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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/2404.04030">arXiv:2404.04030</a> <span> [<a href="https://arxiv.org/pdf/2404.04030">pdf</a>, <a href="https://arxiv.org/format/2404.04030">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/10.1051/0004-6361/202450253">10.1051/0004-6361/202450253 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Effect of magnetospheric conditions on the morphology of Jupiter's UV main auroral emission, as observed by Juno-UVS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Head%2C+L+A">L. A. Head</a>, <a href="/search/physics?searchtype=author&query=Grodent%2C+D">D. Grodent</a>, <a href="/search/physics?searchtype=author&query=Bonfond%2C+B">B. Bonfond</a>, <a href="/search/physics?searchtype=author&query=Moirano%2C+A">A. Moirano</a>, <a href="/search/physics?searchtype=author&query=Benmahi%2C+B">B. Benmahi</a>, <a href="/search/physics?searchtype=author&query=Sicorello%2C+G">G. Sicorello</a>, <a href="/search/physics?searchtype=author&query=G%C3%A9rard%2C+J">J-C G茅rard</a>, <a href="/search/physics?searchtype=author&query=Vogt%2C+M+F">M. F. Vogt</a>, <a href="/search/physics?searchtype=author&query=Hue%2C+V">V. Hue</a>, <a href="/search/physics?searchtype=author&query=Greathouse%2C+T">T. Greathouse</a>, <a href="/search/physics?searchtype=author&query=Gladstone%2C+G+R">G. R. Gladstone</a>, <a href="/search/physics?searchtype=author&query=Yao%2C+Z">Z. Yao</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="2404.04030v2-abstract-short" style="display: inline;"> Auroral emissions are a reflection of magnetospheric processes, and, at Jupiter, it is not entirely certain how the morphology of the UV main emission (ME) varies with magnetospheric compression or the strength of the central current sheet. This work leverages the observations from Juno-UVS to link ME variability with magnetospheric states. Novel arc-detection techniques are used to determine new… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.04030v2-abstract-full').style.display = 'inline'; document.getElementById('2404.04030v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.04030v2-abstract-full" style="display: none;"> Auroral emissions are a reflection of magnetospheric processes, and, at Jupiter, it is not entirely certain how the morphology of the UV main emission (ME) varies with magnetospheric compression or the strength of the central current sheet. This work leverages the observations from Juno-UVS to link ME variability with magnetospheric states. Novel arc-detection techniques are used to determine new reference ovals for the ME from perijoves 1 through 54, in both hemispheres, and analyse how the size and shape of the ME vary compared to this reference oval. The morphology and brightness of the ME vary in local time: the dawn-side ME is typically expanded and the dusk-side ME typically contracted compared to the reference oval, and the dusk-side ME being typically twice as bright as the dawn-side ME. Both the northern and southern ME, and the day-side and night-side ME, expand and contract from their reference ovals synchronously, which indicates that the variable size of the ME is caused by a process occurring throughout the jovian magnetosphere. The poleward latitudinal shift of the auroral footprint of Ganymede correlates with the poleward motion of the ME, whereas a similar relation is not present for the footprint of Io. Additionally, the expansion of the ME correlates well with an increase in magnetodisc current. These two results suggest that a changing current-sheet magnetic field is partially responsible for the variable size of the ME. Finally, magnetospheric compression is linked to a global ME contraction and brightening, though this brightening occurs predominantly in the day-side ME. This observation, and the observation that the dusk-side ME is typically brighter than the dawn-side ME, stands in contrast to the modelled and observed behaviour of field-aligned currents and thus weakens the theoretical link between field-aligned currents and the generation of the auroral ME. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.04030v2-abstract-full').style.display = 'none'; document.getElementById('2404.04030v2-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 688, A205 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.04043">arXiv:2303.04043</a> <span> [<a href="https://arxiv.org/pdf/2303.04043">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> Catalog of Ultraviolet Bright Stars (CUBS): Strategies for UV occultation measurements, planetary illumination modeling, and sky map analyses using hybrid IUE-Kurucz spectra </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Velez%2C+M+A">M. A. Velez</a>, <a href="/search/physics?searchtype=author&query=Retherford%2C+K+D">K. D. Retherford</a>, <a href="/search/physics?searchtype=author&query=Hue%2C+V">V. Hue</a>, <a href="/search/physics?searchtype=author&query=Kammer%2C+J+A">J. A. Kammer</a>, <a href="/search/physics?searchtype=author&query=Becker%2C+T+M">T. M. Becker</a>, <a href="/search/physics?searchtype=author&query=Gladstone%2C+G+R">G. R. Gladstone</a>, <a href="/search/physics?searchtype=author&query=Davis%2C+M+W">M. W. Davis</a>, <a href="/search/physics?searchtype=author&query=Greathouse%2C+T+K">T. K. Greathouse</a>, <a href="/search/physics?searchtype=author&query=Molyneux%2C+P+M">P. M. Molyneux</a>, <a href="/search/physics?searchtype=author&query=Brooks%2C+S+M">S. M. Brooks</a>, <a href="/search/physics?searchtype=author&query=Raut%2C+U">U. Raut</a>, <a href="/search/physics?searchtype=author&query=Versteeg%2C+M+H">M. H. Versteeg</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.04043v1-abstract-short" style="display: inline;"> Ultraviolet spectroscopy is a powerful method to study planetary surface composition through reflectance measurements and atmospheric composition through stellar/solar occultations, transits of other planetary bodies, and direct imaging of airglow and auroral emissions. The next generation of ultraviolet spectrographs (UVS) on board ESA's JUICE (Jupiter Icy Moons Explorer) and NASA's Europa Clippe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.04043v1-abstract-full').style.display = 'inline'; document.getElementById('2303.04043v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.04043v1-abstract-full" style="display: none;"> Ultraviolet spectroscopy is a powerful method to study planetary surface composition through reflectance measurements and atmospheric composition through stellar/solar occultations, transits of other planetary bodies, and direct imaging of airglow and auroral emissions. The next generation of ultraviolet spectrographs (UVS) on board ESA's JUICE (Jupiter Icy Moons Explorer) and NASA's Europa Clipper missions will perform such measurements of Jupiter and its moons in the early 2030's. This work presents a compilation of a detailed UV stellar catalog, named CUBS, of targets with high intensity in the 50-210 nm wavelength range with applications relevant to planetary spectroscopy. These applications include: 1) Planning and simulating occultations, including calibration measurements; 2) Modeling starlight illumination of dark, nightside planetary surfaces primarily lit by the sky; and 3) Studying the origin of diffuse galactic UV light as mapped by existing datasets from Juno-UVS and others. CUBS includes information drawn from resources such as the International Ultraviolet Explorer (IUE) catalog and SIMBAD. We have constructed model spectra at 0.1 nm resolution for almost 90,000 targets using Kurucz models and, when available, IUE spectra. CUBS also includes robust checks for agreement between the Kurucz models and the IUE data. We also present a tool for which our catalog can be used to identify the best candidates for stellar occultation observations, with applications for any UV instrument. We report on our methods for producing CUBS and discuss plans for its implementation during ongoing and upcoming planetary missions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.04043v1-abstract-full').style.display = 'none'; document.getElementById('2303.04043v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 4 figures, submitted to JATIS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.10946">arXiv:2302.10946</a> <span> [<a href="https://arxiv.org/pdf/2302.10946">pdf</a>, <a href="https://arxiv.org/format/2302.10946">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/10.1029/2022JE007610">10.1029/2022JE007610 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Enhanced C$_2$H$_2$ absorption within Jupiter's southern auroral oval from Juno UVS observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Giles%2C+R+S">Rohini S. Giles</a>, <a href="/search/physics?searchtype=author&query=Hue%2C+V">Vincent Hue</a>, <a href="/search/physics?searchtype=author&query=Greathouse%2C+T+K">Thomas K. Greathouse</a>, <a href="/search/physics?searchtype=author&query=Gladstone%2C+G+R">G. Randall Gladstone</a>, <a href="/search/physics?searchtype=author&query=Kammer%2C+J+A">Joshua A. Kammer</a>, <a href="/search/physics?searchtype=author&query=Versteeg%2C+M+H">Maarten H. Versteeg</a>, <a href="/search/physics?searchtype=author&query=Bonfond%2C+B">Bertrand Bonfond</a>, <a href="/search/physics?searchtype=author&query=Grodent%2C+D+G">Denis G. Grodent</a>, <a href="/search/physics?searchtype=author&query=G%C3%A9rard%2C+J">Jean-Claude G茅rard</a>, <a href="/search/physics?searchtype=author&query=Sinclair%2C+J+A">James A. Sinclair</a>, <a href="/search/physics?searchtype=author&query=Bolton%2C+S+J">Scott J. Bolton</a>, <a href="/search/physics?searchtype=author&query=Levin%2C+S+M">Steven M. Levin</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.10946v1-abstract-short" style="display: inline;"> Reflected sunlight observations from the Ultraviolet Spectrograph (UVS) on the Juno spacecraft were used to study the distribution of acetylene (C$_2$H$_2$) at Jupiter's south pole. We find that the shape of the C$_2$H$_2$ absorption feature varies significantly across the polar region, and this can be used to infer spatial variability in the C$_2$H$_2$ abundance. There is a localized region of en… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.10946v1-abstract-full').style.display = 'inline'; document.getElementById('2302.10946v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.10946v1-abstract-full" style="display: none;"> Reflected sunlight observations from the Ultraviolet Spectrograph (UVS) on the Juno spacecraft were used to study the distribution of acetylene (C$_2$H$_2$) at Jupiter's south pole. We find that the shape of the C$_2$H$_2$ absorption feature varies significantly across the polar region, and this can be used to infer spatial variability in the C$_2$H$_2$ abundance. There is a localized region of enhanced C$_2$H$_2$ absorption which coincides with the location of Jupiter's southern polar aurora; the C$_2$H$_2$ abundance poleward of the auroral oval is a factor of 3 higher than adjacent quiescent, non-auroral longitudes. This builds on previous infrared studies which found enhanced C$_2$H$_2$ abundances within the northern auroral oval. This suggests that Jupiter's upper-atmosphere chemistry is being strongly influenced by the influx of charged auroral particles and demonstrates the necessity of developing ion-neutral photochemical models of Jupiter's polar regions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.10946v1-abstract-full').style.display = 'none'; document.getElementById('2302.10946v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in JGR: Planets</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.14712">arXiv:2107.14712</a> <span> [<a href="https://arxiv.org/pdf/2107.14712">pdf</a>, <a href="https://arxiv.org/format/2107.14712">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/10.1093/mnras/stab2218">10.1093/mnras/stab2218 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Jupiter's X-ray aurora during UV dawn storms and injections as observed by XMM-Newton, Hubble, and Hisaki </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Wibisono%2C+A+D">A. D. Wibisono</a>, <a href="/search/physics?searchtype=author&query=Branduardi-Raymont%2C+G">G. Branduardi-Raymont</a>, <a href="/search/physics?searchtype=author&query=Dunn%2C+W+R">W. R. Dunn</a>, <a href="/search/physics?searchtype=author&query=Kimura%2C+T">T. Kimura</a>, <a href="/search/physics?searchtype=author&query=Coates%2C+A+J">A. J. Coates</a>, <a href="/search/physics?searchtype=author&query=Grodent%2C+D">D. Grodent</a>, <a href="/search/physics?searchtype=author&query=Yao%2C+Z+H">Z. H. Yao</a>, <a href="/search/physics?searchtype=author&query=Kita%2C+H">H. Kita</a>, <a href="/search/physics?searchtype=author&query=Rodriguez%2C+P">P. Rodriguez</a>, <a href="/search/physics?searchtype=author&query=Gladstone%2C+G+R">G. R. Gladstone</a>, <a href="/search/physics?searchtype=author&query=Bonfond%2C+B">B. Bonfond</a>, <a href="/search/physics?searchtype=author&query=Haythornthwaite%2C+R+P">R. P. Haythornthwaite</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.14712v1-abstract-short" style="display: inline;"> We present results from a multiwavelength observation of Jupiter's northern aurorae, carried out simultaneously by XMM-Newton, the Hubble Space Telescope (HST), and the Hisaki satellite in September 2019. HST images captured dawn storms and injection events in the far ultraviolet aurora several times during the observation period. Magnetic reconnection occurring in the middle magnetosphere caused… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.14712v1-abstract-full').style.display = 'inline'; document.getElementById('2107.14712v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.14712v1-abstract-full" style="display: none;"> We present results from a multiwavelength observation of Jupiter's northern aurorae, carried out simultaneously by XMM-Newton, the Hubble Space Telescope (HST), and the Hisaki satellite in September 2019. HST images captured dawn storms and injection events in the far ultraviolet aurora several times during the observation period. Magnetic reconnection occurring in the middle magnetosphere caused by internal drivers is thought to start the production of those features. The field lines then dipolarize which injects hot magnetospheric plasma from the reconnection site to enter the inner magnetosphere. Hisaki observed an impulsive brightening in the dawnside Io plasma torus (IPT) during the final appearance of the dawn storms and injection events which is evidence that a large-scale plasma injection penetrated the central IPT between 6-9 RJ (Jupiter radii). The extreme ultraviolet aurora brightened and XMM-Newton detected an increase in the hard X-ray aurora count rate, suggesting an increase in electron precipitation. The dawn storms and injections did not change the brightness of the soft X-ray aurora and they did not "switch-on" its commonly observed quasi-periodic pulsations. Spectral analysis of the X-ray aurora suggests that the precipitating ions responsible for the soft X-ray aurora were iogenic and that a powerlaw continuum was needed to fit the hard X-ray part of the spectra. The spectra coincident with the dawn storms and injections required two powerlaw continua to get good fits. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.14712v1-abstract-full').style.display = 'none'; document.getElementById('2107.14712v1-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 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 7 figures in main text, 6 figures in the appendices. Accepted in MNRAS 28 July 2021</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.05045">arXiv:2106.05045</a> <span> [<a href="https://arxiv.org/pdf/2106.05045">pdf</a>, <a href="https://arxiv.org/format/2106.05045">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/10.1093/mnras/stab1680">10.1093/mnras/stab1680 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searching for Saturn's X-rays during a rare Jupiter Magnetotail Crossing using Chandra </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Weigt%2C+D+M">D. M. Weigt</a>, <a href="/search/physics?searchtype=author&query=Dunn%2C+W+R">W. R. Dunn</a>, <a href="/search/physics?searchtype=author&query=Jackman%2C+C+M">C. M. Jackman</a>, <a href="/search/physics?searchtype=author&query=Kraft%2C+R">R. Kraft</a>, <a href="/search/physics?searchtype=author&query=Branduardi-Raymont%2C+G">G. Branduardi-Raymont</a>, <a href="/search/physics?searchtype=author&query=Nichols%2C+J+D">J. D. Nichols</a>, <a href="/search/physics?searchtype=author&query=Wibisono%2C+A+D">A. D. Wibisono</a>, <a href="/search/physics?searchtype=author&query=Vogt%2C+M+F">M. F. Vogt</a>, <a href="/search/physics?searchtype=author&query=Gladstone%2C+G+R">G. R. Gladstone</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="2106.05045v1-abstract-short" style="display: inline;"> Every 19 years, Saturn passes through Jupiter's 'flapping' magnetotail. Here, we report Chandra X-ray observations of Saturn planned to coincide with this rare planetary alignment and to analyse Saturn's magnetospheric response when transitioning to this unique parameter space. We analyse three Director's Discretionary Time (DDT) observations from the High Resolution Camera (HRC-I) on-board Chandr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.05045v1-abstract-full').style.display = 'inline'; document.getElementById('2106.05045v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.05045v1-abstract-full" style="display: none;"> Every 19 years, Saturn passes through Jupiter's 'flapping' magnetotail. Here, we report Chandra X-ray observations of Saturn planned to coincide with this rare planetary alignment and to analyse Saturn's magnetospheric response when transitioning to this unique parameter space. We analyse three Director's Discretionary Time (DDT) observations from the High Resolution Camera (HRC-I) on-board Chandra, taken on November 19, 21 and 23 2020 with the aim to find auroral and/or disk emissions. We infer the conditions in the kronian system by looking at coincident soft X-ray solar flux data from the Geostationary Operational Environmental Satellite (GOES) and Hubble Space Telescope (HST) observations of Saturn's ultraviolet (UV) auroral emissions. The large Saturn-Sun-Earth angle during this time would mean that most flares from the Earth-facing side of the Sun would not have impacted Saturn. We find no significant detection of Saturn's disk or auroral emissions in any of our observations. We calculate the 3$蟽$ upper band energy flux of Saturn during this time to be 0.9 - 3.04 $\times$ 10$^{14}$ erg cm$^{-2}$ s$^{-1}$ which agrees with fluxes found from previous modelled spectra of the disk emissions. We conclude by discussing the implications of this non-detection and how it is imperative that the next fleet of X-ray telescope (such as Athena and the Lynx mission concept) continue to observe Saturn with their improved spatial and spectral resolution and very enhanced sensitivity to help us finally solve the mysteries behind Saturn's apparently elusive X-ray aurora. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.05045v1-abstract-full').style.display = 'none'; document.getElementById('2106.05045v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 3 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/2106.03570">arXiv:2106.03570</a> <span> [<a href="https://arxiv.org/pdf/2106.03570">pdf</a>, <a href="https://arxiv.org/format/2106.03570">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/s41550-021-01426-9">10.1038/s41550-021-01426-9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A sublimated water atmosphere on Ganymede detected from Hubble Space Telescope observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Roth%2C+L">Lorenz Roth</a>, <a href="/search/physics?searchtype=author&query=Ivchenko%2C+N">Nickolay Ivchenko</a>, <a href="/search/physics?searchtype=author&query=Gladstone%2C+G+R">G. Randall Gladstone</a>, <a href="/search/physics?searchtype=author&query=Saur%2C+J">Joachim Saur</a>, <a href="/search/physics?searchtype=author&query=Grodent%2C+D">Denis Grodent</a>, <a href="/search/physics?searchtype=author&query=Bonfond%2C+B">Bertrand Bonfond</a>, <a href="/search/physics?searchtype=author&query=Molyneux%2C+P+M">Philippa M. Molyneux</a>, <a href="/search/physics?searchtype=author&query=Retherford%2C+K+D">Kurt D. Retherford</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="2106.03570v2-abstract-short" style="display: inline;"> Ganymede's atmosphere is produced by charged particle sputtering and sublimation of its icy surface. Previous far-ultraviolet observations of the O{\small I\,}1356-脜 and O{\small I\,}1304-脜 oxygen emissions were used to infer sputtered molecular oxygen (O$_2$) as an atmospheric constituent, but an expected sublimated water (H$_2$O) component remained undetected. Here we present an analysis of high… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.03570v2-abstract-full').style.display = 'inline'; document.getElementById('2106.03570v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.03570v2-abstract-full" style="display: none;"> Ganymede's atmosphere is produced by charged particle sputtering and sublimation of its icy surface. Previous far-ultraviolet observations of the O{\small I\,}1356-脜 and O{\small I\,}1304-脜 oxygen emissions were used to infer sputtered molecular oxygen (O$_2$) as an atmospheric constituent, but an expected sublimated water (H$_2$O) component remained undetected. Here we present an analysis of high-sensitivity spectra and spectral images acquired by the Hubble Space Telescope revealing H$_2$O in Ganymede's atmosphere. The relative intensity of the oxygen emissions requires contributions from dissociative excitation of water vapor, indicating that H$_2$O is more abundant than O$_2$ around the sub-solar point. Away from the sub-solar region, the emissions are consistent with a pure O$_2$ atmosphere. Eclipse observations constrain atomic oxygen to be at least two orders of magnitude less abundant than these other species. The higher H$_2$O/O$_2$ ratio above the warmer trailing hemisphere compared to the colder leading hemisphere, the spatial concentration to the sub-solar region, and the estimated abundance of $\sim$10$^{15}$ H$_2$O/cm$^{2}$ are consistent with sublimation of the icy surface as source. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.03570v2-abstract-full').style.display = 'none'; document.getElementById('2106.03570v2-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 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">published in Nature Astronomy (2021) (reformatted for arXiv)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.01035">arXiv:2104.01035</a> <span> [<a href="https://arxiv.org/pdf/2104.01035">pdf</a>, <a href="https://arxiv.org/format/2104.01035">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/10.1051/0004-6361/202141783">10.1051/0004-6361/202141783 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A molecular wind blows out of the Kuiper belt </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Kral%2C+Q">Quentin Kral</a>, <a href="/search/physics?searchtype=author&query=Pringle%2C+J+E">J. E. Pringle</a>, <a href="/search/physics?searchtype=author&query=Guilbert-Lepoutre%2C+A">Aur茅lie Guilbert-Lepoutre</a>, <a href="/search/physics?searchtype=author&query=Matr%C3%A0%2C+L">Luca Matr脿</a>, <a href="/search/physics?searchtype=author&query=Moses%2C+J+I">Julianne I. Moses</a>, <a href="/search/physics?searchtype=author&query=Lellouch%2C+E">Emmanuel Lellouch</a>, <a href="/search/physics?searchtype=author&query=Wyatt%2C+M+C">Mark C. Wyatt</a>, <a href="/search/physics?searchtype=author&query=Biver%2C+N">Nicolas Biver</a>, <a href="/search/physics?searchtype=author&query=Bockel%C3%A9e-Morvan%2C+D">Dominique Bockel茅e-Morvan</a>, <a href="/search/physics?searchtype=author&query=Bonsor%2C+A">Amy Bonsor</a>, <a href="/search/physics?searchtype=author&query=Petit%2C+F+L">Franck Le Petit</a>, <a href="/search/physics?searchtype=author&query=Gladstone%2C+G+R">G. Randall Gladstone</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="2104.01035v2-abstract-short" style="display: inline;"> Gas has been detected in many exoplanetary systems ($>$10 Myr), thought to be released in the destruction of volatile-rich planetesimals orbiting in exo-Kuiper belts. In this letter, we aim to explore whether gas is also expected in the Kuiper belt (KB) in our Solar System. To quantify the gas release in our Solar System, we use models for gas release that have been applied to extrasolar planetary… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.01035v2-abstract-full').style.display = 'inline'; document.getElementById('2104.01035v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.01035v2-abstract-full" style="display: none;"> Gas has been detected in many exoplanetary systems ($>$10 Myr), thought to be released in the destruction of volatile-rich planetesimals orbiting in exo-Kuiper belts. In this letter, we aim to explore whether gas is also expected in the Kuiper belt (KB) in our Solar System. To quantify the gas release in our Solar System, we use models for gas release that have been applied to extrasolar planetary systems, as well as a physical model that accounts for gas released due to the progressive internal warming of large planetesimals. We find that only bodies larger than about 4 km can still contain CO ice after 4.6 Gyr of evolution. This finding may provide a clue as to why Jupiter-family comets, thought to originate in the Kuiper belt, are deficient in CO compared to Oort-clouds comets. We predict that gas is still produced in the KB right now at a rate of $2 \times 10^{-8}$ M$_\oplus$/Myr for CO and orders of magnitude more when the Sun was younger. Once released, the gas is quickly pushed out by the Solar wind. Therefore, we predict a gas wind in our Solar System starting at the KB location and extending far beyond with regards to the heliosphere with a current total CO mass of $\sim 2 \times 10^{-12}$ M$_\oplus$. We also predict the existence of a slightly more massive atomic gas wind made of carbon and oxygen (neutral and ionized) with a mass of $\sim 10^{-11}$ M$_\oplus$. We predict that gas is currently present in our Solar System beyond the Kuiper belt and that although it cannot be detected with current instrumentation, it could be observed in the future with an in situ mission using an instrument similar to Alice on New Horizons with larger detectors. Our model of gas release due to slow heating may also work for exoplanetary systems and provide the first real physical mechanism for the gas observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.01035v2-abstract-full').style.display = 'none'; document.getElementById('2104.01035v2-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 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication as a Letter to the editor in A&A; abstract shortened; 15 pages, 5 figures, 4 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 653, L11 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.12208">arXiv:2103.12208</a> <span> [<a href="https://arxiv.org/pdf/2103.12208">pdf</a>, <a href="https://arxiv.org/format/2103.12208">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="Atmospheric and Oceanic Physics">physics.ao-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202140330">10.1051/0004-6361/202140330 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First direct measurement of auroral and equatorial jets in the stratosphere of Jupiter </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Cavali%C3%A9%2C+T">T. Cavali茅</a>, <a href="/search/physics?searchtype=author&query=Benmahi%2C+B">B. Benmahi</a>, <a href="/search/physics?searchtype=author&query=Hue%2C+V">V. Hue</a>, <a href="/search/physics?searchtype=author&query=Moreno%2C+R">R. Moreno</a>, <a href="/search/physics?searchtype=author&query=Lellouch%2C+E">E. Lellouch</a>, <a href="/search/physics?searchtype=author&query=Fouchet%2C+T">T. Fouchet</a>, <a href="/search/physics?searchtype=author&query=Hartogh%2C+P">P. Hartogh</a>, <a href="/search/physics?searchtype=author&query=Rezac%2C+L">L. Rezac</a>, <a href="/search/physics?searchtype=author&query=Greathouse%2C+T+K">T. K. Greathouse</a>, <a href="/search/physics?searchtype=author&query=Gladstone%2C+G+R">G. R. Gladstone</a>, <a href="/search/physics?searchtype=author&query=Sinclair%2C+J+A">J. A. Sinclair</a>, <a href="/search/physics?searchtype=author&query=Dobrijevic%2C+M">M. Dobrijevic</a>, <a href="/search/physics?searchtype=author&query=Billebaud%2C+F">F. Billebaud</a>, <a href="/search/physics?searchtype=author&query=Jarchow%2C+C">C. Jarchow</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="2103.12208v1-abstract-short" style="display: inline;"> Context. The tropospheric wind pattern in Jupiter consists of alternating prograde and retrograde zonal jets with typical velocities of up to 100 m/s around the equator. At much higher altitudes, in the ionosphere, strong auroral jets have been discovered with velocities of 1-2 km/s. There is no such direct measurement in the stratosphere of the planet. Aims. In this paper, we bridge the altitude… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.12208v1-abstract-full').style.display = 'inline'; document.getElementById('2103.12208v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.12208v1-abstract-full" style="display: none;"> Context. The tropospheric wind pattern in Jupiter consists of alternating prograde and retrograde zonal jets with typical velocities of up to 100 m/s around the equator. At much higher altitudes, in the ionosphere, strong auroral jets have been discovered with velocities of 1-2 km/s. There is no such direct measurement in the stratosphere of the planet. Aims. In this paper, we bridge the altitude gap between these measurements by directly measuring the wind speeds in Jupiter's stratosphere. Methods. We use the Atacama Large Millimeter/submillimeter Array's very high spectral and angular resolution imaging of the stratosphere of Jupiter to retrieve the wind speeds as a function of latitude by fitting the Doppler shifts induced by the winds on the spectral lines. Results. We detect for the first time equatorial zonal jets that reside at 1 mbar, i.e. above the altitudes where Jupiter's Quasi-Quadrennial Oscillation occurs. Most noticeably, we find 300-400 m/s non-zonal winds at 0.1 mbar over the polar regions underneath the main auroral ovals. They are in counter-rotation and lie several hundreds of kilometers below the ionospheric auroral winds. We suspect them to be the lower tail of the ionospheric auroral winds. Conclusions. We detect directly and for the first time strong winds in Jupiter's stratosphere. They are zonal at low-to-mid latitudes and non-zonal at polar latitudes. The wind system found at polar latitudes may help increase the effciency of chemical complexification by confining the photochemical products in a region of large energetic electron precipitation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.12208v1-abstract-full').style.display = 'none'; document.getElementById('2103.12208v1-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, 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">7 pages and 3 figures (+ 5 pages and 5 figures for the appendix). Published in A&A 647, L8</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astronomy and Astrophysics, Volume 647, L8 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1301.3797">arXiv:1301.3797</a> <span> [<a href="https://arxiv.org/pdf/1301.3797">pdf</a>, <a href="https://arxiv.org/ps/1301.3797">ps</a>, <a href="https://arxiv.org/format/1301.3797">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="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/10.1029/2012JA017869">10.1029/2012JA017869 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MeV electrons detected by the Alice UV spectrograph during the New Horizons flyby of Jupiter </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Steffl%2C+A+J">A. J. Steffl</a>, <a href="/search/physics?searchtype=author&query=Shinn%2C+A+B">A. B. Shinn</a>, <a href="/search/physics?searchtype=author&query=Gladstone%2C+G+R">G. R. Gladstone</a>, <a href="/search/physics?searchtype=author&query=Parker%2C+J+W">J. Wm. Parker</a>, <a href="/search/physics?searchtype=author&query=Retherford%2C+K+D">K. D. Retherford</a>, <a href="/search/physics?searchtype=author&query=Slater%2C+D+C">D. C. Slater</a>, <a href="/search/physics?searchtype=author&query=Versteeg%2C+M+H">M. H. Versteeg</a>, <a href="/search/physics?searchtype=author&query=Stern%2C+S+A">S. A. Stern</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="1301.3797v1-abstract-short" style="display: inline;"> In early 2007, the New Horizons spacecraft flew through the Jovian magnetosphere on the dusk side. Here, we present results from a novel means of detecting energetic electrons along New Horizons' trajectory: the background count rate of the Alice ultraviolet spectrograph. Electrons with energies >1 MeV can penetrate the thin aluminum housing of Alice, interact with the microchannel plate detector,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1301.3797v1-abstract-full').style.display = 'inline'; document.getElementById('1301.3797v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1301.3797v1-abstract-full" style="display: none;"> In early 2007, the New Horizons spacecraft flew through the Jovian magnetosphere on the dusk side. Here, we present results from a novel means of detecting energetic electrons along New Horizons' trajectory: the background count rate of the Alice ultraviolet spectrograph. Electrons with energies >1 MeV can penetrate the thin aluminum housing of Alice, interact with the microchannel plate detector, and produce a count that is indistinguishable from an FUV photon. We present Alice data, proportional to the MeV electron flux, from an 11-day period centered on the spacecraft's closest approach to Jupiter, and compare it to electron data from the PEPSSI instrument. We find that a solar wind compression event passed over the spacecraft just prior to it entering the Jovian magnetosphere. Subsequently, the magnetopause boundary was detected at a distance of 67 R_J suggesting a compressed magnetospheric configuration. Three days later, when the spacecraft was 35-90 R_J downstream of Jupiter, New Horizons observed a series of 15 current sheet crossings, all of which occurred significantly northward of model predictions implying solar wind influence over the middle and outer Jovian magnetosphere, even to radial distances as small as ~35 R_J. In addition, we find the Jovian current sheet, which had a half-thickness of at least 7.4 R_J between 1930 and 2100 LT abruptly thinned to a thickness of ~3.4 R_J around 2200 LT. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1301.3797v1-abstract-full').style.display = 'none'; document.getElementById('1301.3797v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 January, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">39 pages, 8 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Geophysical Research (Space Physics), 2012, vol 117, pp. A10222 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1012.1088">arXiv:1012.1088</a> <span> [<a href="https://arxiv.org/pdf/1012.1088">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.pss.2006.11.009">10.1016/j.pss.2006.11.009 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> X-rays from solar system objects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bhardwaj%2C+A">Anil Bhardwaj</a>, <a href="/search/physics?searchtype=author&query=Elsner%2C+R+F">Ronald F. Elsner</a>, <a href="/search/physics?searchtype=author&query=Gladstone%2C+G+R">G. Randall Gladstone</a>, <a href="/search/physics?searchtype=author&query=Cravens%2C+T+E">Thomas E. Cravens</a>, <a href="/search/physics?searchtype=author&query=Lisse%2C+C+M">Carey M. Lisse</a>, <a href="/search/physics?searchtype=author&query=Dennerl%2C+K">Konrad Dennerl</a>, <a href="/search/physics?searchtype=author&query=Branduardi-Raymont%2C+G">Graziella Branduardi-Raymont</a>, <a href="/search/physics?searchtype=author&query=Wargelin%2C+B+J">Bradford J. Wargelin</a>, <a href="/search/physics?searchtype=author&query=Waite%2C+J+H">J. Hunter Waite</a>, <a href="/search/physics?searchtype=author&query=Robertson%2C+I">Ina Robertson</a>, <a href="/search/physics?searchtype=author&query=Ostgaard%2C+N">Nikolai Ostgaard</a>, <a href="/search/physics?searchtype=author&query=Beiersdorfer%2C+P">Peter Beiersdorfer</a>, <a href="/search/physics?searchtype=author&query=Snowden%2C+S+L">Steven L. Snowden</a>, <a href="/search/physics?searchtype=author&query=Kharchenko%2C+V">Vasili Kharchenko</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="1012.1088v1-abstract-short" style="display: inline;"> During the last few years our knowledge about the X-ray emission from bodies within the solar system has significantly improved. Several new solar system objects are now known to shine in X-rays at energies below 2 keV. Apart from the Sun, the known X-ray emitters now include planets (Venus, Earth, Mars, Jupiter, and Saturn), planetary satellites (Moon, Io, Europa, and Ganymede), all active comets… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1012.1088v1-abstract-full').style.display = 'inline'; document.getElementById('1012.1088v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1012.1088v1-abstract-full" style="display: none;"> During the last few years our knowledge about the X-ray emission from bodies within the solar system has significantly improved. Several new solar system objects are now known to shine in X-rays at energies below 2 keV. Apart from the Sun, the known X-ray emitters now include planets (Venus, Earth, Mars, Jupiter, and Saturn), planetary satellites (Moon, Io, Europa, and Ganymede), all active comets, the Io plasma torus (IPT), the rings of Saturn, the coronae (exospheres) of Earth and Mars, and the heliosphere. The advent of higher-resolution X-ray spectroscopy with the Chandra and XMM-Newton X-ray observatories has been of great benefit in advancing the field of planetary X-ray astronomy. Progress in modeling X-ray emission, laboratory studies of X-ray production, and theoretical calculations of cross-sections, have all contributed to our understanding of processes that produce X-rays from the solar system bodies. At Jupiter and Earth, both auroral and non-auroral disk X-ray emissions have been observed. X-rays have been detected from Saturn's disk, but no convincing evidence of an X-ray aurora has been observed. The first soft (0.1- 2 keV) X-ray observation of Earth's aurora by Chandra shows that it is highly variable. The non-auroral X-ray emissions from Jupiter, Saturn, and Earth, those from the disk of Mars, Venus, and Moon, and from the rings of Saturn, are mainly produced by scattering of solar X-rays. The spectral characteristics of X-ray emission from comets, the heliosphere, the geocorona, and the Martian halo are quite similar, but they appear to be quite different from those of Jovian auroral X-rays. X-rays from the Galilean satellites and the IPT are mostly driven by impact of Jovian magnetospheric particles. This paper reviews studies of the soft X-ray emission from the solar system bodies, excluding the Sun. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1012.1088v1-abstract-full').style.display = 'none'; document.getElementById('1012.1088v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 December, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Planetary and Space Science, Volume 55, Issue 9, p. 1135-1189 (2007) </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 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