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</div> <div class="control"> <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/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> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a 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