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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/2304.02597">arXiv:2304.02597</a> <span> [<a href="https://arxiv.org/pdf/2304.02597">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Geophysics">physics.geo-ph</span> </div> </div> <p class="title is-5 mathjax"> Lithosphere strain rate and stress field orientations near the Alpine arc in Switzerland </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Houli%C3%A9%2C+N">Nicolas Houli茅</a>, <a href="/search/physics?searchtype=author&query=Woessner%2C+J">Jochen Woessner</a>, <a href="/search/physics?searchtype=author&query=Giardini%2C+D">Domenico Giardini</a>, <a href="/search/physics?searchtype=author&query=Rothacher%2C+M">Markus Rothacher</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.02597v1-abstract-short" style="display: inline;"> In this study we test whether principal components of the strain rate and stress tensors align within Switzerland. We find that 1) Helvetic Nappes line (HNL) is the relevant tectonic boundary to define different domains of crustal stress/surface strain rates orientations and 2) orientations of T- axes (of moment tensor solutions) and long-term asthenosphere cumulative finite strain (from SKS shear… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02597v1-abstract-full').style.display = 'inline'; document.getElementById('2304.02597v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.02597v1-abstract-full" style="display: none;"> In this study we test whether principal components of the strain rate and stress tensors align within Switzerland. We find that 1) Helvetic Nappes line (HNL) is the relevant tectonic boundary to define different domains of crustal stress/surface strain rates orientations and 2) orientations of T- axes (of moment tensor solutions) and long-term asthenosphere cumulative finite strain (from SKS shear wave splitting) are consistent at the scale of the Alpine arc in Switzerland. At a more local scale, we find that seismic activity and surface deformation are in agreement but in three regions (Basel, Swiss Jura and Ticino); possibly because of the low levels of deformation and/or seismicity. In the Basel area, deep seismicity exists while surface deformation is absent. In the Ticino and the Swiss Jura, where seismic activity is close to absent, surface deformation is detected at a level of ~2 10E-8/yr (~6.3 10E-16/s). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02597v1-abstract-full').style.display = 'none'; document.getElementById('2304.02597v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.04585">arXiv:2210.04585</a> <span> [<a href="https://arxiv.org/pdf/2210.04585">pdf</a>, <a href="https://arxiv.org/format/2210.04585">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Geophysics">physics.geo-ph</span> </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/10.26443/seismica.v1i1.253">10.26443/seismica.v1i1.253 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Locating the Nordstream explosions without a velocity model using polarization analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=St%C3%A4hler%2C+S+C">Simon C. St盲hler</a>, <a href="/search/physics?searchtype=author&query=Zenh%C3%A4usern%2C+G">G. Zenh盲usern</a>, <a href="/search/physics?searchtype=author&query=Clinton%2C+J">J. Clinton</a>, <a href="/search/physics?searchtype=author&query=Giardini%2C+D">D. Giardini</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="2210.04585v1-abstract-short" style="display: inline;"> The seismic events that preceded the leaks in the Nordstream pipelines in the Baltic Sea have been interpreted as explosions on the seabed, most likely man-made. We use a polarization-based location method initially developed for marsquakes to locate the source region without a subsurface velocity model. We show that the 2 largest seismic events can be unambiguously attributed to the methane plume… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.04585v1-abstract-full').style.display = 'inline'; document.getElementById('2210.04585v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.04585v1-abstract-full" style="display: none;"> The seismic events that preceded the leaks in the Nordstream pipelines in the Baltic Sea have been interpreted as explosions on the seabed, most likely man-made. We use a polarization-based location method initially developed for marsquakes to locate the source region without a subsurface velocity model. We show that the 2 largest seismic events can be unambiguously attributed to the methane plumes observed on the sea surface. The two largest events can be located with this method, using 4 and 5 stations located around the source, with location uncertainties of 30km and 10x60km. We can further show that both events emitted seismic energy for at least ten minutes after the initial explosion, indicative of resonances in the water column or the depressurizing pipeline. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.04585v1-abstract-full').style.display = 'none'; document.getElementById('2210.04585v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">6 pages, 2 figures, submitted as fast report to Seismica</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> published in Seismica (1) 1, 2022 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.15136">arXiv:2206.15136</a> <span> [<a href="https://arxiv.org/pdf/2206.15136">pdf</a>, <a href="https://arxiv.org/format/2206.15136">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="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41550-022-01803-y">10.1038/s41550-022-01803-y <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Tectonics of Cerberus Fossae unveiled by marsquakes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=St%C3%A4hler%2C+S+C">Simon C. St盲hler</a>, <a href="/search/physics?searchtype=author&query=Mittelholz%2C+A">Anna Mittelholz</a>, <a href="/search/physics?searchtype=author&query=Perrin%2C+C">Cl茅ment Perrin</a>, <a href="/search/physics?searchtype=author&query=Kawamura%2C+T">Taichi Kawamura</a>, <a href="/search/physics?searchtype=author&query=Kim%2C+D">Doyeon Kim</a>, <a href="/search/physics?searchtype=author&query=Knapmeyer%2C+M">Martin Knapmeyer</a>, <a href="/search/physics?searchtype=author&query=Zenh%C3%A4usern%2C+G">G茅raldine Zenh盲usern</a>, <a href="/search/physics?searchtype=author&query=Clinton%2C+J">John Clinton</a>, <a href="/search/physics?searchtype=author&query=Giardini%2C+D">Domenico Giardini</a>, <a href="/search/physics?searchtype=author&query=Lognonn%C3%A9%2C+P">Philippe Lognonn茅</a>, <a href="/search/physics?searchtype=author&query=Banerdt%2C+W+B">W. Bruce Banerdt</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="2206.15136v1-abstract-short" style="display: inline;"> The InSight mission has measured Mars' seismicity since February 2018 and has allowed to investigate tectonics on another planet. Seismic data shows that most of the widely distributed surface faults are not seismically active, and that seismicity is mostly originating from a single graben structure, the Cerberus Fossae. We show that both major families of marsquakes characterized by low and high… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.15136v1-abstract-full').style.display = 'inline'; document.getElementById('2206.15136v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.15136v1-abstract-full" style="display: none;"> The InSight mission has measured Mars' seismicity since February 2018 and has allowed to investigate tectonics on another planet. Seismic data shows that most of the widely distributed surface faults are not seismically active, and that seismicity is mostly originating from a single graben structure, the Cerberus Fossae. We show that both major families of marsquakes characterized by low and high frequency content, LF and HF events respectively, are located on central and eastern parts of this graben system. LF hypocenters are located at 15-50 km depth and the spectral character suggests a structurally weak, potentially warm source region consistent with recent volcanic activity at those depths. HF marsquakes occur in the brittle, shallow part of the crust and might originate in fault planes associated with the graben flanks. Estimated magnitudes are between 2.8 and 3.8, resulting in a total seismic moment release within Cerberus Fossae of 1.4-5.6 $\times10^{15}$ Nm/yr, or at least half of the observed value of the entire planet. Our findings confirm that Cerberus Fossae represents a unique tectonic setting shaped by current day volcanic processes, with implications for minimum local heat flow. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.15136v1-abstract-full').style.display = 'none'; document.getElementById('2206.15136v1-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">15 pages, 8 figures, Nature Astronomy (2022)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> InSight contribution 233 <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 86A15 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.12959">arXiv:2204.12959</a> <span> [<a href="https://arxiv.org/pdf/2204.12959">pdf</a>, <a href="https://arxiv.org/format/2204.12959">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Geophysics">physics.geo-ph</span> </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/10.1785/0120220019">10.1785/0120220019 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Low Frequency Marsquakes and Where to Find Them: Back Azimuth Determination Using a Polarization Analysis Approach </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Zenh%C3%A4usern%2C+G">G茅raldine Zenh盲usern</a>, <a href="/search/physics?searchtype=author&query=St%C3%A4hler%2C+S+C">Simon C. St盲hler</a>, <a href="/search/physics?searchtype=author&query=Clinton%2C+J+F">John F. Clinton</a>, <a href="/search/physics?searchtype=author&query=Giardini%2C+D">Domenico Giardini</a>, <a href="/search/physics?searchtype=author&query=Ceylan%2C+S">Savas Ceylan</a>, <a href="/search/physics?searchtype=author&query=Garcia%2C+R+F">Rapha毛l F. Garcia</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="2204.12959v1-abstract-short" style="display: inline;"> NASA's InSight mission on Mars continues to record seismic data over 3 years after landing, and to date, over a thousand marsquakes have been identified. With only a single seismic station, the determination of the epicentral location is far more challenging than on Earth. The Marsquake Service (MQS) produces seismicity catalogues from data collected by InSight and provides distance and back azimu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.12959v1-abstract-full').style.display = 'inline'; document.getElementById('2204.12959v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.12959v1-abstract-full" style="display: none;"> NASA's InSight mission on Mars continues to record seismic data over 3 years after landing, and to date, over a thousand marsquakes have been identified. With only a single seismic station, the determination of the epicentral location is far more challenging than on Earth. The Marsquake Service (MQS) produces seismicity catalogues from data collected by InSight and provides distance and back azimuth estimates when these can be reliably determined - when both are available these are combined to provide a location. Currently, MQS do not assign a back azimuth to the vast majority of marsquakes. In this work we develop and apply a polarization analysis method to determine the back azimuth of seismic events from the polarization of observed P and S-wave arrivals. The method is first applied to synthetic marsquakes, and then calibrated using a set of well-located earthquakes that have been recorded in Tennant Creek, Australia. We find that the back azimuth is estimated reliably using our polarization method. The same approach is then used for a set of high quality marsquakes recorded up to October 2021. We are able to estimate back azimuths for 24 marsquakes, 16 of these without MQS back azimuths. We locate most events to the east of InSight, in the general region of Cerberus Fossae. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.12959v1-abstract-full').style.display = 'none'; document.getElementById('2204.12959v1-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">27 pages, 11 figures. Supplement 24 pages, 23 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Bulletin of the Seismological Society of America (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.04467">arXiv:2204.04467</a> <span> [<a href="https://arxiv.org/pdf/2204.04467">pdf</a>, <a href="https://arxiv.org/format/2204.04467">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="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</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.106.062003">10.1103/PhysRevD.106.062003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Bayesian parameter-estimation of Galactic binaries in LISA data with Gaussian Process Regression </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Strub%2C+S+H">Stefan H. Strub</a>, <a href="/search/physics?searchtype=author&query=Ferraioli%2C+L">Luigi Ferraioli</a>, <a href="/search/physics?searchtype=author&query=Schmelzbach%2C+C">Cedric Schmelzbach</a>, <a href="/search/physics?searchtype=author&query=St%C3%A4hler%2C+S+C">Simon C. St盲hler</a>, <a href="/search/physics?searchtype=author&query=Giardini%2C+D">Domenico Giardini</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="2204.04467v3-abstract-short" style="display: inline;"> The Laser Interferometer Space Antenna (LISA), which is currently under construction, is designed to measure gravitational wave signals in the milli-Hertz frequency band. It is expected that tens of millions of Galactic binaries will be the dominant sources of observed gravitational waves. The Galactic binaries producing signals at mHz frequency range emit quasi monochromatic gravitational waves,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.04467v3-abstract-full').style.display = 'inline'; document.getElementById('2204.04467v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.04467v3-abstract-full" style="display: none;"> The Laser Interferometer Space Antenna (LISA), which is currently under construction, is designed to measure gravitational wave signals in the milli-Hertz frequency band. It is expected that tens of millions of Galactic binaries will be the dominant sources of observed gravitational waves. The Galactic binaries producing signals at mHz frequency range emit quasi monochromatic gravitational waves, which will be constantly measured by LISA. To resolve as many Galactic binaries as possible is a central challenge of the upcoming LISA data set analysis. Although it is estimated that tens of thousands of these overlapping gravitational wave signals are resolvable, and the rest blurs into a galactic foreground noise; extracting tens of thousands of signals using Bayesian approaches is still computationally expensive. We developed a new end-to-end pipeline using Gaussian Process Regression to model the log-likelihood function in order to rapidly compute Bayesian posterior distributions. Using the pipeline we are able to solve the Lisa Data Challenge (LDC) 1-3 consisting of noisy data as well as additional challenges with overlapping signals and particularly faint signals. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.04467v3-abstract-full').style.display = 'none'; document.getElementById('2204.04467v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">13 pages, 10 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.04438">arXiv:2112.04438</a> <span> [<a href="https://arxiv.org/pdf/2112.04438">pdf</a>, <a href="https://arxiv.org/format/2112.04438">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="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Geophysics">physics.geo-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/10.1007/s11214-022-00941-z">10.1007/s11214-022-00941-z <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The InSight HP$^3$ Penetrator (Mole) on Mars: Soil Properties Derived From the Penetration Attempts and Related Activities </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Spohn%2C+T">T. Spohn</a>, <a href="/search/physics?searchtype=author&query=Hudson%2C+T+L">T. L. Hudson</a>, <a href="/search/physics?searchtype=author&query=Marteau%2C+E">E. Marteau</a>, <a href="/search/physics?searchtype=author&query=Golombek%2C+M">M. Golombek</a>, <a href="/search/physics?searchtype=author&query=Grott%2C+M">M. Grott</a>, <a href="/search/physics?searchtype=author&query=Wippermann%2C+T">T. Wippermann</a>, <a href="/search/physics?searchtype=author&query=Ali%2C+K+S">K. S. Ali</a>, <a href="/search/physics?searchtype=author&query=Schmelzbach%2C+C">C. Schmelzbach</a>, <a href="/search/physics?searchtype=author&query=Kedar%2C+S">S. Kedar</a>, <a href="/search/physics?searchtype=author&query=Hurst%2C+K">K. Hurst</a>, <a href="/search/physics?searchtype=author&query=Trebi-Ollennu%2C+A">A. Trebi-Ollennu</a>, <a href="/search/physics?searchtype=author&query=Ansan%2C+V">V. Ansan</a>, <a href="/search/physics?searchtype=author&query=Garvin%2C+J">J. Garvin</a>, <a href="/search/physics?searchtype=author&query=Knollenberg%2C+J">J. Knollenberg</a>, <a href="/search/physics?searchtype=author&query=Mueller%2C+N">N. Mueller</a>, <a href="/search/physics?searchtype=author&query=Piqeux%2C+S">S. Piqeux</a>, <a href="/search/physics?searchtype=author&query=Lichtenheldt%2C+R">R. Lichtenheldt</a>, <a href="/search/physics?searchtype=author&query=Krause%2C+C">C. Krause</a>, <a href="/search/physics?searchtype=author&query=Fantinati%2C+C">C. Fantinati</a>, <a href="/search/physics?searchtype=author&query=Brinkman%2C+N">N. Brinkman</a>, <a href="/search/physics?searchtype=author&query=Sollberger%2C+D">D. Sollberger</a>, <a href="/search/physics?searchtype=author&query=Delage%2C+P">P. Delage</a>, <a href="/search/physics?searchtype=author&query=Vrettos%2C+C">C. Vrettos</a>, <a href="/search/physics?searchtype=author&query=Reershemius%2C+S">S. Reershemius</a>, <a href="/search/physics?searchtype=author&query=Wisniewski%2C+L">L. Wisniewski</a> , et al. (9 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="2112.04438v1-abstract-short" style="display: inline;"> The NASA InSight Lander on Mars includes the Heat Flow and Physical Properties Package HP$^3$ to measure the surface heat flow of the planet. The package uses temperature sensors that would have been brought to the target depth of 3--5 m by a small penetrator, nicknamed the mole. The mole requiring friction on its hull to balance remaining recoil from its hammer mechanism did not penetrate to the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.04438v1-abstract-full').style.display = 'inline'; document.getElementById('2112.04438v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.04438v1-abstract-full" style="display: none;"> The NASA InSight Lander on Mars includes the Heat Flow and Physical Properties Package HP$^3$ to measure the surface heat flow of the planet. The package uses temperature sensors that would have been brought to the target depth of 3--5 m by a small penetrator, nicknamed the mole. The mole requiring friction on its hull to balance remaining recoil from its hammer mechanism did not penetrate to the targeted depth. Instead, by precessing about a point midway along its hull, it carved a 7 cm deep and 5-6 cm wide pit and reached a depth of initially 31 cm. The root cause of the failure - as was determined through an extensive, almost two years long campaign - was a lack of friction in an unexpectedly thick cohesive duricrust. During the campaign -- described in detail in this paper -- the mole penetrated further aided by friction applied using the scoop at the end of the robotic Instrument Deployment Arm and by direct support by the latter. The mole finally reached a depth of 40 cm, bringing the mole body 1--2 cm below the surface. The penetration record of the mole and its thermal sensors were used to measure thermal and mechanical soil parameters such as the thermal conductivity and the penetration resistance of the duricrust and its cohesion. The hammerings of the mole were recorded by the seismometer SEIS and the signals could be used to derive a P-wave velocity and a S-wave velocity and elastic moduli representative of the topmost tens of cm of the regolith. The combined data were used to derive a model of the regolith that has an about 20 cm thick duricrust underneath a 1 cm thick unconsolidated layer of sand mixed with dust and above another 10 cm of unconsolidated sand. Underneath the latter, a layer more resistant to penetration and possibly consisting of debris from a small impact crater is inferred. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.04438v1-abstract-full').style.display = 'none'; document.getElementById('2112.04438v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">78 pages 22 figures, , submitted to Space Science Reviews</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> InSight contribution # 223 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Space Science Reviews (2022) 218: 72 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.13206">arXiv:2109.13206</a> <span> [<a href="https://arxiv.org/pdf/2109.13206">pdf</a>, <a href="https://arxiv.org/format/2109.13206">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="Geophysics">physics.geo-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/10.1016/j.icarus.2021.114871">10.1016/j.icarus.2021.114871 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Tidal-Thermal Evolution of the Pluto-Charon System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bagheri%2C+A">Amirhossein Bagheri</a>, <a href="/search/physics?searchtype=author&query=Khan%2C+A">Amir Khan</a>, <a href="/search/physics?searchtype=author&query=Deschamps%2C+F">Frederic Deschamps</a>, <a href="/search/physics?searchtype=author&query=Samuel%2C+H">Henri Samuel</a>, <a href="/search/physics?searchtype=author&query=Kruglyakov%2C+M">Mikhail Kruglyakov</a>, <a href="/search/physics?searchtype=author&query=Giardini%2C+D">Domenico Giardini</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.13206v1-abstract-short" style="display: inline;"> Existence of subsurface oceans on the satellites of the giant planets and Trans-Neptunian objects has been predicted for some time. Oceans on icy worlds exert a considerable influence on the dynamics of the ice-ocean system and, because of the astrobiological potential, represent an important objective for future missions. The Pluto-Charon system is representative of an icy moon orbiting a dwarf p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.13206v1-abstract-full').style.display = 'inline'; document.getElementById('2109.13206v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.13206v1-abstract-full" style="display: none;"> Existence of subsurface oceans on the satellites of the giant planets and Trans-Neptunian objects has been predicted for some time. Oceans on icy worlds exert a considerable influence on the dynamics of the ice-ocean system and, because of the astrobiological potential, represent an important objective for future missions. The Pluto-Charon system is representative of an icy moon orbiting a dwarf planet formed from the remnants of a giant impact. Evolution of icy moons is primarily controlled by the mode and efficiency of heat transfer through the outer ice shell, which is influenced by the presence of impurities, by tidal dissipation in the ice shell, and the radioactive element budget in the core. Previous studies on the evolution of the Pluto-Charon system considered either only the thermal or the tidal evolution, and in the cases where both were considered, the important effect of the presence of impurities in the liquid oceans was not addressed. We consider the joint tidal-thermal evolution of the system by combining a comprehensive tidal model that incorporates a viscoelastic tidal response with a parameterized convection model developed for icy worlds. This approach enables an extensive analysis of the conditions required for formation and maintenance of subsurface liquid oceans to the present. Our results show that because of fast circularization and synchronization of the orbits, tidal heating is only important during the early stages of evolution (<1 Myr). We test the sensitivity of our results to the initial orbital and thermal parameters. In all the cases, oceans on Pluto are always predicted to remain liquid to the present, ranging from 40 km to 150-km thick, whereas oceans on Charon have solidified. This is supported by New Horizons observations of extensional faults on Pluto and both extensional and compressional faults on Charon. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.13206v1-abstract-full').style.display = 'none'; document.getElementById('2109.13206v1-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 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.12807">arXiv:2009.12807</a> <span> [<a href="https://arxiv.org/pdf/2009.12807">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 Methods for Astrophysics">astro-ph.IM</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="Geophysics">physics.geo-ph</span> </div> </div> <p class="title is-5 mathjax"> Exploring the near-surface at the lunar South Pole with geophysical tools </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Schmelzbach%2C+C">C. Schmelzbach</a>, <a href="/search/physics?searchtype=author&query=St%C3%A4hler%2C+S">S. St盲hler</a>, <a href="/search/physics?searchtype=author&query=Schmerr%2C+N+C">N. C. Schmerr</a>, <a href="/search/physics?searchtype=author&query=Knapmeyer%2C+M">M. Knapmeyer</a>, <a href="/search/physics?searchtype=author&query=Sollberger%2C+D">D. Sollberger</a>, <a href="/search/physics?searchtype=author&query=Edme%2C+P">P. Edme</a>, <a href="/search/physics?searchtype=author&query=Khan%2C+A">A. Khan</a>, <a href="/search/physics?searchtype=author&query=Brinkman%2C+N">N. Brinkman</a>, <a href="/search/physics?searchtype=author&query=Ferraioli%2C+L">L. Ferraioli</a>, <a href="/search/physics?searchtype=author&query=Robertsson%2C+J+O+A">J. O. A. Robertsson</a>, <a href="/search/physics?searchtype=author&query=Giardini%2C+D">D. Giardini</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="2009.12807v1-abstract-short" style="display: inline;"> Geophysical imaging of the lunar near-surface structure will be key for in situ resource utilization, identification of hazards for crews and infrastructure, and answering science questions on the formation and interior of the Moon. The goal of this white paper is to highlight the value of ground-based geophysical experiments by a crew and to outline a series of experiments to address key science… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.12807v1-abstract-full').style.display = 'inline'; document.getElementById('2009.12807v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.12807v1-abstract-full" style="display: none;"> Geophysical imaging of the lunar near-surface structure will be key for in situ resource utilization, identification of hazards for crews and infrastructure, and answering science questions on the formation and interior of the Moon. The goal of this white paper is to highlight the value of ground-based geophysical experiments by a crew and to outline a series of experiments to address key science questions. Specifically, we propose for the Artemis III crewed mission multidisciplinary investigations using geophysical methods such as seismic, seismological, ground penetrating radar, and electromagnetic techniques. We identified a series of prime near-surface targets for such geophysical investigations: (1) establishing a lunar fault monitoring observatory across a lobate scarp to study recent lunar seismicity, (2) determining the physical properties of the regolith at the landing site, (3) investigating the structure and in-situ properties of permanently shadowed regions in the context of the search for water ice and other cold-trapped volatiles, and (4) imaging the interior structure of the South-Pole Aitken basin. Beyond Artemis III, the Moon will serve as a comprehensive testbed for extra-terrestrial geophysics. Hence, lessons learned from human geophysical exploration of the Moon will be key for the exploration of the moons of Mars and near-Earth object(s), and prepare us for the human exploration of space beyond the Moon. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.12807v1-abstract-full').style.display = 'none'; document.getElementById('2009.12807v1-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 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">2 pages, 1 figure, 27 references</span> </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/1803.09635">arXiv:1803.09635</a> <span> [<a href="https://arxiv.org/pdf/1803.09635">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Geophysics">physics.geo-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/978-3-319-99670-7_46">10.1007/978-3-319-99670-7_46 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Autonomous decision-making against induced seismicity in deep fluid injections </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Mignan%2C+A">Arnaud Mignan</a>, <a href="/search/physics?searchtype=author&query=Broccardo%2C+M">Marco Broccardo</a>, <a href="/search/physics?searchtype=author&query=Wiemer%2C+S">Stefan Wiemer</a>, <a href="/search/physics?searchtype=author&query=Giardini%2C+D">Domenico Giardini</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="1803.09635v1-abstract-short" style="display: inline;"> The rise in the frequency of anthropogenic earthquakes due to deep fluid injections is posing serious economic, societal, and legal challenges to geo-energy and waste-disposal projects. We propose an actuarial approach to mitigate this risk, first by defining an autonomous decision-making process based on an adaptive traffic light system (ATLS) to stop risky injections, and second by quantifying a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.09635v1-abstract-full').style.display = 'inline'; document.getElementById('1803.09635v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1803.09635v1-abstract-full" style="display: none;"> The rise in the frequency of anthropogenic earthquakes due to deep fluid injections is posing serious economic, societal, and legal challenges to geo-energy and waste-disposal projects. We propose an actuarial approach to mitigate this risk, first by defining an autonomous decision-making process based on an adaptive traffic light system (ATLS) to stop risky injections, and second by quantifying a "cost of public safety" based on the probability of an injection-well being abandoned. The ATLS underlying statistical model is first confirmed to be representative of injection-induced seismicity, with examples taken from past reservoir stimulation experiments (mostly from Enhanced Geothermal Systems, EGS). Then the decision strategy is formalized: Being integrable, the model yields a closed-form ATLS solution that maps a risk-based safety standard or norm to an earthquake magnitude not to exceed during stimulation. Finally, the EGS levelized cost of electricity (LCOE) is reformulated in terms of null expectation, with the cost of abandoned injection-well implemented. We find that the price increase to mitigate the increased seismic risk in populated areas can counterbalance the heat credit. However this "public safety cost" disappears if buildings are based on earthquake-resistant designs or if a more relaxed risk safety standard or norm is chosen. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.09635v1-abstract-full').style.display = 'none'; document.getElementById('1803.09635v1-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> 22 March, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 4 figures, conference (International Symposium on Energy Geotechnics, 26-28 September 2018, Lausanne, Switzerland)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Energy Geotechnics, A. Ferrari and L. Laloui (Eds.), SEG 2018, SSGG, pp. 369-376, 2019 </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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