this paper, the HASPIDE project will be described and some preliminary results on PI and glass substrates will be reported. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.17114v1-abstract-full').style.display = 'none'; document.getElementById('2211.17114v1-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> 30 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/2209.12791">arXiv:2209.12791</a> <span> [<a href="https://arxiv.org/pdf/2209.12791">pdf</a>, <a href="https://arxiv.org/format/2209.12791">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="Classical Physics">physics.class-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/10.1088/1361-6382/acbadd">10.1088/1361-6382/acbadd <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The role of low-energy electrons in the charging process of LISA test masses </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Taioli%2C+S">Simone Taioli</a>, <a href="/search/physics?searchtype=author&query=Dapor%2C+M">Maurizio Dapor</a>, <a href="/search/physics?searchtype=author&query=Dimiccoli%2C+F">Francesco Dimiccoli</a>, <a href="/search/physics?searchtype=author&query=Fabi%2C+M">Michele Fabi</a>, <a href="/search/physics?searchtype=author&query=Ferroni%2C+V">Valerio Ferroni</a>, <a href="/search/physics?searchtype=author&query=Grimani%2C+C">Catia Grimani</a>, <a href="/search/physics?searchtype=author&query=Villani%2C+M">Mattia Villani</a>, <a href="/search/physics?searchtype=author&query=Weber%2C+W+J">William Joseph Weber</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="2209.12791v2-abstract-short" style="display: inline;"> The space environment encountered by operating spacecraft is populated by a continuous flux of charged particles that penetrate into electronic devices inducing phantom commands and loss of control, eventually leading to satellite failure. Moreover, electron static discharge that results from secondary electron emission of the device materials can also be responsible for satellite malfunction. In… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.12791v2-abstract-full').style.display = 'inline'; document.getElementById('2209.12791v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.12791v2-abstract-full" style="display: none;"> The space environment encountered by operating spacecraft is populated by a continuous flux of charged particles that penetrate into electronic devices inducing phantom commands and loss of control, eventually leading to satellite failure. Moreover, electron static discharge that results from secondary electron emission of the device materials can also be responsible for satellite malfunction. In this regard, the estimate of the total electron yield is fundamental for our understanding of the test-mass charging associated with galactic cosmic rays in the LISA Pathfinder mission and in the forthcoming gravitational wave observatory LISA. To unveil the role of low energy electrons in this process owing to galactic and solar energetic particle events, in this work we study the interaction of keV and sub-keV electrons with a gold slab using a mixed Monte Carlo and ab-initio framework. We determine the energy spectrum of the electrons emerging from such a gold slab hit by a primary electron beam by considering the relevant energy loss mechanisms as well as the elastic scattering events. We also show that our results are consistent with experimental data and Monte Carlo simulations carried out with the GEANT4-DNA toolkit. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.12791v2-abstract-full').style.display = 'none'; document.getElementById('2209.12791v2-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.12329">arXiv:2209.12329</a> <span> [<a href="https://arxiv.org/pdf/2209.12329">pdf</a>, <a href="https://arxiv.org/format/2209.12329">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="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> Interplanetary medium monitoring with LISA: lessons from LISA Pathfinder </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Cesarini%2C+A">A. Cesarini</a>, <a href="/search/physics?searchtype=author&query=Grimani%2C+C">C. Grimani</a>, <a href="/search/physics?searchtype=author&query=Benella%2C+S">S. Benella</a>, <a href="/search/physics?searchtype=author&query=Fabi%2C+M">M. Fabi</a>, <a href="/search/physics?searchtype=author&query=Sabbatini%2C+F">F. Sabbatini</a>, <a href="/search/physics?searchtype=author&query=Villani%2C+M">M. Villani</a>, <a href="/search/physics?searchtype=author&query=Telloni%2C+D">D. Telloni</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="2209.12329v1-abstract-short" style="display: inline;"> The Laser Interferometer Space Antenna (LISA) of the European Space Agency (ESA) will be the first low-frequency gravitational-wave observatory orbiting the Sun at 1 AU. The LISA Pathfinder (LPF) mission, aiming at testing of the instruments to be located on board the LISA spacecraft (S/C), hosted, among the others, fluxgate magnetometers and a particle detector as parts of a diagnostics subsystem… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.12329v1-abstract-full').style.display = 'inline'; document.getElementById('2209.12329v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.12329v1-abstract-full" style="display: none;"> The Laser Interferometer Space Antenna (LISA) of the European Space Agency (ESA) will be the first low-frequency gravitational-wave observatory orbiting the Sun at 1 AU. The LISA Pathfinder (LPF) mission, aiming at testing of the instruments to be located on board the LISA spacecraft (S/C), hosted, among the others, fluxgate magnetometers and a particle detector as parts of a diagnostics subsystem. These instruments allowed us for the estimate of the magnetic and Coulomb spurious forces acting on the test masses that constitute the mirrors of the interferometer. With these instruments we also had the possibility to study the galactic cosmic-ray short term-term variations as a function of the particle energy and the associated interplanetary disturbances. Platform magnetometers and particle detectors will be also placed on board each LISA S/C. This work reports about an empirical method that allowed us to disentangle the interplanetary and onboard-generated components of the magnetic field by using the LPF magnetometer measurements. Moreover, we estimate the number and fluence of solar energetic particle events expected to be observed with the ESA Next Generation Radiation Monitor during the mission lifetime. An additional cosmic-ray detector, similar to that designed for LPF, in combination with magnetometers, would permit to observe the evolution of recurrent and non-recurrent galactic cosmic-ray variations and associated increases of the interplanetary magnetic field at the transit of high-speed solar wind streams and interplanetary counterparts of coronal mass ejections. The diagnostics subsystem of LISA makes this mission also a natural multi-point observatory for space weather science investigations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.12329v1-abstract-full').style.display = 'none'; document.getElementById('2209.12329v1-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 September, 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">Accepted for publication Journal of Space Weather and Space Climate (JSWSC)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.08849">arXiv:2208.08849</a> <span> [<a href="https://arxiv.org/pdf/2208.08849">pdf</a>, <a href="https://arxiv.org/ps/2208.08849">ps</a>, <a href="https://arxiv.org/format/2208.08849">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 Astrophysical Phenomena">astro-ph.HE</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> <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/10.1051/0004-6361/202243984">10.1051/0004-6361/202243984 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Bridging the gap between Monte Carlo simulations and measurements of the LISA Pathfinder test-mass charging for LISA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Grimani%2C+C">Catia Grimani</a>, <a href="/search/physics?searchtype=author&query=Villani%2C+M">Mattia Villani</a>, <a href="/search/physics?searchtype=author&query=Fabi%2C+M">Michele Fabi</a>, <a href="/search/physics?searchtype=author&query=Cesarini%2C+A">Andrea Cesarini</a>, <a href="/search/physics?searchtype=author&query=Sabbatini%2C+F">Federico Sabbatini</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="2208.08849v1-abstract-short" style="display: inline;"> Cubic gold-platinum free-falling test masses (TMs) constitute the mirrors of future LISA and LISA-like interferometers for low-frequency gravitational wave detection in space. High-energy particles of Galactic and solar origin charge the TMs and thus induce spurious electrostatic and magnetic forces that limit the sensitivity of these interferometers. Prelaunch Monte Carlo simulations of the TM ch… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.08849v1-abstract-full').style.display = 'inline'; document.getElementById('2208.08849v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.08849v1-abstract-full" style="display: none;"> Cubic gold-platinum free-falling test masses (TMs) constitute the mirrors of future LISA and LISA-like interferometers for low-frequency gravitational wave detection in space. High-energy particles of Galactic and solar origin charge the TMs and thus induce spurious electrostatic and magnetic forces that limit the sensitivity of these interferometers. Prelaunch Monte Carlo simulations of the TM charging were carried out for the LISA Pathfinder (LPF) mission, that was planned to test the LISA instrumentation. Measurements and simulations were compared during the mission operations. The measured net TM charging agreed with simulation estimates, while the charging noise was three to four times higher. We aim to bridge the gap between LPF TM charging noise simulations and observations. New Monte Carlo simulations of the LPF TM charging due to both Galactic and solar particles were carried out with the FLUKA/LEI toolkit. This allowed propagating low-energy electrons down to a few electronvolt. These improved FLUKA/LEI simulations agree with observations gathered during the mission operations within statistical and Monte Carlo errors. The charging noise induced by Galactic cosmic rays is about one thousand charges per second. This value increases to tens of thousands charges per second during solar energetic particle events. Similar results are expected for the LISA TM charging. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.08849v1-abstract-full').style.display = 'none'; document.getElementById('2208.08849v1-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> 18 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">11 pages, 9 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 666, A38 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.02690">arXiv:2012.02690</a> <span> [<a href="https://arxiv.org/pdf/2012.02690">pdf</a>, <a href="https://arxiv.org/format/2012.02690">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/10.1088/1361-6382/abd142">10.1088/1361-6382/abd142 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Low-energy electromagnetic processes affecting free-falling test-mass charging for LISA and future space interferometers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Grimani%2C+C">Catia Grimani</a>, <a href="/search/physics?searchtype=author&query=Cesarini%2C+A">Andrea Cesarini</a>, <a href="/search/physics?searchtype=author&query=Fabi%2C+M">Michele Fabi</a>, <a href="/search/physics?searchtype=author&query=Villani%2C+M">Mattia Villani</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="2012.02690v1-abstract-short" style="display: inline;"> Galactic cosmic rays and solar energetic particles charge gold-platinum, free-falling test masses (TMs) on board interferometers for the detection of gravitational waves in space. The charging process induces spurious forces on the test masses that affect the sensitivity of these instruments mainly below $10^{-3}$ Hz. Geant4 and FLUKA Monte Carlo simulations were carried out to study the TM chargi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02690v1-abstract-full').style.display = 'inline'; document.getElementById('2012.02690v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.02690v1-abstract-full" style="display: none;"> Galactic cosmic rays and solar energetic particles charge gold-platinum, free-falling test masses (TMs) on board interferometers for the detection of gravitational waves in space. The charging process induces spurious forces on the test masses that affect the sensitivity of these instruments mainly below $10^{-3}$ Hz. Geant4 and FLUKA Monte Carlo simulations were carried out to study the TM charging process on board the LISA Pathfinder mission that remained into orbit around the Sun-Earth Lagrange point L1 between 2016 and 2017. While a good agreement was observed between simulations and measurements of the TMs net charging, the shot noise associated with charging fluctuations of both positive and negative particles resulted 3-4 times higher that predicted. The origin of this mismatch was attributed to the propagation of electrons and photons only above 100 eV in the simulations. In this paper, low-energy electromagnetic processes to be included in the future Monte Carlo simulations for LISA and LISA-like space interferometers TM charging are considered. {It is found that electrons and photons below 100 eV give a contribution to the effective charging comparable to that of the whole sample of particles above this energy. In particular, for incident protons ionization contributes twice with respect to low energy kinetic emission and electron backscattering. The other processes are found to play a negligible role. For heavy nuclei only sputtering must be considered. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02690v1-abstract-full').style.display = 'none'; document.getElementById('2012.02690v1-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 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">Accepted for publication in Classical and Quantum Gravity</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.01152">arXiv:2012.01152</a> <span> [<a href="https://arxiv.org/pdf/2012.01152">pdf</a>, <a href="https://arxiv.org/ps/2012.01152">ps</a>, <a href="https://arxiv.org/format/2012.01152">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey 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/abbb90">10.3847/1538-4357/abbb90 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Recurrent galactic cosmic-ray flux modulation in L1 and geomagnetic activity during the declining phase of the solar cycle 24 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Grimani%2C+C">Catia Grimani</a>, <a href="/search/physics?searchtype=author&query=Cesarini%2C+A">Andrea Cesarini</a>, <a href="/search/physics?searchtype=author&query=Fabi%2C+M">Michele Fabi</a>, <a href="/search/physics?searchtype=author&query=Sabbatini%2C+F">Federico Sabbatini</a>, <a href="/search/physics?searchtype=author&query=Telloni%2C+D">Daniele Telloni</a>, <a href="/search/physics?searchtype=author&query=Villani%2C+M">Mattia Villani</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="2012.01152v2-abstract-short" style="display: inline;"> Galactic cosmic-ray (GCR) flux short-term variations ($<$1 month) in the inner heliosphere are mainly associated with the passage of high-speed solar wind streams (HSS) and interplanetary (IP) counterparts of coronal mass ejections (ICMEs). Data gathered with a particle detector flown on board the ESA LISA Pathfinder (LPF) spacecraft, during the declining part of the solar cycle 24 (February 2016… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.01152v2-abstract-full').style.display = 'inline'; document.getElementById('2012.01152v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.01152v2-abstract-full" style="display: none;"> Galactic cosmic-ray (GCR) flux short-term variations ($<$1 month) in the inner heliosphere are mainly associated with the passage of high-speed solar wind streams (HSS) and interplanetary (IP) counterparts of coronal mass ejections (ICMEs). Data gathered with a particle detector flown on board the ESA LISA Pathfinder (LPF) spacecraft, during the declining part of the solar cycle 24 (February 2016 - July 2017) around the Lagrange point L1, have allowed to study the characteristics of recurrent cosmic-ray flux modulations above 70 MeV n$^{-1}$. %These modulations are observed when the solar wind speed is $>$ 400 km s$^{-1}$ and/or the IP magnetic field intensity $>$ 10 nT. It is shown that the amplitude and evolution of individual modulations depend in a unique way on both IP plasma parameters and particle flux intensity before HSS and ICMEs transit. By comparing the LPF data with those gathered contemporaneously with the magnetic spectrometer experiment AMS-02 on board the International Space Station and with those of Earth polar neutron monitors, the GCR flux modulation was studied at different energies during recurrent short-term variations. It is also aimed to set the near real-time particle observation requirements to disentangle the role of long and short-term variations of the GCR flux to evaluate the performance of high-sensitivity instruments in space such as the future interferometers for gravitational wave detection. Finally, the association between recurrent GCR flux variation observations in L1 and weak to moderate geomagnetic activity in 2016-2017 is discussed. Short-term recurrent GCR flux variations are good proxies of recurrent geomagnetic activity when the B$_z$ component of the IP magnetic field is directed northern. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.01152v2-abstract-full').style.display = 'none'; document.getElementById('2012.01152v2-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 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">Journal ref:</span> ApJ 904 64 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.11584">arXiv:1908.11584</a> <span> [<a href="https://arxiv.org/pdf/1908.11584">pdf</a>, <a href="https://arxiv.org/format/1908.11584">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/10.1103/PhysRevLett.123.111101">10.1103/PhysRevLett.123.111101 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LISA Pathfinder Performance Confirmed in an Open-Loop Configuration: Results from the Free-Fall Actuation Mode </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Armano%2C+M">M. Armano</a>, <a href="/search/physics?searchtype=author&query=Audley%2C+H">H. Audley</a>, <a href="/search/physics?searchtype=author&query=Baird%2C+J">J. Baird</a>, <a href="/search/physics?searchtype=author&query=Binetruy%2C+P">P. Binetruy</a>, <a href="/search/physics?searchtype=author&query=Born%2C+M">M. Born</a>, <a href="/search/physics?searchtype=author&query=Bortoluzzi%2C+D">D. Bortoluzzi</a>, <a href="/search/physics?searchtype=author&query=Castelli%2C+E">E. Castelli</a>, <a href="/search/physics?searchtype=author&query=Cavalleri%2C+A">A. Cavalleri</a>, <a href="/search/physics?searchtype=author&query=Cesarini%2C+A">A. Cesarini</a>, <a href="/search/physics?searchtype=author&query=Cruise%2C+A+M">A. M. Cruise</a>, <a href="/search/physics?searchtype=author&query=Danzmann%2C+K">K. Danzmann</a>, <a href="/search/physics?searchtype=author&query=Silva%2C+M+d+D">M. de Deus Silva</a>, <a href="/search/physics?searchtype=author&query=Diepholz%2C+I">I. Diepholz</a>, <a href="/search/physics?searchtype=author&query=Dixon%2C+G">G. Dixon</a>, <a href="/search/physics?searchtype=author&query=Dolesi%2C+R">R. Dolesi</a>, <a href="/search/physics?searchtype=author&query=Ferraioli%2C+L">L. Ferraioli</a>, <a href="/search/physics?searchtype=author&query=Ferroni%2C+V">V. Ferroni</a>, <a href="/search/physics?searchtype=author&query=Fitzsimons%2C+E+D">E. D. Fitzsimons</a>, <a href="/search/physics?searchtype=author&query=Freschi%2C+M">M. Freschi</a>, <a href="/search/physics?searchtype=author&query=Gesa%2C+L">L. Gesa</a>, <a href="/search/physics?searchtype=author&query=Gibert%2C+F">F. Gibert</a>, <a href="/search/physics?searchtype=author&query=Giardini%2C+D">D. Giardini</a>, <a href="/search/physics?searchtype=author&query=Giusteri%2C+R">R. Giusteri</a>, <a href="/search/physics?searchtype=author&query=Grimani%2C+C">C. Grimani</a>, <a href="/search/physics?searchtype=author&query=Grzymisch%2C+J">J. Grzymisch</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="1908.11584v1-abstract-short" style="display: inline;"> We report on the results of the LISA Pathfinder (LPF) free-fall mode experiment, in which the control force needed to compensate the quasistatic differential force acting on two test masses is applied intermittently as a series of "impulse" forces lasting a few seconds and separated by roughly 350 s periods of true free fall. This represents an alternative to the normal LPF mode of operation in wh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.11584v1-abstract-full').style.display = 'inline'; document.getElementById('1908.11584v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.11584v1-abstract-full" style="display: none;"> We report on the results of the LISA Pathfinder (LPF) free-fall mode experiment, in which the control force needed to compensate the quasistatic differential force acting on two test masses is applied intermittently as a series of "impulse" forces lasting a few seconds and separated by roughly 350 s periods of true free fall. This represents an alternative to the normal LPF mode of operation in which this balancing force is applied continuously, with the advantage that the acceleration noise during free fall is measured in the absence of the actuation force, thus eliminating associated noise and force calibration errors. The differential acceleration noise measurement presented here with the free-fall mode agrees with noise measured with the continuous actuation scheme, representing an important and independent confirmation of the LPF result. An additional measurement with larger actuation forces also shows that the technique can be used to eliminate actuation noise when this is a dominant factor. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.11584v1-abstract-full').style.display = 'none'; document.getElementById('1908.11584v1-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> 30 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.04694">arXiv:1904.04694</a> <span> [<a href="https://arxiv.org/pdf/1904.04694">pdf</a>, <a href="https://arxiv.org/ps/1904.04694">ps</a>, <a href="https://arxiv.org/format/1904.04694">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 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/ab0c99">10.3847/1538-4357/ab0c99 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Forbush decreases and $<$ 2-day GCR flux non-recurrent variations studied with LISA Pathfinder </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Grimani%2C+C">C. Grimani</a>, <a href="/search/physics?searchtype=author&query=Armano%2C+M">M. Armano</a>, <a href="/search/physics?searchtype=author&query=Audley%2C+H">H. Audley</a>, <a href="/search/physics?searchtype=author&query=Baird%2C+J">J. Baird</a>, <a href="/search/physics?searchtype=author&query=Benella%2C+S">S. Benella</a>, <a href="/search/physics?searchtype=author&query=Binetruy%2C+P">P. Binetruy</a>, <a href="/search/physics?searchtype=author&query=Born%2C+M">M. Born</a>, <a href="/search/physics?searchtype=author&query=Bortoluzzi%2C+D">D. Bortoluzzi</a>, <a href="/search/physics?searchtype=author&query=Castelli%2C+E">E. Castelli</a>, <a href="/search/physics?searchtype=author&query=Cavalleri%2C+A">A. Cavalleri</a>, <a href="/search/physics?searchtype=author&query=Cesarini%2C+A">A. Cesarini</a>, <a href="/search/physics?searchtype=author&query=Cruise%2C+A+M">A. M. Cruise</a>, <a href="/search/physics?searchtype=author&query=Danzmann%2C+K">K. Danzmann</a>, <a href="/search/physics?searchtype=author&query=Silva%2C+M+d+D">M. de Deus Silva</a>, <a href="/search/physics?searchtype=author&query=Diepholz%2C+I">I. Diepholz</a>, <a href="/search/physics?searchtype=author&query=Dixon%2C+G">G. Dixon</a>, <a href="/search/physics?searchtype=author&query=Dolesi%2C+R">R. Dolesi</a>, <a href="/search/physics?searchtype=author&query=Fabi%2C+M">M. Fabi</a>, <a href="/search/physics?searchtype=author&query=Ferraioli%2C+L">L. Ferraioli</a>, <a href="/search/physics?searchtype=author&query=Ferroni%2C+V">V. Ferroni</a>, <a href="/search/physics?searchtype=author&query=Finetti%2C+N">N. Finetti</a>, <a href="/search/physics?searchtype=author&query=Fitzsimons%2C+E+D">E. D. Fitzsimons</a>, <a href="/search/physics?searchtype=author&query=Freschi%2C+M">M. Freschi</a>, <a href="/search/physics?searchtype=author&query=Gesa%2C+L">L. Gesa</a>, <a href="/search/physics?searchtype=author&query=Gibert%2C+F">F. Gibert</a> , et al. (60 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="1904.04694v1-abstract-short" style="display: inline;"> Non-recurrent short term variations of the galactic cosmic-ray (GCR) flux above 70 MeV n$^{-1}$ were observed between 2016 February 18 and 2017 July 3 aboard the European Space Agency LISA Pathfinder (LPF) mission orbiting around the Lagrange point L1 at 1.5$\times$10$^6$ km from Earth. The energy dependence of three Forbush decreases (FDs) is studied and reported here. A comparison of these obser… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.04694v1-abstract-full').style.display = 'inline'; document.getElementById('1904.04694v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.04694v1-abstract-full" style="display: none;"> Non-recurrent short term variations of the galactic cosmic-ray (GCR) flux above 70 MeV n$^{-1}$ were observed between 2016 February 18 and 2017 July 3 aboard the European Space Agency LISA Pathfinder (LPF) mission orbiting around the Lagrange point L1 at 1.5$\times$10$^6$ km from Earth. The energy dependence of three Forbush decreases (FDs) is studied and reported here. A comparison of these observations with others carried out in space down to the energy of a few tens of MeV n$^{-1}$ shows that the same GCR flux parameterization applies to events of different intensity during the main phase. FD observations in L1 with LPF and geomagnetic storm occurrence is also presented. Finally, the characteristics of GCR flux non-recurrent variations (peaks and depressions) of duration $<$ 2 days and their association with interplanetary structures are investigated. It is found that, most likely, plasma compression regions between subsequent corotating high-speed streams cause peaks, while heliospheric current sheet crossing cause the majority of the depressions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.04694v1-abstract-full').style.display = 'none'; document.getElementById('1904.04694v1-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 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> M. Armano et al 2019 ApJ 874 167 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1807.02435">arXiv:1807.02435</a> <span> [<a href="https://arxiv.org/pdf/1807.02435">pdf</a>, <a href="https://arxiv.org/format/1807.02435">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.98.062001">10.1103/PhysRevD.98.062001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Precision Charge Control for Isolated Free-Falling Test Masses: LISA Pathfinder Results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Armano%2C+M">M. Armano</a>, <a href="/search/physics?searchtype=author&query=Audley%2C+H">H. Audley</a>, <a href="/search/physics?searchtype=author&query=Baird%2C+J">J. Baird</a>, <a href="/search/physics?searchtype=author&query=Binetruy%2C+P">P. Binetruy</a>, <a href="/search/physics?searchtype=author&query=Born%2C+M">M. Born</a>, <a href="/search/physics?searchtype=author&query=Bortoluzzi%2C+D">D. Bortoluzzi</a>, <a href="/search/physics?searchtype=author&query=Castelli%2C+E">E. Castelli</a>, <a href="/search/physics?searchtype=author&query=Cavalleri%2C+A">A. Cavalleri</a>, <a href="/search/physics?searchtype=author&query=Cesarini%2C+A">A. Cesarini</a>, <a href="/search/physics?searchtype=author&query=Cruise%2C+A+M">A. M. Cruise</a>, <a href="/search/physics?searchtype=author&query=Danzmann%2C+K">K. Danzmann</a>, <a href="/search/physics?searchtype=author&query=Silva%2C+M+d+D">M. de Deus Silva</a>, <a href="/search/physics?searchtype=author&query=Diepholz%2C+I">I. Diepholz</a>, <a href="/search/physics?searchtype=author&query=Dixon%2C+G">G. Dixon</a>, <a href="/search/physics?searchtype=author&query=Dolesi%2C+R">R. Dolesi</a>, <a href="/search/physics?searchtype=author&query=Ferraioli%2C+L">L. Ferraioli</a>, <a href="/search/physics?searchtype=author&query=Ferroni%2C+V">V. Ferroni</a>, <a href="/search/physics?searchtype=author&query=Fitzsimons%2C+E+D">E. D. Fitzsimons</a>, <a href="/search/physics?searchtype=author&query=Freschi%2C+M">M. Freschi</a>, <a href="/search/physics?searchtype=author&query=Gesa%2C+L">L. Gesa</a>, <a href="/search/physics?searchtype=author&query=Giardini%2C+D">D. Giardini</a>, <a href="/search/physics?searchtype=author&query=Gibert%2C+F">F. Gibert</a>, <a href="/search/physics?searchtype=author&query=Giusteri%2C+R">R. Giusteri</a>, <a href="/search/physics?searchtype=author&query=Grimani%2C+C">C. Grimani</a>, <a href="/search/physics?searchtype=author&query=Grzymisch%2C+J">J. Grzymisch</a> , et al. (60 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="1807.02435v2-abstract-short" style="display: inline;"> The LISA Pathfinder charge management device was responsible for neutralising the cosmic ray induced electric charge that inevitably accumulated on the free-falling test masses at the heart of the experiment. We present measurements made on ground and in-flight that quantify the performance of this contactless discharge system which was based on photo-emission under UV illumination. In addition, a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.02435v2-abstract-full').style.display = 'inline'; document.getElementById('1807.02435v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.02435v2-abstract-full" style="display: none;"> The LISA Pathfinder charge management device was responsible for neutralising the cosmic ray induced electric charge that inevitably accumulated on the free-falling test masses at the heart of the experiment. We present measurements made on ground and in-flight that quantify the performance of this contactless discharge system which was based on photo-emission under UV illumination. In addition, a two-part simulation is described that was developed alongside the hardware. Modelling of the absorbed UV light within the Pathfinder sensor was carried out with the GEANT4 software toolkit and a separate MATLAB charge transfer model calculated the net photocurrent between the test masses and surrounding housing in the presence of AC and DC electric fields. We confront the results of these models with observations and draw conclusions for the design of discharge systems for future experiments like LISA that will also employ free-falling test masses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.02435v2-abstract-full').style.display = 'none'; document.getElementById('1807.02435v2-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 98, 062001 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1802.09374">arXiv:1802.09374</a> <span> [<a href="https://arxiv.org/pdf/1802.09374">pdf</a>, <a href="https://arxiv.org/ps/1802.09374">ps</a>, <a href="https://arxiv.org/format/1802.09374">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="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.3847/1538-4357/aaa774">10.3847/1538-4357/aaa774 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characteristics and energy dependence of recurrent galactic cosmic-ray flux depressions and of a Forbush decrease with LISA Pathfinder </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Armano%2C+M">M. Armano</a>, <a href="/search/physics?searchtype=author&query=Audley%2C+H">H. Audley</a>, <a href="/search/physics?searchtype=author&query=Baird%2C+J">J. Baird</a>, <a href="/search/physics?searchtype=author&query=Bassan%2C+M">M. Bassan</a>, <a href="/search/physics?searchtype=author&query=Benella%2C+S">S. Benella</a>, <a href="/search/physics?searchtype=author&query=Binetruy%2C+P">P. Binetruy</a>, <a href="/search/physics?searchtype=author&query=Born%2C+M">M. Born</a>, <a href="/search/physics?searchtype=author&query=Bortoluzzi%2C+D">D. Bortoluzzi</a>, <a href="/search/physics?searchtype=author&query=Cavalleri%2C+A">A. Cavalleri</a>, <a href="/search/physics?searchtype=author&query=Cesarini%2C+A">A. Cesarini</a>, <a href="/search/physics?searchtype=author&query=Cruise%2C+A+M">A. M. Cruise</a>, <a href="/search/physics?searchtype=author&query=Danzmann%2C+K">K. Danzmann</a>, <a href="/search/physics?searchtype=author&query=Silva%2C+M+d+D">M. de Deus Silva</a>, <a href="/search/physics?searchtype=author&query=Diepholz%2C+I">I. Diepholz</a>, <a href="/search/physics?searchtype=author&query=Dixon%2C+G">G. Dixon</a>, <a href="/search/physics?searchtype=author&query=Dolesi%2C+R">R. Dolesi</a>, <a href="/search/physics?searchtype=author&query=Fabi%2C+M">M. Fabi</a>, <a href="/search/physics?searchtype=author&query=Ferraioli%2C+L">L. Ferraioli</a>, <a href="/search/physics?searchtype=author&query=Ferroni%2C+V">V. Ferroni</a>, <a href="/search/physics?searchtype=author&query=Finetti%2C+N">N. Finetti</a>, <a href="/search/physics?searchtype=author&query=Fitzsimons%2C+E+D">E. D. Fitzsimons</a>, <a href="/search/physics?searchtype=author&query=Freschi%2C+M">M. Freschi</a>, <a href="/search/physics?searchtype=author&query=Gesa%2C+L">L. Gesa</a>, <a href="/search/physics?searchtype=author&query=Gibert%2C+F">F. Gibert</a>, <a href="/search/physics?searchtype=author&query=Giardini%2C+D">D. Giardini</a> , et al. (60 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="1802.09374v2-abstract-short" style="display: inline;"> Galactic cosmic-ray (GCR) energy spectra observed in the inner heliosphere are modulated by the solar activity, the solar polarity and structures of solar and interplanetary origin. A high counting rate particle detector (PD) aboard LISA Pathfinder (LPF), meant for subsystems diagnostics, was devoted to the measurement of galactic cosmic-ray and solar energetic particle integral fluxes above 70 Me… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.09374v2-abstract-full').style.display = 'inline'; document.getElementById('1802.09374v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.09374v2-abstract-full" style="display: none;"> Galactic cosmic-ray (GCR) energy spectra observed in the inner heliosphere are modulated by the solar activity, the solar polarity and structures of solar and interplanetary origin. A high counting rate particle detector (PD) aboard LISA Pathfinder (LPF), meant for subsystems diagnostics, was devoted to the measurement of galactic cosmic-ray and solar energetic particle integral fluxes above 70 MeV n$^{-1}$ up to 6500 counts s$^{-1}$. PD data were gathered with a sampling time of 15 s. Characteristics and energy-dependence of GCR flux recurrent depressions and of a Forbush decrease dated August 2, 2016 are reported here. The capability of interplanetary missions, carrying PDs for instrument performance purposes, in monitoring the passage of interplanetary coronal mass ejections (ICMEs) is also discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.09374v2-abstract-full').style.display = 'none'; document.getElementById('1802.09374v2-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> 27 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, 854, 2018, 113 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1306.4487">arXiv:1306.4487</a> <span> [<a href="https://arxiv.org/pdf/1306.4487">pdf</a>, <a href="https://arxiv.org/ps/1306.4487">ps</a>, <a href="https://arxiv.org/format/1306.4487">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</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="Data Analysis, Statistics and Probability">physics.data-an</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"> State space modelling and data analysis exercises in LISA Pathfinder </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Nofrarias%2C+M">M Nofrarias</a>, <a href="/search/physics?searchtype=author&query=Antonucci%2C+F">F Antonucci</a>, <a href="/search/physics?searchtype=author&query=Armano%2C+M">M Armano</a>, <a href="/search/physics?searchtype=author&query=Audley%2C+H">H Audley</a>, <a href="/search/physics?searchtype=author&query=Auger%2C+G">G Auger</a>, <a href="/search/physics?searchtype=author&query=Benedetti%2C+M">M Benedetti</a>, <a href="/search/physics?searchtype=author&query=Binetruy%2C+P">P Binetruy</a>, <a href="/search/physics?searchtype=author&query=Bogenstahl%2C+J">J Bogenstahl</a>, <a href="/search/physics?searchtype=author&query=Bortoluzzi%2C+D">D Bortoluzzi</a>, <a href="/search/physics?searchtype=author&query=Brandt%2C+N">N Brandt</a>, <a href="/search/physics?searchtype=author&query=Caleno%2C+M">M Caleno</a>, <a href="/search/physics?searchtype=author&query=Cavalleri%2C+A">A Cavalleri</a>, <a href="/search/physics?searchtype=author&query=Congedo%2C+G">G Congedo</a>, <a href="/search/physics?searchtype=author&query=Cruise%2C+M">M Cruise</a>, <a href="/search/physics?searchtype=author&query=Danzmann%2C+K">K Danzmann</a>, <a href="/search/physics?searchtype=author&query=De+Marchi%2C+F">F De Marchi</a>, <a href="/search/physics?searchtype=author&query=Diaz-Aguilo%2C+M">M Diaz-Aguilo</a>, <a href="/search/physics?searchtype=author&query=Diepholz%2C+I">I Diepholz</a>, <a href="/search/physics?searchtype=author&query=Dixon%2C+G">G Dixon</a>, <a href="/search/physics?searchtype=author&query=Dolesi%2C+R">R Dolesi</a>, <a href="/search/physics?searchtype=author&query=Dunbar%2C+N">N Dunbar</a>, <a href="/search/physics?searchtype=author&query=Fauste%2C+J">J Fauste</a>, <a href="/search/physics?searchtype=author&query=Ferraioli%2C+L">L Ferraioli</a>, <a href="/search/physics?searchtype=author&query=Fichter%2C+V+F+W">V Ferroni W Fichter</a>, <a href="/search/physics?searchtype=author&query=Fitzsimons%2C+E">E Fitzsimons</a> , et al. (61 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="1306.4487v2-abstract-short" style="display: inline;"> LISA Pathfinder is a mission planned by the European Space Agency to test the key technologies that will allow the detection of gravitational waves in space. The instrument on-board, the LISA Technology package, will undergo an exhaustive campaign of calibrations and noise characterisation campaigns in order to fully describe the noise model. Data analysis plays an important role in the mission an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1306.4487v2-abstract-full').style.display = 'inline'; document.getElementById('1306.4487v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1306.4487v2-abstract-full" style="display: none;"> LISA Pathfinder is a mission planned by the European Space Agency to test the key technologies that will allow the detection of gravitational waves in space. The instrument on-board, the LISA Technology package, will undergo an exhaustive campaign of calibrations and noise characterisation campaigns in order to fully describe the noise model. Data analysis plays an important role in the mission and for that reason the data analysis team has been developing a toolbox which contains all the functionalities required during operations. In this contribution we give an overview of recent activities, focusing on the improvements in the modelling of the instrument and in the data analysis campaigns performed both with real and simulated data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1306.4487v2-abstract-full').style.display = 'none'; document.getElementById('1306.4487v2-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 June, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 June, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2013. </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">Plenary talk presented at the 9th International LISA Symposium, 21-25 May 2012, Paris</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2013ASPC..467..161N </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 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