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Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computational Physics">physics.comp-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-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/10.1038/s41550-021-01505-x">10.1038/s41550-021-01505-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Signatures of Strong Magnetization and Metal-Poor Atmosphere for a Neptune-Size Exoplanet </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Ben-Jaffel%2C+L">Lotfi Ben-Jaffel</a>, <a href="/search/physics?searchtype=author&query=Ballester%2C+G+E">Gilda E. Ballester</a>, <a href="/search/physics?searchtype=author&query=Mu%C3%B1oz%2C+A+G">Antonio Garc铆a Mu帽oz</a>, <a href="/search/physics?searchtype=author&query=Lavvas%2C+P">Panayotis Lavvas</a>, <a href="/search/physics?searchtype=author&query=Sing%2C+D+K">David K. Sing</a>, <a href="/search/physics?searchtype=author&query=Sanz-Forcada%2C+J">Jorge Sanz-Forcada</a>, <a href="/search/physics?searchtype=author&query=Cohen%2C+O">Ofer Cohen</a>, <a href="/search/physics?searchtype=author&query=Kataria%2C+T">Tiffany Kataria</a>, <a href="/search/physics?searchtype=author&query=Henry%2C+G+W">Gregory W. Henry</a>, <a href="/search/physics?searchtype=author&query=Buchhave%2C+L">Lars Buchhave</a>, <a href="/search/physics?searchtype=author&query=Mikal-Evans%2C+T">Thomas Mikal-Evans</a>, <a href="/search/physics?searchtype=author&query=Wakeford%2C+H+R">Hannah R. Wakeford</a>, <a href="/search/physics?searchtype=author&query=L%C3%B3pez-Morales%2C+M">Mercedes L贸pez-Morales</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="2211.05155v1-abstract-short" style="display: inline;"> The magnetosphere of an exoplanet has yet to be unambiguously detected. Investigations of star-planet interaction and neutral atomic hydrogen absorption during transit to detect magnetic fields in hot Jupiters have been inconclusive, and interpretations of the transit absorption non-unique. In contrast, ionized species escaping a magnetized exoplanet, particularly from the polar caps, should popul… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.05155v1-abstract-full').style.display = 'inline'; document.getElementById('2211.05155v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.05155v1-abstract-full" style="display: none;"> The magnetosphere of an exoplanet has yet to be unambiguously detected. Investigations of star-planet interaction and neutral atomic hydrogen absorption during transit to detect magnetic fields in hot Jupiters have been inconclusive, and interpretations of the transit absorption non-unique. In contrast, ionized species escaping a magnetized exoplanet, particularly from the polar caps, should populate the magnetosphere, allowing detection of different regions from the plasmasphere to the extended magnetotail, and characterization of the magnetic field producing them. Here, we report ultraviolet observations of HAT-P-11b, a low-mass (0.08 MJ) exoplanet showing strong, phase-extended transit absorption of neutral hydrogen (maximum and tail transit depths of 32 \pm 4%, 27 \pm 4%) and singly ionized carbon (15 \pm 4%, 12.5 \pm 4%). We show that the atmosphere should have less than six times the solar metallicity (at 200 bars), and the exoplanet must also have an extended magnetotail (1.8-3.1 AU). The HAT-P-11b equatorial magnetic field strength should be about 1-5 Gauss. Our panchromatic approach using ionized species to simultaneously derive metallicity and magnetic field strength can now constrain interior and dynamo models of exoplanets, with implications for formation and evolution scenarios. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.05155v1-abstract-full').style.display = 'none'; document.getElementById('2211.05155v1-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 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">68 pages, 12 figures. Published in Nature Astronomy on December 16 2021. Main draft and Supplementary information are included in a single file. Full-text access to a view-only version of the paper via : https://rdcu.be/cDlYv</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature Astronomy 6, 2022, 141 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.10261">arXiv:2204.10261</a> <span> [<a href="https://arxiv.org/pdf/2204.10261">pdf</a>, <a href="https://arxiv.org/format/2204.10261">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/10.1051/0004-6361/202243834">10.1051/0004-6361/202243834 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The HD 260655 system: Two rocky worlds transiting a bright M dwarf at 10 pc </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Luque%2C+R">R. Luque</a>, <a href="/search/physics?searchtype=author&query=Fulton%2C+B+J">B. J. Fulton</a>, <a href="/search/physics?searchtype=author&query=Kunimoto%2C+M">M. Kunimoto</a>, <a href="/search/physics?searchtype=author&query=Amado%2C+P+J">P. J. Amado</a>, <a href="/search/physics?searchtype=author&query=Gorrini%2C+P">P. Gorrini</a>, <a href="/search/physics?searchtype=author&query=Dreizler%2C+S">S. Dreizler</a>, <a href="/search/physics?searchtype=author&query=Hellier%2C+C">C. Hellier</a>, <a href="/search/physics?searchtype=author&query=Henry%2C+G+W">G. W. Henry</a>, <a href="/search/physics?searchtype=author&query=Molaverdikhani%2C+K">K. Molaverdikhani</a>, <a href="/search/physics?searchtype=author&query=Morello%2C+G">G. Morello</a>, <a href="/search/physics?searchtype=author&query=Pe%C3%B1a-Mo%C3%B1ino%2C+L">L. Pe帽a-Mo帽ino</a>, <a href="/search/physics?searchtype=author&query=P%C3%A9rez-Torres%2C+M">M. P茅rez-Torres</a>, <a href="/search/physics?searchtype=author&query=Pozuelos%2C+F+J">F. J. Pozuelos</a>, <a href="/search/physics?searchtype=author&query=Shan%2C+Y">Y. Shan</a>, <a href="/search/physics?searchtype=author&query=Anglada-Escud%C3%A9%2C+G">G. Anglada-Escud茅</a>, <a href="/search/physics?searchtype=author&query=B%C3%A9jar%2C+V+J+S">V. J. S. B茅jar</a>, <a href="/search/physics?searchtype=author&query=Bergond%2C+G">G. Bergond</a>, <a href="/search/physics?searchtype=author&query=Boyle%2C+A+W">A. W. Boyle</a>, <a href="/search/physics?searchtype=author&query=Caballero%2C+J+A">J. A. Caballero</a>, <a href="/search/physics?searchtype=author&query=Charbonneau%2C+D">D. Charbonneau</a>, <a href="/search/physics?searchtype=author&query=Ciardi%2C+D+R">D. R. Ciardi</a>, <a href="/search/physics?searchtype=author&query=Dufoer%2C+S">S. Dufoer</a>, <a href="/search/physics?searchtype=author&query=Espinoza%2C+N">N. Espinoza</a>, <a href="/search/physics?searchtype=author&query=Everett%2C+M">M. Everett</a>, <a href="/search/physics?searchtype=author&query=Fischer%2C+D">D. Fischer</a> , et al. (42 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="2204.10261v3-abstract-short" style="display: inline;"> We report the discovery of a multi-planetary system transiting the M0 V dwarf HD 260655 (GJ 239, TOI-4599). The system consists of at least two transiting planets, namely HD 260655 b, with a period of 2.77 d, a radius of R$_b$ = 1.240$\pm$0.023 R$_\oplus$, a mass of M$_b$ = 2.14$\pm$0.34 M$_\oplus$, and a bulk density of $蟻_b$ = 6.2$\pm$1.0 g cm$^{-3}$, and HD 260655 c, with a period of 5.71 d, a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.10261v3-abstract-full').style.display = 'inline'; document.getElementById('2204.10261v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.10261v3-abstract-full" style="display: none;"> We report the discovery of a multi-planetary system transiting the M0 V dwarf HD 260655 (GJ 239, TOI-4599). The system consists of at least two transiting planets, namely HD 260655 b, with a period of 2.77 d, a radius of R$_b$ = 1.240$\pm$0.023 R$_\oplus$, a mass of M$_b$ = 2.14$\pm$0.34 M$_\oplus$, and a bulk density of $蟻_b$ = 6.2$\pm$1.0 g cm$^{-3}$, and HD 260655 c, with a period of 5.71 d, a radius of R$_c$ = 1.533$^{+0.051}_{-0.046}$ R$_\oplus$, a mass of M$_c$ = 3.09$\pm$0.48 M$_\oplus$, and a bulk density of $蟻_c$ = 4.7$^{+0.9}_{-0.8}$ g cm$^{-3}$. The planets were detected in transit by the TESS mission and confirmed independently with archival and new precise radial velocities obtained with the HIRES and CARMENES instruments since 1998 and 2016, respectively. At a distance of 10 pc, HD 260655 becomes the fourth closest known multi-transiting planet system after HD 219134, LTT 1445 A, and AU Mic. Due to the apparent brightness of the host star (J = 6.7 mag), both planets are among the most suitable rocky worlds known today for atmospheric studies with the JWST, both in transmission and emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.10261v3-abstract-full').style.display = 'none'; document.getElementById('2204.10261v3-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 17 figures. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 664, A199 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.12126">arXiv:2105.12126</a> <span> [<a href="https://arxiv.org/pdf/2105.12126">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="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/10.1088/1674-4527/21/6/131">10.1088/1674-4527/21/6/131 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> How much has the Sun influenced Northern Hemisphere temperature trends? An ongoing debate </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Connolly%2C+R">Ronan Connolly</a>, <a href="/search/physics?searchtype=author&query=Soon%2C+W">Willie Soon</a>, <a href="/search/physics?searchtype=author&query=Connolly%2C+M">Michael Connolly</a>, <a href="/search/physics?searchtype=author&query=Baliunas%2C+S">Sallie Baliunas</a>, <a href="/search/physics?searchtype=author&query=Berglund%2C+J">Johan Berglund</a>, <a href="/search/physics?searchtype=author&query=Butler%2C+C+J">C. J. Butler</a>, <a href="/search/physics?searchtype=author&query=Cionco%2C+R+G">Rodolfo Gustavo Cionco</a>, <a href="/search/physics?searchtype=author&query=Elias%2C+A+G">Ana G. Elias</a>, <a href="/search/physics?searchtype=author&query=Fedorov%2C+V+M">Valery M. Fedorov</a>, <a href="/search/physics?searchtype=author&query=Harde%2C+H">Hermann Harde</a>, <a href="/search/physics?searchtype=author&query=Henry%2C+G+W">Gregory W. Henry</a>, <a href="/search/physics?searchtype=author&query=Hoyt%2C+D+V">Douglas V. Hoyt</a>, <a href="/search/physics?searchtype=author&query=Humlum%2C+O">Ole Humlum</a>, <a href="/search/physics?searchtype=author&query=Legates%2C+D+R">David R. Legates</a>, <a href="/search/physics?searchtype=author&query=L%C3%BCning%2C+S">Sebastian L眉ning</a>, <a href="/search/physics?searchtype=author&query=Scafetta%2C+N">Nicola Scafetta</a>, <a href="/search/physics?searchtype=author&query=Solheim%2C+J">Jan-Erik Solheim</a>, <a href="/search/physics?searchtype=author&query=Szarka%2C+L">L谩szl贸 Szarka</a>, <a href="/search/physics?searchtype=author&query=van+Loon%2C+H">Harry van Loon</a>, <a href="/search/physics?searchtype=author&query=Herrera%2C+V+M+V">V铆ctor M. Velasco Herrera</a>, <a href="/search/physics?searchtype=author&query=Willson%2C+R+C">Richard C. Willson</a>, <a href="/search/physics?searchtype=author&query=Yan%2C+H">Hong Yan</a>, <a href="/search/physics?searchtype=author&query=Zhang%2C+W">Weijia Zhang</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="2105.12126v1-abstract-short" style="display: inline;"> To evaluate the role of Total Solar Irradiance (TSI) on Northern Hemisphere (NH) surface air temperature trends it is important to have reliable estimates of both quantities. 16 different TSI estimates were compiled from the literature. 1/2 of these estimates are low variability and 1/2 are high variability. 5 largely-independent methods for estimating NH temperature trends were evaluated using: 1… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.12126v1-abstract-full').style.display = 'inline'; document.getElementById('2105.12126v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.12126v1-abstract-full" style="display: none;"> To evaluate the role of Total Solar Irradiance (TSI) on Northern Hemisphere (NH) surface air temperature trends it is important to have reliable estimates of both quantities. 16 different TSI estimates were compiled from the literature. 1/2 of these estimates are low variability and 1/2 are high variability. 5 largely-independent methods for estimating NH temperature trends were evaluated using: 1) only rural weather stations; 2) all available stations whether urban or rural (the standard approach); 3) only sea surface temperatures; 4) tree-ring temperature proxies; 5) glacier length temperature proxies. The standard estimates using urban as well as rural stations were anomalous as they implied a much greater warming in recent decades than the other estimates. This suggests urbanization bias might still be a problem in current global temperature datasets despite the conclusions of some earlier studies. Still, all 5 estimates confirm it is currently warmer than the late 19th century, i.e., there has been some global warming since 1850. For the 5 estimates of NH temperatures, the contribution from direct solar forcing for all 16 estimates of TSI was evaluated using simple linear least-squares fitting. The role of human activity in recent warming was then calculated by fitting the residuals to the UN IPCC's recommended anthropogenic forcings time series. For all 5 NH temperature series, different TSI estimates implied everything from recent global warming being mostly human-caused to it being mostly natural. It seems previous studies (including the most recent IPCC reports) that had prematurely concluded the former failed to adequately consider all the relevant estimates of TSI and/or to satisfactorily address the uncertainties still associated with NH temperature trend estimates. Several recommendations are provided on how future research could more satisfactorily resolve these issues. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.12126v1-abstract-full').style.display = 'none'; document.getElementById('2105.12126v1-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">71 pages, 18 figures. To be published in Research in Astronomy and Astrophysics</span> </p> </li> </ol> <div class="is-hidden-tablet"> <!-- feedback for mobile only --> <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"> <!-- MetaColumn 1 --> <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 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