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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.10969">arXiv:2303.10969</a> <span> [<a href="https://arxiv.org/pdf/2303.10969">pdf</a>, <a href="https://arxiv.org/format/2303.10969">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202345938">10.1051/0004-6361/202345938 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The 17 April 2021 widespread solar energetic particle event </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dresing%2C+N">N. Dresing</a>, <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez-Garc%C3%ADa%2C+L">L. Rodr铆guez-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Jebaraj%2C+I+C">I. C. Jebaraj</a>, <a href="/search/astro-ph?searchtype=author&query=Warmuth%2C+A">A. Warmuth</a>, <a href="/search/astro-ph?searchtype=author&query=Wallace%2C+S">S. Wallace</a>, <a href="/search/astro-ph?searchtype=author&query=Balmaceda%2C+L">L. Balmaceda</a>, <a href="/search/astro-ph?searchtype=author&query=Podladchikova%2C+T">T. Podladchikova</a>, <a href="/search/astro-ph?searchtype=author&query=Strauss%2C+R+D">R. D. Strauss</a>, <a href="/search/astro-ph?searchtype=author&query=Kouloumvakos%2C+A">A. Kouloumvakos</a>, <a href="/search/astro-ph?searchtype=author&query=Palmroos%2C+C">C. Palmroos</a>, <a href="/search/astro-ph?searchtype=author&query=Krupar%2C+V">V. Krupar</a>, <a href="/search/astro-ph?searchtype=author&query=Gieseler%2C+J">J. Gieseler</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+Z">Z. Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Mitchell%2C+J+G">J. G. Mitchell</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+C+M+S">C. M. S. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=de+Nolfo%2C+G+A">G. A. de Nolfo</a>, <a href="/search/astro-ph?searchtype=author&query=Palmerio%2C+E">E. Palmerio</a>, <a href="/search/astro-ph?searchtype=author&query=Carcaboso%2C+F">F. Carcaboso</a>, <a href="/search/astro-ph?searchtype=author&query=Kilpua%2C+E+K+J">E. K. J. Kilpua</a>, <a href="/search/astro-ph?searchtype=author&query=Trotta%2C+D">D. Trotta</a>, <a href="/search/astro-ph?searchtype=author&query=Auster%2C+U">U. Auster</a>, <a href="/search/astro-ph?searchtype=author&query=Asvestari%2C+E">E. Asvestari</a>, <a href="/search/astro-ph?searchtype=author&query=da+Silva%2C+D">D. da Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Dr%C3%B6ge%2C+W">W. Dr枚ge</a>, <a href="/search/astro-ph?searchtype=author&query=Getachew%2C+T">T. Getachew</a> , et al. (24 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.10969v1-abstract-short" style="display: inline;"> Context. A solar eruption on 17 April 2021 produced a widespread Solar Energetic Particle (SEP) event that was observed by five longitudinally well-separated observers in the inner heliosphere at heliocentric distances of 0.42 to 1 au: BepiColombo, Parker Solar Probe, Solar Orbiter, STEREO A, and near-Earth spacecraft. The event produced relativistic electrons and protons. It was associated with a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.10969v1-abstract-full').style.display = 'inline'; document.getElementById('2303.10969v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.10969v1-abstract-full" style="display: none;"> Context. A solar eruption on 17 April 2021 produced a widespread Solar Energetic Particle (SEP) event that was observed by five longitudinally well-separated observers in the inner heliosphere at heliocentric distances of 0.42 to 1 au: BepiColombo, Parker Solar Probe, Solar Orbiter, STEREO A, and near-Earth spacecraft. The event produced relativistic electrons and protons. It was associated with a long-lasting solar hard X-ray flare and a medium fast Coronal Mass Ejection (CME) with a speed of 880 km/s driving a shock, an EUV wave as well as long-lasting radio burst activity showing four distinct type III burst. Methods. A multi-spacecraft analysis of remote-sensing and in-situ observations is applied to attribute the SEP observations at the different locations to the various potential source regions at the Sun. An ENLIL simulation is used to characterize the interplanetary state and its role for the energetic particle transport. The magnetic connection between each spacecraft and the Sun is determined. Based on a reconstruction of the coronal shock front we determine the times when the shock establishes magnetic connections with the different observers. Radio observations are used to characterize the directivity of the four main injection episodes, which are then employed in a 2D SEP transport simulation. Results. Timing analysis of the inferred SEP solar injection suggests different source processes being important for the electron and the proton event. Comparison among the characteristics and timing of the potential particle sources, such as the CME-driven shock or the flare, suggests a stronger shock contribution for the proton event and a more likely flare-related source of the electron event. Conclusions. We find that in this event an important ingredient for the wide SEP spread was the wide longitudinal range of about 110 degrees covered by distinct SEP injections. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.10969v1-abstract-full').style.display = 'none'; document.getElementById('2303.10969v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A105 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.14832">arXiv:2302.14832</a> <span> [<a href="https://arxiv.org/pdf/2302.14832">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"> Planetary Exploration Horizon 2061 Report Chapter 5: Enabling technologies for planetary exploration </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Grande%2C+M">Manuel Grande</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+L">Linli Guo</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+M">Michel Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=Makaya%2C+A">Advenit Makaya</a>, <a href="/search/astro-ph?searchtype=author&query=Asmar%2C+S">Sami Asmar</a>, <a href="/search/astro-ph?searchtype=author&query=Atkinson%2C+D">David Atkinson</a>, <a href="/search/astro-ph?searchtype=author&query=Bourdon%2C+A">Anne Bourdon</a>, <a href="/search/astro-ph?searchtype=author&query=Chabert%2C+P">Pascal Chabert</a>, <a href="/search/astro-ph?searchtype=author&query=Chien%2C+S">Steve Chien</a>, <a href="/search/astro-ph?searchtype=author&query=Day%2C+J">John Day</a>, <a href="/search/astro-ph?searchtype=author&query=Fairen%2C+A+G">Alberto G. Fairen</a>, <a href="/search/astro-ph?searchtype=author&query=Freeman%2C+A">Anthony Freeman</a>, <a href="/search/astro-ph?searchtype=author&query=Genova%2C+A">Antonio Genova</a>, <a href="/search/astro-ph?searchtype=author&query=Herique%2C+A">Alain Herique</a>, <a href="/search/astro-ph?searchtype=author&query=Kofman%2C+W">Wlodek Kofman</a>, <a href="/search/astro-ph?searchtype=author&query=Lazio%2C+J">Joseph Lazio</a>, <a href="/search/astro-ph?searchtype=author&query=Mousis%2C+O">Olivier Mousis</a>, <a href="/search/astro-ph?searchtype=author&query=Ori%2C+G+G">Gian Gabriele Ori</a>, <a href="/search/astro-ph?searchtype=author&query=Parro%2C+V">Victor Parro</a>, <a href="/search/astro-ph?searchtype=author&query=Preston%2C+R">Robert Preston</a>, <a href="/search/astro-ph?searchtype=author&query=Rodriguez-Manfredi%2C+J+A">Jose A Rodriguez-Manfredi</a>, <a href="/search/astro-ph?searchtype=author&query=Sterken%2C+V">Veerle Sterken</a>, <a href="/search/astro-ph?searchtype=author&query=Stephenson%2C+K">Keith Stephenson</a>, <a href="/search/astro-ph?searchtype=author&query=Hook%2C+J+V">Joshua Vander Hook</a>, <a href="/search/astro-ph?searchtype=author&query=Waite%2C+H">Hunter Waite</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.14832v1-abstract-short" style="display: inline;"> The main objective of this chapter is to present an overview of the different areas of key technologies that will be needed to fly the technically most challenging of the representative missions identified in chapter 4 (the Pillar 2 Horizon 2061 report). It starts with a description of the future scientific instruments which will address the key questions of Horizon 2061 described in chapter 3 (th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.14832v1-abstract-full').style.display = 'inline'; document.getElementById('2302.14832v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.14832v1-abstract-full" style="display: none;"> The main objective of this chapter is to present an overview of the different areas of key technologies that will be needed to fly the technically most challenging of the representative missions identified in chapter 4 (the Pillar 2 Horizon 2061 report). It starts with a description of the future scientific instruments which will address the key questions of Horizon 2061 described in chapter 3 (the Pillar 1 Horizon 2061 report) and the new technologies that the next generations of space instruments will require (section 2). From there, the chapter follows the line of logical development and implementation of a planetary mission: section 3 describes some of the novel mission architectures that will be needed and how they will articulate interplanetary spacecraft and science platforms; section 4 summarizes the system-level technologies needed: power, propulsion, navigation, communication, advanced autonomy on board planetary spacecraft; section 5 describes the diversity of specialized science platforms that will be needed to survive, operate and return scientific data from the extreme environments that future missions will target; section 6 describes the new technology developments that will be needed for long-duration missions and semi-permanent settlements; finally, section 7 attempts to anticipate on the disruptive technologies that should emerge and progressively prevail in the decades to come to meet the long-term needs of future planetary missions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.14832v1-abstract-full').style.display = 'none'; document.getElementById('2302.14832v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">100 pages, 23 figures, Horizon 2061 is a science-driven, foresight exercise, for future scientific investigations</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.13243">arXiv:2202.13243</a> <span> [<a href="https://arxiv.org/pdf/2202.13243">pdf</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="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/10.1007/s11214-020-00712-8">10.1007/s11214-020-00712-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Investigating Mercury's Environment with the Two-Spacecraft BepiColombo Mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Milillo%2C+A">A. Milillo</a>, <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+M">M. Fujimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Murakami%2C+G">G. Murakami</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhoff%2C+J">J. Benkhoff</a>, <a href="/search/astro-ph?searchtype=author&query=Zender%2C+J">J. Zender</a>, <a href="/search/astro-ph?searchtype=author&query=Aizawa%2C+S">S. Aizawa</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%B3sa%2C+M">M. D贸sa</a>, <a href="/search/astro-ph?searchtype=author&query=Griton%2C+L">L. Griton</a>, <a href="/search/astro-ph?searchtype=author&query=Heyner%2C+D">D. Heyner</a>, <a href="/search/astro-ph?searchtype=author&query=Ho%2C+G">G. Ho</a>, <a href="/search/astro-ph?searchtype=author&query=Imber%2C+S+M">S. M. Imber</a>, <a href="/search/astro-ph?searchtype=author&query=Jia%2C+X">X. Jia</a>, <a href="/search/astro-ph?searchtype=author&query=Karlsson%2C+T">T. Karlsson</a>, <a href="/search/astro-ph?searchtype=author&query=Killen%2C+R+M">R. M. Killen</a>, <a href="/search/astro-ph?searchtype=author&query=Laurenza%2C+M">M. Laurenza</a>, <a href="/search/astro-ph?searchtype=author&query=Lindsay%2C+S+T">S. T. Lindsay</a>, <a href="/search/astro-ph?searchtype=author&query=McKenna-Lawlor%2C+S">S. McKenna-Lawlor</a>, <a href="/search/astro-ph?searchtype=author&query=Mura%2C+A">A. Mura</a>, <a href="/search/astro-ph?searchtype=author&query=Raines%2C+J+M">J. M. Raines</a>, <a href="/search/astro-ph?searchtype=author&query=Rothery%2C+D+A">D. A. Rothery</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+N">N. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/astro-ph?searchtype=author&query=Berezhnoy%2C+A">A. Berezhnoy</a>, <a href="/search/astro-ph?searchtype=author&query=Bourdin%2C+P+-">P. -A. Bourdin</a>, <a href="/search/astro-ph?searchtype=author&query=Bunce%2C+E+J">E. J. Bunce</a> , et al. (54 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2202.13243v1-abstract-short" style="display: inline;"> The ESA-JAXA BepiColombo mission will provide simultaneous measurements from two spacecraft, offering an unprecedented opportunity to investigate magnetospheric and exospheric dynamics at Mercury as well as their interactions with the solar wind, radiation, and interplanetary dust. Many scientific instruments onboard the two spacecraft will be completely, or partially devoted to study the near-spa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.13243v1-abstract-full').style.display = 'inline'; document.getElementById('2202.13243v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.13243v1-abstract-full" style="display: none;"> The ESA-JAXA BepiColombo mission will provide simultaneous measurements from two spacecraft, offering an unprecedented opportunity to investigate magnetospheric and exospheric dynamics at Mercury as well as their interactions with the solar wind, radiation, and interplanetary dust. Many scientific instruments onboard the two spacecraft will be completely, or partially devoted to study the near-space environment of Mercury as well as the complex processes that govern it. Many issues remain unsolved even after the MESSENGER mission that ended in 2015. The specific orbits of the two spacecraft, MPO and Mio, and the comprehensive scientific payload allow a wider range of scientific questions to be addressed than those that could be achieved by the individual instruments acting alone, or by previous missions. These joint observations are of key importance because many phenomena in Mercury's environment are highly temporally and spatially variable. Examples of possible coordinated observations are described in this article, analysing the required geometrical conditions, pointing, resolutions and operation timing of different BepiColombo instruments sensors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.13243v1-abstract-full').style.display = 'none'; document.getElementById('2202.13243v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">78 pages, 14 figures, published</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Space Science Reviews (2020), Volume 216, Issue 5, article id.93 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.01410">arXiv:2103.01410</a> <span> [<a href="https://arxiv.org/pdf/2103.01410">pdf</a>, <a href="https://arxiv.org/format/2103.01410">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> </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/10.1093/mnras/stab645">10.1093/mnras/stab645 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Implications of an improved water equation of state for water-rich planets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Huang%2C+C">Chenliang Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Rice%2C+D+R">David R. Rice</a>, <a href="/search/astro-ph?searchtype=author&query=Grande%2C+Z+M">Zachary M. Grande</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D">Dean Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+J+S">Jesse S. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Boisvert%2C+J+H">John H. Boisvert</a>, <a href="/search/astro-ph?searchtype=author&query=Tschauner%2C+O">Oliver Tschauner</a>, <a href="/search/astro-ph?searchtype=author&query=Salamat%2C+A">Ashkan Salamat</a>, <a href="/search/astro-ph?searchtype=author&query=Steffen%2C+J+H">Jason H. Steffen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2103.01410v1-abstract-short" style="display: inline;"> Water (H$_{2}$O), in all forms, is an important constituent in planetary bodies, controlling habitability and influencing geological activity. Under conditions found in the interior of many planets, as the pressure increases, the H-bonds in water gradually weaken and are replaced by ionic bonds. Recent experimental measurements of the water equation of state (EOS) showed both a new phase of H-bond… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.01410v1-abstract-full').style.display = 'inline'; document.getElementById('2103.01410v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.01410v1-abstract-full" style="display: none;"> Water (H$_{2}$O), in all forms, is an important constituent in planetary bodies, controlling habitability and influencing geological activity. Under conditions found in the interior of many planets, as the pressure increases, the H-bonds in water gradually weaken and are replaced by ionic bonds. Recent experimental measurements of the water equation of state (EOS) showed both a new phase of H-bonded water ice, ice-VII$_t$, and a relatively low transition pressure just above 30 GPa to ionic bonded ice-X, which has a bulk modulus 2.5 times larger. The higher bulk modulus of ice-X produces larger planets for a given mass, thereby either reducing the atmospheric contribution to the volume of many exoplanets or limiting their water content. We investigate the impact of the new EOS measurements on the planetary mass-radius relation and interior structure for water-rich planets. We find that the change in the planet mass-radius relation caused by the systematic differences between previous and new experimental EOS measurements are comparable to the observational uncertainties in some planet sizes -- an issue that will become more important as observations continue to improve. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.01410v1-abstract-full').style.display = 'none'; document.getElementById('2103.01410v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 4 figures. Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2003.06603">arXiv:2003.06603</a> <span> [<a href="https://arxiv.org/pdf/2003.06603">pdf</a>, <a href="https://arxiv.org/format/2003.06603">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> </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/10.3847/2041-8213/ab3ec2">10.3847/2041-8213/ab3ec2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The pivot energy of Solar Energetic Particles Affecting the Martian surface radiation environment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Guo%2C+J">Jingnan Guo</a>, <a href="/search/astro-ph?searchtype=author&query=Wimmer-Schweingruber%2C+R+F">Robert F. Wimmer-Schweingruber</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yuming Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Grande%2C+M">Manuel Grande</a>, <a href="/search/astro-ph?searchtype=author&query=Matthiae%2C+D">Daniel Matthiae</a>, <a href="/search/astro-ph?searchtype=author&query=Zeitlin%2C+C">Cary Zeitlin</a>, <a href="/search/astro-ph?searchtype=author&query=Ehresmann%2C+B">Bent Ehresmann</a>, <a href="/search/astro-ph?searchtype=author&query=Hassler%2C+D+M">Donald M. Hassler</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="2003.06603v1-abstract-short" style="display: inline;"> Space radiation is a major risk for humans, especially on long-duration missions to outer space, e.g., a manned mission to Mars. Galactic cosmic rays (GCR) contribute a predictable radiation background, the main risk is due to the highly variable and currently unpredictable flux of solar energetic particles (SEPs). Such sporadic SEP events may induce acute health effects and are thus considered a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.06603v1-abstract-full').style.display = 'inline'; document.getElementById('2003.06603v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.06603v1-abstract-full" style="display: none;"> Space radiation is a major risk for humans, especially on long-duration missions to outer space, e.g., a manned mission to Mars. Galactic cosmic rays (GCR) contribute a predictable radiation background, the main risk is due to the highly variable and currently unpredictable flux of solar energetic particles (SEPs). Such sporadic SEP events may induce acute health effects and are thus considered a critical mission risk for future human exploration of Mars. Therefore, it is of utmost importance to study, model, and predict the surface radiation environment during such events. It is well known that the deep-space SEP differential energy spectrum at high energies is often given by a power law. We use a measurement-validated particle transport code to show that, for large SEP events with proton energy extending above ~ 500 MeV with a power-law distribution, it is sufficient to measure the SEP flux at a pivot energy of ~ 300 MeV above the Martian atmosphere to predict the dose rate on the Martian surface. In conjunction with a validation by in-situ measurements from the Martian surface, this remarkable simplification and elegant quantification could enable instant predictions of the radiation environment on the surface of Mars upon the onset of large SEP events. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.06603v1-abstract-full').style.display = 'none'; document.getElementById('2003.06603v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Letters , 883, 1, L12 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.07731">arXiv:1908.07731</a> <span> [<a href="https://arxiv.org/pdf/1908.07731">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> </div> </div> <p class="title is-5 mathjax"> GAUSS -- A Sample Return Mission to Ceres </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shi%2C+X">Xian Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo-Rogez%2C+J">Julie Castillo-Rogez</a>, <a href="/search/astro-ph?searchtype=author&query=Hsieh%2C+H">Henry Hsieh</a>, <a href="/search/astro-ph?searchtype=author&query=Hui%2C+H">Hejiu Hui</a>, <a href="/search/astro-ph?searchtype=author&query=Ip%2C+W">Wing-Huen Ip</a>, <a href="/search/astro-ph?searchtype=author&query=Lei%2C+H">Hanlun Lei</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+J">Jian-Yang Li</a>, <a href="/search/astro-ph?searchtype=author&query=Tosi%2C+F">Federico Tosi</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+L">Liyong Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+J">Jessica Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Barucci%2C+A">Antonella Barucci</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+P">Pierre Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Bagatin%2C+A+C">Adriano Campo Bagatin</a>, <a href="/search/astro-ph?searchtype=author&query=Capaccioni%2C+F">Fabrizio Capaccioni</a>, <a href="/search/astro-ph?searchtype=author&query=Coates%2C+A">Andrew Coates</a>, <a href="/search/astro-ph?searchtype=author&query=Cremonese%2C+G">Gabriele Cremonese</a>, <a href="/search/astro-ph?searchtype=author&query=Duffard%2C+R">Rene Duffard</a>, <a href="/search/astro-ph?searchtype=author&query=Jaumann%2C+R">Ralf Jaumann</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+G">Geraint Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Grande%2C+M">Manuel Grande</a>, <a href="/search/astro-ph?searchtype=author&query=Kallio%2C+E">Esa Kallio</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+Y">Yangting Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Mousis%2C+O">Olivier Mousis</a>, <a href="/search/astro-ph?searchtype=author&query=Nathues%2C+A">Andreas Nathues</a>, <a href="/search/astro-ph?searchtype=author&query=Oberst%2C+J">J眉rgen Oberst</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1908.07731v2-abstract-short" style="display: inline;"> The goal of Project GAUSS is to return samples from the dwarf planet Ceres. Ceres is the most accessible ocean world candidate and the largest reservoir of water in the inner solar system. It shows active cryovolcanism and hydrothermal activities in recent history that resulted in minerals not found in any other planets to date except for Earth's upper crust. The possible occurrence of recent subs… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.07731v2-abstract-full').style.display = 'inline'; document.getElementById('1908.07731v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.07731v2-abstract-full" style="display: none;"> The goal of Project GAUSS is to return samples from the dwarf planet Ceres. Ceres is the most accessible ocean world candidate and the largest reservoir of water in the inner solar system. It shows active cryovolcanism and hydrothermal activities in recent history that resulted in minerals not found in any other planets to date except for Earth's upper crust. The possible occurrence of recent subsurface ocean on Ceres and the complex geochemistry suggest possible past habitability and even the potential for ongoing habitability. Aiming to answer a broad spectrum of questions about the origin and evolution of Ceres and its potential habitability, GAUSS will return samples from this possible ocean world for the first time. The project will address the following top-level scientific questions: 1) What is the origin of Ceres and the origin and transfer of water and other volatiles in the inner solar system? 2) What are the physical properties and internal structure of Ceres? What do they tell us about the evolutionary and aqueous alteration history of icy dwarf planets? 3) What are the astrobiological implications of Ceres? Was it habitable in the past and is it still today? 4) What are the mineralogical connections between Ceres and our current collections of primitive meteorites? GAUSS will first perform a high-resolution global remote sensing investigation, characterizing the geophysical and geochemical properties of Ceres. Candidate sampling sites will then be identified, and observation campaigns will be run for an in-depth assessment of the candidate sites. Once the sampling site is selected, a lander will be deployed on the surface to collect samples and return them to Earth in cryogenic conditions that preserves the volatile and organic composition as well as the original physical status as much as possible. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.07731v2-abstract-full').style.display = 'none'; document.getElementById('1908.07731v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Section 3.4 revised; List of team members updated; Typos corrected</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1906.11990">arXiv:1906.11990</a> <span> [<a href="https://arxiv.org/pdf/1906.11990">pdf</a>, <a href="https://arxiv.org/format/1906.11990">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Materials Science">cond-mat.mtrl-sci</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Bond strengthening in dense H2O and implications to planetary composition </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Grande%2C+Z+M">Zachary M. Grande</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+C">Chenliang Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D">Dean Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+J+S">Jesse S. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Boisvert%2C+J+H">John H. Boisvert</a>, <a href="/search/astro-ph?searchtype=author&query=Tschauner%2C+O">Oliver Tschauner</a>, <a href="/search/astro-ph?searchtype=author&query=Steffen%2C+J+H">Jason H. Steffen</a>, <a href="/search/astro-ph?searchtype=author&query=Salamat%2C+A">Ashkan Salamat</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="1906.11990v1-abstract-short" style="display: inline;"> H2O is an important constituent in planetary bodies, controlling habitability and, in geologically-active bodies, plate tectonics. At pressures within the interior of many planets, the H-bonds in H2O collapse into stronger, ionic bonds. Here we present agreement between X-ray diffraction and Raman spectroscopy for the transition from ice-VII to ice-X occurring at a pressure of approximately 30.9 G… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.11990v1-abstract-full').style.display = 'inline'; document.getElementById('1906.11990v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.11990v1-abstract-full" style="display: none;"> H2O is an important constituent in planetary bodies, controlling habitability and, in geologically-active bodies, plate tectonics. At pressures within the interior of many planets, the H-bonds in H2O collapse into stronger, ionic bonds. Here we present agreement between X-ray diffraction and Raman spectroscopy for the transition from ice-VII to ice-X occurring at a pressure of approximately 30.9 GPa by means of combining grain normalizing heat treatment via direct laser heating with static compression. This is evidenced by the emergence of the characteristic Raman mode of cuprite-like ice-X and an abrupt 2.5-fold increase in bulk modulus, implying a significant increase in bond strength. This is preceded by a transition from cubic ice-VII to a structure of tetragonal symmetry, ice-VIIt at 5.1 GPa. Our results significantly shift the mass/radius relationship of water-rich planets and define a high-pressure limit for release of chemically-bound water within the Earth, making the deep mantle a potential long-term reservoir of ancient water. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.11990v1-abstract-full').style.display = 'none'; document.getElementById('1906.11990v1-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 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1802.04772">arXiv:1802.04772</a> <span> [<a href="https://arxiv.org/pdf/1802.04772">pdf</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/10.1007/s12567-011-0014-x">10.1007/s12567-011-0014-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Cosmic Dust Analyzer onboard Cassini: ten years of discoveries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Srama%2C+R">Ralf Srama</a>, <a href="/search/astro-ph?searchtype=author&query=Kempf%2C+S">Sascha Kempf</a>, <a href="/search/astro-ph?searchtype=author&query=Moragas-Klostermeyer%2C+G">Georg Moragas-Klostermeyer</a>, <a href="/search/astro-ph?searchtype=author&query=Altobelli%2C+N">Nicolas Altobelli</a>, <a href="/search/astro-ph?searchtype=author&query=Auer%2C+S">Siegfried Auer</a>, <a href="/search/astro-ph?searchtype=author&query=Beckmann%2C+U">Uwe Beckmann</a>, <a href="/search/astro-ph?searchtype=author&query=Bugiel%2C+S">Sebastian Bugiel</a>, <a href="/search/astro-ph?searchtype=author&query=Burton%2C+M">Marcia Burton</a>, <a href="/search/astro-ph?searchtype=author&query=Economou%2C+T">Tom Economou</a>, <a href="/search/astro-ph?searchtype=author&query=Fechtig%2C+H">Hugo Fechtig</a>, <a href="/search/astro-ph?searchtype=author&query=Fiege%2C+K">Katherina Fiege</a>, <a href="/search/astro-ph?searchtype=author&query=Green%2C+S+F">Simon F. Green</a>, <a href="/search/astro-ph?searchtype=author&query=Grande%2C+M">Manuel Grande</a>, <a href="/search/astro-ph?searchtype=author&query=Havnes%2C+O">Ove Havnes</a>, <a href="/search/astro-ph?searchtype=author&query=Hillier%2C+J+K">Jon K. Hillier</a>, <a href="/search/astro-ph?searchtype=author&query=Helfert%2C+S">Stefan Helfert</a>, <a href="/search/astro-ph?searchtype=author&query=Horanyi%2C+M">Mihaly Horanyi</a>, <a href="/search/astro-ph?searchtype=author&query=Hsu%2C+S">Sean Hsu</a>, <a href="/search/astro-ph?searchtype=author&query=Igenbergs%2C+E">Eduard Igenbergs</a>, <a href="/search/astro-ph?searchtype=author&query=Jessberger%2C+E+K">E. K. Jessberger</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+T+V">Torrence V. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Khalisi%2C+E">Emil Khalisi</a>, <a href="/search/astro-ph?searchtype=author&query=Kr%C3%BCger%2C+H">Harald Kr眉ger</a>, <a href="/search/astro-ph?searchtype=author&query=Matt%2C+G">G眉nter Matt</a>, <a href="/search/astro-ph?searchtype=author&query=Mocker%2C+A">Anna Mocker</a> , et al. (16 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="1802.04772v1-abstract-short" style="display: inline;"> The interplanetary space probe Cassini/Huygens reached Saturn in July 2004 after seven years of cruise phase. The Cosmic Dust Analyzer (CDA) measures the interplanetary, interstellar and planetary dust in our solar system since 1999 and provided unique discoveries. In 1999, CDA detected interstellar dust in the inner solar system followed by the detection of electrical charges of interplanetary du… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.04772v1-abstract-full').style.display = 'inline'; document.getElementById('1802.04772v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.04772v1-abstract-full" style="display: none;"> The interplanetary space probe Cassini/Huygens reached Saturn in July 2004 after seven years of cruise phase. The Cosmic Dust Analyzer (CDA) measures the interplanetary, interstellar and planetary dust in our solar system since 1999 and provided unique discoveries. In 1999, CDA detected interstellar dust in the inner solar system followed by the detection of electrical charges of interplanetary dust grains during the cruise phase between Earth and Jupiter. The instrument determined the composition of interplanetary dust and the nanometre sized dust streams originating from Jupiter's moon Io. During the approach to Saturn in 2004, similar streams of submicron grains with speeds in the order of 100 km/s were detected from Saturn's inner and outer ring system and are released to the interplanetary magnetic field. Since 2004 CDA measured more than one million dust impacts characterizing the dust environment of Saturn. The instrument is one of three experiments which discovered the active ice geysers located at the south pole of Saturn's moon Enceladus in 2005. Later, a detailed compositional analysis of the water ice grains in Saturn's E ring system lead to the discovery of large reservoirs of liquid water (oceans) below the icy crust of Enceladus. Finally, the determination of the dust- magnetosphere interaction and the discovery of the extended E ring (at least twice as large as predicted) allowed the definition of a dynamical dust model of Saturn's E ring describing the observed properties. This paper summarizes the discoveries of a ten year story of success based on reliable measurements with the most advanced dust detector flown in space until today. This paper focuses on cruise results and findings achieved at Saturn with a focus on flux and density measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.04772v1-abstract-full').style.display = 'none'; document.getElementById('1802.04772v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 February, 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">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 12 Figures, DLRK 2011</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Srama, R., Kempf, S., Moragas-Klostermeyer, G. et al. CEAS Space J (2011) 2: 3. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1701.01354">arXiv:1701.01354</a> <span> [<a href="https://arxiv.org/pdf/1701.01354">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> </div> </div> <p class="title is-5 mathjax"> Virtual Planetary Space Weather Services offered by the Europlanet H2020 Research Infrastructure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+N">N. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Grande%2C+M">M. Grande</a>, <a href="/search/astro-ph?searchtype=author&query=Achilleos%2C+N">N. Achilleos</a>, <a href="/search/astro-ph?searchtype=author&query=Barth%C3%A9l%C3%A9my%2C+M">M. Barth茅l茅my</a>, <a href="/search/astro-ph?searchtype=author&query=Bouchemit%2C+M">M. Bouchemit</a>, <a href="/search/astro-ph?searchtype=author&query=Benson%2C+K">K. Benson</a>, <a href="/search/astro-ph?searchtype=author&query=Blelly%2C+P+-">P. -L. Blelly</a>, <a href="/search/astro-ph?searchtype=author&query=Budnik%2C+E">E. Budnik</a>, <a href="/search/astro-ph?searchtype=author&query=Caussarieu%2C+S">S. Caussarieu</a>, <a href="/search/astro-ph?searchtype=author&query=Cecconi%2C+B">B. Cecconi</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+T">T. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%A9not%2C+V">V. G茅not</a>, <a href="/search/astro-ph?searchtype=author&query=Guio%2C+P">P. Guio</a>, <a href="/search/astro-ph?searchtype=author&query=Goutenoir%2C+A">A. Goutenoir</a>, <a href="/search/astro-ph?searchtype=author&query=Grison%2C+B">B. Grison</a>, <a href="/search/astro-ph?searchtype=author&query=Hueso%2C+R">R. Hueso</a>, <a href="/search/astro-ph?searchtype=author&query=Indurain%2C+M">M. Indurain</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+G+H">G. H. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Lilensten%2C+J">J. Lilensten</a>, <a href="/search/astro-ph?searchtype=author&query=Marchaudon%2C+A">A. Marchaudon</a>, <a href="/search/astro-ph?searchtype=author&query=Matthi%C3%A4e%2C+D">D. Matthi盲e</a>, <a href="/search/astro-ph?searchtype=author&query=Opitz%2C+A">A. Opitz</a>, <a href="/search/astro-ph?searchtype=author&query=Rouillard%2C+A">A. Rouillard</a>, <a href="/search/astro-ph?searchtype=author&query=Stanislawska%2C+I">I. Stanislawska</a>, <a href="/search/astro-ph?searchtype=author&query=Soucek%2C+J">J. Soucek</a> , et al. (3 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="1701.01354v1-abstract-short" style="display: inline;"> The Europlanet 2020 Research Infrastructure will include new Planetary Space Weather Services (PSWS) that will extend the concepts of space weather and space situational awareness to other planets in our Solar System and in particular to spacecraft that voyage through it. PSWS will make five entirely new toolkits accessible to the research community and to industrial partners planning for space mi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.01354v1-abstract-full').style.display = 'inline'; document.getElementById('1701.01354v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1701.01354v1-abstract-full" style="display: none;"> The Europlanet 2020 Research Infrastructure will include new Planetary Space Weather Services (PSWS) that will extend the concepts of space weather and space situational awareness to other planets in our Solar System and in particular to spacecraft that voyage through it. PSWS will make five entirely new toolkits accessible to the research community and to industrial partners planning for space missions: a general planetary space weather toolkit, as well as three toolkits dedicated to the following key planetary environments: Mars, comets, and outer planets. This will give the European planetary science community new methods, interfaces, functionalities and/or plugins dedicated to planetary space weather in the tools and models available within the partner institutes. It will also create a novel event-diary toolkit aiming at predicting and detecting planetary events like meteor showers and impacts. A variety of tools are available for tracing propagation of planetary and/or solar events through the Solar System and modelling the response of the planetary environment (surfaces, atmospheres, ionospheres, and magnetospheres) to those events. But these tools were not originally designed for planetary event prediction and space weather applications. PSWS will provide the additional research and tailoring required to apply them for these purposes. PSWS will be to review, test, improve and adapt methods and tools available within the partner institutes in order to make prototype planetary event and space weather services operational in Europe at the end of the programme. To achieve its objectives PSWS will use a few tools and standards developed for the Astronomy Virtual Observatory (VO). This paper gives an overview of the project together with a few illustrations of prototype services based on VO standards and protocols. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.01354v1-abstract-full').style.display = 'none'; document.getElementById('1701.01354v1-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 January, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2017. </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">14 pages</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1503.06135">arXiv:1503.06135</a> <span> [<a href="https://arxiv.org/pdf/1503.06135">pdf</a>, <a href="https://arxiv.org/ps/1503.06135">ps</a>, <a href="https://arxiv.org/format/1503.06135">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/10.1016/j.asr.2015.03.023">10.1016/j.asr.2015.03.023 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Understanding space weather to shield society: A global road map for 2015-2025 commissioned by COSPAR and ILWS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Schrijver%2C+C+J">Carolus J. Schrijver</a>, <a href="/search/astro-ph?searchtype=author&query=Kauristie%2C+K">Kirsti Kauristie</a>, <a href="/search/astro-ph?searchtype=author&query=Aylward%2C+A+D">Alan D. Aylward</a>, <a href="/search/astro-ph?searchtype=author&query=Denardini%2C+C+M">Clezio M. Denardini</a>, <a href="/search/astro-ph?searchtype=author&query=Gibson%2C+S+E">Sarah E. Gibson</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+A">Alexi Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Gopalswamy%2C+N">Nat Gopalswamy</a>, <a href="/search/astro-ph?searchtype=author&query=Grande%2C+M">Manuel Grande</a>, <a href="/search/astro-ph?searchtype=author&query=Hapgood%2C+M">Mike Hapgood</a>, <a href="/search/astro-ph?searchtype=author&query=Heynderickx%2C+D">Daniel Heynderickx</a>, <a href="/search/astro-ph?searchtype=author&query=Jakowski%2C+N">Norbert Jakowski</a>, <a href="/search/astro-ph?searchtype=author&query=Kalegaev%2C+V+V">Vladimir V. Kalegaev</a>, <a href="/search/astro-ph?searchtype=author&query=Lapenta%2C+G">Giovanni Lapenta</a>, <a href="/search/astro-ph?searchtype=author&query=Linker%2C+J+A">Jon A. Linker</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+S">Siqing Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Mandrini%2C+C+H">Cristina H. Mandrini</a>, <a href="/search/astro-ph?searchtype=author&query=Mann%2C+I+R">Ian R. Mann</a>, <a href="/search/astro-ph?searchtype=author&query=Nagatsuma%2C+T">Tsutomu Nagatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Nandi%2C+D">Dibyendu Nandi</a>, <a href="/search/astro-ph?searchtype=author&query=Obara%2C+T">Takahiro Obara</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+T+P">T. Paul O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Onsager%2C+T">Terrance Onsager</a>, <a href="/search/astro-ph?searchtype=author&query=Opgenoorth%2C+H+J">Hermann J. Opgenoorth</a>, <a href="/search/astro-ph?searchtype=author&query=Terkildsen%2C+M">Michael Terkildsen</a>, <a href="/search/astro-ph?searchtype=author&query=Valladares%2C+C+E">Cesar E. Valladares</a> , et al. (1 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="1503.06135v1-abstract-short" style="display: inline;"> There is a growing appreciation that the environmental conditions that we call space weather impact the technological infrastructure that powers the coupled economies around the world. With that comes the need to better shield society against space weather by improving forecasts, environmental specifications, and infrastructure design. [...] advanced understanding of space weather requires a coord… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.06135v1-abstract-full').style.display = 'inline'; document.getElementById('1503.06135v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.06135v1-abstract-full" style="display: none;"> There is a growing appreciation that the environmental conditions that we call space weather impact the technological infrastructure that powers the coupled economies around the world. With that comes the need to better shield society against space weather by improving forecasts, environmental specifications, and infrastructure design. [...] advanced understanding of space weather requires a coordinated international approach to effectively provide awareness of the processes within the Sun-Earth system through observation-driven models. This roadmap prioritizes the scientific focus areas and research infrastructure that are needed to significantly advance our understanding of space weather of all intensities and of its implications for society. Advancement of the existing system observatory through the addition of small to moderate state-of-the-art capabilities designed to fill observational gaps will enable significant advances. Such a strategy requires urgent action: key instrumentation needs to be sustained, and action needs to be taken before core capabilities are lost in the aging ensemble. We recommend advances through priority focus (1) on observation-based modeling throughout the Sun-Earth system, (2) on forecasts more than 12 hrs ahead of the magnetic structure of incoming coronal mass ejections, (3) on understanding the geospace response to variable solar-wind stresses that lead to intense geomagnetically-induced currents and ionospheric and radiation storms, and (4) on developing a comprehensive specification of space climate, including the characterization of extreme space storms to guide resilient and robust engineering of technological infrastructures. The roadmap clusters its implementation recommendations by formulating three action pathways, and outlines needed instrumentation and research programs and infrastructure for each of these. [...] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.06135v1-abstract-full').style.display = 'none'; document.getElementById('1503.06135v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 March, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2015. </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">In press for Advances of Space Research: an international roadmap on the science of space weather, commissioned by COSPAR and ILWS (63 pages and 4 figures)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1207.3968">arXiv:1207.3968</a> <span> [<a href="https://arxiv.org/pdf/1207.3968">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </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/s11207-010-9599-z">10.1007/s11207-010-9599-z <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Transient Structures and Stream Interaction Regions in the Solar Wind: Results from EISCAT Interplanetary Scintillation, STEREO HI and Venus Express ASPERA-4 Measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dorrian%2C+G">Gareth Dorrian</a>, <a href="/search/astro-ph?searchtype=author&query=Breen%2C+A">Andy Breen</a>, <a href="/search/astro-ph?searchtype=author&query=Davies%2C+J">Jackie Davies</a>, <a href="/search/astro-ph?searchtype=author&query=Rouillard%2C+A">Alexi Rouillard</a>, <a href="/search/astro-ph?searchtype=author&query=Fallows%2C+R">Richard Fallows</a>, <a href="/search/astro-ph?searchtype=author&query=Whittaker%2C+I">Ian Whittaker</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+D">Daniel Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+R">Richard Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+C">Chris Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Grande%2C+M">Manuel Grande</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="1207.3968v1-abstract-short" style="display: inline;"> We discuss the detection and evolution of a complex series of transient and quasi-static solar wind structures in the days following the well-known comet 2P / Encke tail disconnection event in April 2007. The evolution of transient solar wind structures ranging in size from < 105 km to > 106 km was characterized using one-minute time resolution observation of Interplanetary Scintillation (IPS) mad… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.3968v1-abstract-full').style.display = 'inline'; document.getElementById('1207.3968v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1207.3968v1-abstract-full" style="display: none;"> We discuss the detection and evolution of a complex series of transient and quasi-static solar wind structures in the days following the well-known comet 2P / Encke tail disconnection event in April 2007. The evolution of transient solar wind structures ranging in size from < 105 km to > 106 km was characterized using one-minute time resolution observation of Interplanetary Scintillation (IPS) made using the European Incoherent SCA Tter (EISCA T) radar system. Simultaneously, the global structure and evolution of these features was characterized by the Heliospheric Imagers (HI) on the Solar TERrestrial RElations Observatory (STEREO) spacecraft, placing the IPS observations in context. Of particular interest was the observation of one transient in the slow wind apparently being swept up and entrained by a Stream Interaction Region (SIR). The SIR itself was later detected in-situ at Venus by the Analyser of Space Plasma and Energetic Atoms (ASPERA-4) instrument on the Venus Express (VEX) spacecraft. The availability of such diverse data sources over a range of different time resolutions enables us to develop a global picture of these complex events that would not have been possible if these instruments were used in isolation. We suggest that the range of solar wind transients discussed here maybe the interplanetary counterparts of transient structures previously reported from coronagraph observations and are likely to correspond to transient magnetic structures reported in in-situ measurements in interplanetary space. The results reported here also provide the first indication of heliocentric distances at which transients become entrained. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.3968v1-abstract-full').style.display = 'none'; document.getElementById('1207.3968v1-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 July, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">32 pages, 16 Figures, published in Solar Physics, 2010</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Solar Physics (2010), Volume 265, Issue 1-2, pp. 207-231 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0603507">arXiv:astro-ph/0603507</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0603507">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0603507">ps</a>, <a href="https://arxiv.org/format/astro-ph/0603507">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-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/10.1088/1742-6596/39/1/020">10.1088/1742-6596/39/1/020 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Indirect signatures for axion(-like) particles </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zioutas%2C+K">K. Zioutas</a>, <a href="/search/astro-ph?searchtype=author&query=Dennerl%2C+K">K. Dennerl</a>, <a href="/search/astro-ph?searchtype=author&query=Grande%2C+M">M. Grande</a>, <a href="/search/astro-ph?searchtype=author&query=Hoffmann%2C+D+H+H">D. H. H. Hoffmann</a>, <a href="/search/astro-ph?searchtype=author&query=Huovelin%2C+J">J. Huovelin</a>, <a href="/search/astro-ph?searchtype=author&query=Lakic%2C+B">B. Lakic</a>, <a href="/search/astro-ph?searchtype=author&query=Orlando%2C+S">S. Orlando</a>, <a href="/search/astro-ph?searchtype=author&query=Ortiz%2C+A">A. Ortiz</a>, <a href="/search/astro-ph?searchtype=author&query=Papaevangelou%2C+T">Th. Papaevangelou</a>, <a href="/search/astro-ph?searchtype=author&query=Semertzidis%2C+Y">Y. Semertzidis</a>, <a href="/search/astro-ph?searchtype=author&query=Tzamarias%2C+S">Sp. Tzamarias</a>, <a href="/search/astro-ph?searchtype=author&query=Vilhu%2C+O">O. Vilhu</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="astro-ph/0603507v1-abstract-short" style="display: inline;"> Magnetic field dependent transient solar observations are suggestive for axion-photon oscillations with light axion(-like) particle involvement. Novel dark-moon measurements with the SMART X-ray detectors can be conclusive for radiatively decaying massive exotica like the generic solar Kaluza-Klein axions. Furthermore, the predicted intrinsic strong solar magnetic fields could be the reason of e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0603507v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0603507v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0603507v1-abstract-full" style="display: none;"> Magnetic field dependent transient solar observations are suggestive for axion-photon oscillations with light axion(-like) particle involvement. Novel dark-moon measurements with the SMART X-ray detectors can be conclusive for radiatively decaying massive exotica like the generic solar Kaluza-Klein axions. Furthermore, the predicted intrinsic strong solar magnetic fields could be the reason of enhanced low energy axion production. Such an axion component could be the as yet unknown origin of the strong quiet Sun X-ray luminosity at energies below 1 keV. Solar axion telescopes should lower their threshold, aiming to copy processes that might occur near the solar surface, be it due to spontaneous or magnetically induced radiative decay of axion(-like) particles. This is motivated also by the recent claim of an axion-like particle detection by the laser experiment PVLAS. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0603507v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0603507v1-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 March, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2006. </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">9 pages, 2 Figures, TAUP2005 conf. proc. (extended version)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J.Phys.Conf.Ser. 39 (2006) 103-106 </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 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><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 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

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