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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/2502.09186">arXiv:2502.09186</a> <span> [<a href="https://arxiv.org/pdf/2502.09186">pdf</a>, <a href="https://arxiv.org/format/2502.09186">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> </div> </div> <p class="title is-5 mathjax"> New Models of Jupiter's Magnetopause and Bow Shock through the $Juno$ Prime Mission: Probabilistic Location, Shape, and Internally-driven Variation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Rutala%2C+M+J">M. J. Rutala</a>, <a href="/search/physics?searchtype=author&query=Jackman%2C+C+M">C. M. Jackman</a>, <a href="/search/physics?searchtype=author&query=Louis%2C+C+K">C. K. Louis</a>, <a href="/search/physics?searchtype=author&query=Azari%2C+A+R">A. R. Azari</a>, <a href="/search/physics?searchtype=author&query=Bagenal%2C+F">F. Bagenal</a>, <a href="/search/physics?searchtype=author&query=Joy%2C+S+P">S. P. Joy</a>, <a href="/search/physics?searchtype=author&query=Kurth%2C+W+S">W. S. Kurth</a>, <a href="/search/physics?searchtype=author&query=Keebler%2C+T+B">T. B. Keebler</a>, <a href="/search/physics?searchtype=author&query=Giles%2C+R+S">R. S. Giles</a>, <a href="/search/physics?searchtype=author&query=Ebert%2C+R+W">R. W. Ebert</a>, <a href="/search/physics?searchtype=author&query=Bowers%2C+C+F">C. F. Bowers</a>, <a href="/search/physics?searchtype=author&query=Vogt%2C+M+F">M. F. Vogt</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="2502.09186v1-abstract-short" style="display: inline;"> The interaction between Jupiter's magnetosphere and the solar wind is not well-constrained: while internal energetic plasma processes are thought to dominate plasma circulation, the solar wind nonetheless exerts significant control over the shape and scale of the whole structure. To better constrain this interaction, we derive new functional forms for Jupiter's magnetopause and bow shock using dat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.09186v1-abstract-full').style.display = 'inline'; document.getElementById('2502.09186v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.09186v1-abstract-full" style="display: none;"> The interaction between Jupiter's magnetosphere and the solar wind is not well-constrained: while internal energetic plasma processes are thought to dominate plasma circulation, the solar wind nonetheless exerts significant control over the shape and scale of the whole structure. To better constrain this interaction, we derive new functional forms for Jupiter's magnetopause and bow shock using data from the $Ulysses$, $Galileo$, $Cassini$, and $Juno$ missions and calibrated solar wind estimates from the Multi-Model Ensemble System for the Heliosphere (MMESH). We design an empirical Bayesian model to estimate the locations of the boundaries using a Markov-chain Monte Carlo (MCMC) algorithm, expanding our model to sample all times, not only boundary crossing events. The boundary surfaces which best describe the data are thus estimated without the need for a full, physics-based magnetohydrodynamic (MHD) treatment of the Jovian magnetosphere and the additional assumptions required for such. The new magnetopause model exhibits significant polar flattening and dawn-dusk asymmetry, and includes a narrowing of the magnetotail when compared to previous models. The new bow shock model is largely axisymmetric. Both boundary models describe surfaces which lie closer to Jupiter than previous models, which has important implications for the modern picture of Jupiter's dynamic magnetosphere and the expected science results of current and upcoming Jupiter-bound spacecraft. Applying these models to $Juno$'s trajectory, we estimate that the spacecraft should be expected to spend ${\sim}19\%$ of each orbit in the magnetosheath and ${\sim}4\%$ of each orbit in the solar wind starting from Perijove 64 (PJ64, 21 July 2021). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.09186v1-abstract-full').style.display = 'none'; document.getElementById('2502.09186v1-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, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </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">34 pages, 11 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/2410.17304">arXiv:2410.17304</a> <span> [<a href="https://arxiv.org/pdf/2410.17304">pdf</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> </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/10.1029/2024GL113193">10.1029/2024GL113193 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Corotation-bounce resonance of ions in Jupiter's magnetosphere </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Sarkango%2C+Y">Y. Sarkango</a>, <a href="/search/physics?searchtype=author&query=Szalay%2C+J+R">J. R. Szalay</a>, <a href="/search/physics?searchtype=author&query=Damiano%2C+P+A">P. A. Damiano</a>, <a href="/search/physics?searchtype=author&query=Sulaiman%2C+A+H">A. H. Sulaiman</a>, <a href="/search/physics?searchtype=author&query=Delamere%2C+P+A">P. A. Delamere</a>, <a href="/search/physics?searchtype=author&query=Saur%2C+J">J. Saur</a>, <a href="/search/physics?searchtype=author&query=McComas%2C+D+J">D. J. McComas</a>, <a href="/search/physics?searchtype=author&query=Ebert%2C+R+W">R. W. Ebert</a>, <a href="/search/physics?searchtype=author&query=Allegrini%2C+F">F. Allegrini</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="2410.17304v2-abstract-short" style="display: inline;"> Banded energy distributions of H$^{+}$, O$^{++}$, S$^{+++}$, and O$^+$ or S$^{++}$ ions between 100 eV to ~20 keV are consistently observed in Jupiter's magnetosphere mapping to M-shells between M=10-20. The bands correspond to flux enhancements at similar speeds for different ion species, providing the first evidence of simultaneous bounce-resonant acceleration of multiple ion species in Jupiter'… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.17304v2-abstract-full').style.display = 'inline'; document.getElementById('2410.17304v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.17304v2-abstract-full" style="display: none;"> Banded energy distributions of H$^{+}$, O$^{++}$, S$^{+++}$, and O$^+$ or S$^{++}$ ions between 100 eV to ~20 keV are consistently observed in Jupiter's magnetosphere mapping to M-shells between M=10-20. The bands correspond to flux enhancements at similar speeds for different ion species, providing the first evidence of simultaneous bounce-resonant acceleration of multiple ion species in Jupiter's magnetosphere. Ion enhancements occur for energies at which the bounce frequencies of the trapped ions matched integer harmonics of the System-III corotation frequency. The observations highlight a previously unknown interaction between corotation and bounce motion of <10 keV energy ions that is a fundamental and persistent process occurring in Jupiter's magnetosphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.17304v2-abstract-full').style.display = 'none'; document.getElementById('2410.17304v2-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> 23 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.01993">arXiv:2404.01993</a> <span> [<a href="https://arxiv.org/pdf/2404.01993">pdf</a>, <a href="https://arxiv.org/format/2404.01993">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="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="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> <p class="title is-5 mathjax"> CME Deflection and East-West Asymmetry of ESP Intensity in Solar Cycles 23 and 24 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Due%C3%B1as%2C+A+S+F">Adolfo Santa Fe Due帽as</a>, <a href="/search/physics?searchtype=author&query=Ebert%2C+R+W">Robert W. Ebert</a>, <a href="/search/physics?searchtype=author&query=Li%2C+G">Gang Li</a>, <a href="/search/physics?searchtype=author&query=Ding%2C+Z">Zheyi Ding</a>, <a href="/search/physics?searchtype=author&query=Dayeh%2C+M+A">Maher A. Dayeh</a>, <a href="/search/physics?searchtype=author&query=Desai%2C+M+I">Mihir I. Desai</a>, <a href="/search/physics?searchtype=author&query=Jian%2C+L+K">Lan K. Jian</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="2404.01993v1-abstract-short" style="display: inline;"> We investigate the East-West asymmetry in energetic storm particle (ESP) heavy ion intensities at interplanetary shocks driven by coronal mass ejections (CMEs) during solar cycles (SCs) 23 and 24. We use observations from NASA's ACE and STEREO missions of helium (He), oxygen (O), and iron (Fe) intensities from ~0.13 to 3 MeV/nucleon. We examine the longitudinal distribution of ESP intensities and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.01993v1-abstract-full').style.display = 'inline'; document.getElementById('2404.01993v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.01993v1-abstract-full" style="display: none;"> We investigate the East-West asymmetry in energetic storm particle (ESP) heavy ion intensities at interplanetary shocks driven by coronal mass ejections (CMEs) during solar cycles (SCs) 23 and 24. We use observations from NASA's ACE and STEREO missions of helium (He), oxygen (O), and iron (Fe) intensities from ~0.13 to 3 MeV/nucleon. We examine the longitudinal distribution of ESP intensities and the correlation of ESP intensities with the near-Sun CME speed and the average transit CME speed for eastern and western events. We observed an East-West asymmetry reversal of ESP heavy ion intensities from SC 23 to 24. We have determined that this change in asymmetry is caused by a shift in the heliolongitude distribution of the CME speed ratio (the ratio of CME near-Sun speed to CME average transit speed) from west to east. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.01993v1-abstract-full').style.display = 'none'; document.getElementById('2404.01993v1-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> 2 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.02458">arXiv:2307.02458</a> <span> [<a href="https://arxiv.org/pdf/2307.02458">pdf</a>, <a href="https://arxiv.org/format/2307.02458">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="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/10.1029/2023JA031502">10.1029/2023JA031502 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The East-West Asymmetry of Particle Intensity in Energetic Storm Particle Events </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Ding%2C+Z">Zheyi Ding</a>, <a href="/search/physics?searchtype=author&query=Li%2C+G">Gang Li</a>, <a href="/search/physics?searchtype=author&query=Due%C3%B1as%2C+A+S+F">Adolfo Santa Fe Due帽as</a>, <a href="/search/physics?searchtype=author&query=Ebert%2C+R+W">Robert W. Ebert</a>, <a href="/search/physics?searchtype=author&query=Wijsen%2C+N">Nicolas Wijsen</a>, <a href="/search/physics?searchtype=author&query=Poedts%2C+S">Stefaan Poedts</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="2307.02458v1-abstract-short" style="display: inline;"> We examine the East-West asymmetry of the peak intensity in energetic storm particle (ESP) events using the improved Particle Acceleration and Transport in the Heliosphere (iPATH) model. We find that injection efficiency peaks east of the nose of coronal mass ejection shock where the shock exhibits a quasi-parallel geometry. We show that the peak intensity at the eastern flank is generally larger… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.02458v1-abstract-full').style.display = 'inline'; document.getElementById('2307.02458v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.02458v1-abstract-full" style="display: none;"> We examine the East-West asymmetry of the peak intensity in energetic storm particle (ESP) events using the improved Particle Acceleration and Transport in the Heliosphere (iPATH) model. We find that injection efficiency peaks east of the nose of coronal mass ejection shock where the shock exhibits a quasi-parallel geometry. We show that the peak intensity at the eastern flank is generally larger than that at the western flank and it positively correlates with the injection efficiency. We also examine this asymmetry for heavy ions, which depends sensitively on the ion energy. Comparison between the modelling results with the measurements of ESP events at 1 au shows a reasonable agreement. We suggest that the injection efficiency can be a primary factor leading to the East-West asymmetry of the peak intensity in ESP events. Additionally, the charge-to-mass (Q/A) dependence of the maximum particle energy affects this asymmetry for heavy ions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.02458v1-abstract-full').style.display = 'none'; document.getElementById('2307.02458v1-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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 for publication in JGR: space physics. 19 pages, 8 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/2301.03731">arXiv:2301.03731</a> <span> [<a href="https://arxiv.org/pdf/2301.03731">pdf</a>, <a href="https://arxiv.org/format/2301.03731">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="Plasma Physics">physics.plasm-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/10.1029/2022JA031280">10.1029/2022JA031280 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Force-free current sheets in the Jovian magnetodisk: the key role of electron field-aligned anisotropy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Artemyev%2C+A+V">A. V. Artemyev</a>, <a href="/search/physics?searchtype=author&query=Ma%2C+Q">Q. Ma</a>, <a href="/search/physics?searchtype=author&query=Ebert%2C+R+W">R. W. Ebert</a>, <a href="/search/physics?searchtype=author&query=Zhang%2C+X+-">X. -J. Zhang</a>, <a href="/search/physics?searchtype=author&query=Allegrini%2C+F">F. Allegrini</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="2301.03731v1-abstract-short" style="display: inline;"> Current sheets are an essential element of the planetary magnetotails, where strong plasma currents self-consistently support magnetic field gradients. The current sheet configuration is determined by plasma populations that contribute to the current density. The most commonly investigated configuration is supported by diamagnetic cross-field currents of hot ions, typical for the magnetospheres of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.03731v1-abstract-full').style.display = 'inline'; document.getElementById('2301.03731v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.03731v1-abstract-full" style="display: none;"> Current sheets are an essential element of the planetary magnetotails, where strong plasma currents self-consistently support magnetic field gradients. The current sheet configuration is determined by plasma populations that contribute to the current density. The most commonly investigated configuration is supported by diamagnetic cross-field currents of hot ions, typical for the magnetospheres of magnetized planets. In this study, we examine a new type of the current sheet configuration supported by field-aligned currents from electron streams in the Jovian magnetodisk. Such bi-directional streams increase the electron thermal anisotropy close to the fire-hose instability threshold and lead to strong magnetic field shear. The current sheet configuration supported by electron streams is nearly force-free, with B=const across the sheet. Using Juno plasma and magnetic field measurements, we investigate the internal structure of such current sheets and discuss possible mechanisms for their formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.03731v1-abstract-full').style.display = 'none'; document.getElementById('2301.03731v1-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 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.03740">arXiv:2212.03740</a> <span> [<a href="https://arxiv.org/pdf/2212.03740">pdf</a>, <a href="https://arxiv.org/format/2212.03740">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/10.1029/2022JA031155">10.1029/2022JA031155 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Effect of a magnetosphere compression on Jovian radio emissions: in situ case study using Juno data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Louis%2C+C+K">C. K. Louis</a>, <a href="/search/physics?searchtype=author&query=Jackman%2C+C+M">C. M. Jackman</a>, <a href="/search/physics?searchtype=author&query=Hospodarsky%2C+G">G. Hospodarsky</a>, <a href="/search/physics?searchtype=author&query=Hackett%2C+A+O">A. O'Kane Hackett</a>, <a href="/search/physics?searchtype=author&query=Devon-Hurley%2C+E">E. Devon-Hurley</a>, <a href="/search/physics?searchtype=author&query=Zarka%2C+P">P. Zarka</a>, <a href="/search/physics?searchtype=author&query=Kurth%2C+W+S">W. S. Kurth</a>, <a href="/search/physics?searchtype=author&query=Ebert%2C+R+W">R. W. Ebert</a>, <a href="/search/physics?searchtype=author&query=Weigt%2C+D+M">D. M. Weigt</a>, <a href="/search/physics?searchtype=author&query=Fogg%2C+A+R">A. R. Fogg</a>, <a href="/search/physics?searchtype=author&query=Waters%2C+J+E">J. E. Waters</a>, <a href="/search/physics?searchtype=author&query=Entee%2C+S+M">S. Mc Entee</a>, <a href="/search/physics?searchtype=author&query=Connerney%2C+J+E+P">J. E. P. Connerney</a>, <a href="/search/physics?searchtype=author&query=Louarn%2C+P">P. Louarn</a>, <a href="/search/physics?searchtype=author&query=Levin%2C+S">S. Levin</a>, <a href="/search/physics?searchtype=author&query=Bolton%2C+S+J">S. J. Bolton</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="2212.03740v2-abstract-short" style="display: inline;"> During its 53-day polar orbit around Jupiter, Juno often crosses the boundaries of the Jovian magnetosphere (namely the magnetopause and bow shock). From the boundary locations, the upstream solar wind dynamic pressure can be inferred, which in turn illustrates the state of compression or relaxation of the system. The aim of this study is to examine Jovian radio emissions during magnetospheric com… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.03740v2-abstract-full').style.display = 'inline'; document.getElementById('2212.03740v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.03740v2-abstract-full" style="display: none;"> During its 53-day polar orbit around Jupiter, Juno often crosses the boundaries of the Jovian magnetosphere (namely the magnetopause and bow shock). From the boundary locations, the upstream solar wind dynamic pressure can be inferred, which in turn illustrates the state of compression or relaxation of the system. The aim of this study is to examine Jovian radio emissions during magnetospheric compressions, in order to determine the relationship between the solar wind and Jovian radio emissions. In this paper, we give a complete list of bow shock and magnetopause crossings (from June 2016 to August 2022), along with some extra informations (e.g. solar wind dynamic pressure and position of the standoff distances inferred from Joy et al. (2002)). We then select two compression events that occur in succession (inferred from magnetopause crossings) and we present a case study of the response of the Jovian radio emissions. We demonstrate that magnetospheric compressions lead to the activation of new radio sources. Newly activated broadband kilometric emissions are observed almost simultaneously to compression of the magnetosphere, with sources covering a large range of longitudes. Decametric emission sources are seen to be activated more than one rotation later only at specific longitudes and dusk local times. Finally, the activation of narrowband kilometric radiation is not observed during the compression phase, but when the magnetosphere is in its expansion phase. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.03740v2-abstract-full').style.display = 'none'; document.getElementById('2212.03740v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.11600">arXiv:2210.11600</a> <span> [<a href="https://arxiv.org/pdf/2210.11600">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac91c1">10.3847/1538-4365/ac91c1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Statistical Study and Live Catalogue of Multi-Spacecraft 3He-Rich Time Periods over Solar Cycles 23, 24, and 25 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Hart%2C+S+T">Samuel T. Hart</a>, <a href="/search/physics?searchtype=author&query=Dayeh%2C+M+A">Maher A. Dayeh</a>, <a href="/search/physics?searchtype=author&query=Bu%C4%8D%C3%ADk%2C+R">Radoslav Bu膷铆k</a>, <a href="/search/physics?searchtype=author&query=Desai%2C+M+I">Mihir I. Desai</a>, <a href="/search/physics?searchtype=author&query=Ebert%2C+R+W">Robert W. Ebert</a>, <a href="/search/physics?searchtype=author&query=Ho%2C+G+C">George C. Ho</a>, <a href="/search/physics?searchtype=author&query=Li%2C+G">Gang Li</a>, <a href="/search/physics?searchtype=author&query=Mason%2C+G+M">Glenn M. Mason</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.11600v1-abstract-short" style="display: inline;"> Using ion measurements from Ultra-Low-Energy Isotope Spectrometer (ULEIS) observations onboard Advanced Composition Explorer (ACE) and Solar Isotope Spectrometer (SIS) observations onboard the Solar Terrestrial Observatory (STEREO)-A and STEREO-B spacecraft, we have identified 854 3He-rich time periods between 1997 September and 2021 March. We include all event types with observed 3He enhancements… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.11600v1-abstract-full').style.display = 'inline'; document.getElementById('2210.11600v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.11600v1-abstract-full" style="display: none;"> Using ion measurements from Ultra-Low-Energy Isotope Spectrometer (ULEIS) observations onboard Advanced Composition Explorer (ACE) and Solar Isotope Spectrometer (SIS) observations onboard the Solar Terrestrial Observatory (STEREO)-A and STEREO-B spacecraft, we have identified 854 3He-rich time periods between 1997 September and 2021 March. We include all event types with observed 3He enhancements such as corotating interaction regions (CIRs), gradual solar energetic particle (SEP) events, interplanetary shocks, and impulsive SEP events. We employ two different mass separation techniques to obtain 3He, 4He, Fe, and O fluences for each event, and we determine the 3He/4He and Fe/O abundance ratios between 0.32 to 0.45 MeV/nucleon and 0.64 to 1.28 MeV/nucleon. We find a clear correlation in the 3He/4He and Fe/O abundance ratios between both energy ranges. We find two distinct trends in the 3He/4He vs. Fe/O relation. For low 3He/4He values, there is a positive linear correlation between 3He/4He and Fe/O. However, at 3He/4He ~ 0.3, Fe/O appears to reach a limit and the correlation weakens significantly. We provide a live catalogue of 3He rich time periods that includes the robust determination of the onset and end times of the 3He enhancements in SEP-associated periods for different types of events observed my multiple spacecraft. This catalogue is available for public use. New releases will follow after major additions such as adding new periods from new missions (e.g., Parker Solar Probe and Solar Orbiter), identifying event types (impulsive SEP events, etc.), or adding new parameters such as remote observations detailing characteristics of the active regions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.11600v1-abstract-full').style.display = 'none'; document.getElementById('2210.11600v1-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 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 9 figures, publishing in ApJ Supplemental Series</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.05386">arXiv:2209.05386</a> <span> [<a href="https://arxiv.org/pdf/2209.05386">pdf</a>, <a href="https://arxiv.org/format/2209.05386">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="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/10.3847/1538-4357/acb7e0">10.3847/1538-4357/acb7e0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observation of Turbulent Magnetohydrodynamic Cascade in the Jovian Magnetosheath </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Andr%C3%A9s%2C+N">N. Andr茅s</a>, <a href="/search/physics?searchtype=author&query=Bandyopadhyay%2C+R">R. Bandyopadhyay</a>, <a href="/search/physics?searchtype=author&query=McComas%2C+D+J">D. J. McComas</a>, <a href="/search/physics?searchtype=author&query=Szalay%2C+J+R">J. R. Szalay</a>, <a href="/search/physics?searchtype=author&query=Allegrini%2C+F">F. Allegrini</a>, <a href="/search/physics?searchtype=author&query=Ebert%2C+R+W">R. W. Ebert</a>, <a href="/search/physics?searchtype=author&query=Gershman%2C+D+J">D. J. Gershman</a>, <a href="/search/physics?searchtype=author&query=Connerney%2C+J+E+P">J. E. P. Connerney</a>, <a href="/search/physics?searchtype=author&query=Bolton%2C+S+J">S. J. Bolton</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.05386v2-abstract-short" style="display: inline;"> We present the first estimation of the energy cascade rate in Jupiter's magnetosheath (MS). We use in-situ observations from the Jovian Auroral Distributions Experiment (JADE) and the magnetometer investigation (MAG) instruments onboard the Juno spacecraft, in concert with two recent compressible models to investigate the cascade rate in the magnetohydrodynamic (MHD) scales. While a high level of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.05386v2-abstract-full').style.display = 'inline'; document.getElementById('2209.05386v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.05386v2-abstract-full" style="display: none;"> We present the first estimation of the energy cascade rate in Jupiter's magnetosheath (MS). We use in-situ observations from the Jovian Auroral Distributions Experiment (JADE) and the magnetometer investigation (MAG) instruments onboard the Juno spacecraft, in concert with two recent compressible models to investigate the cascade rate in the magnetohydrodynamic (MHD) scales. While a high level of compressible density fluctuations is observed in the Jovian MS, a constant energy flux exists in the MHD inertial range. The compressible isothermal and polytropic energy cascade rates increase in the MHD range when density fluctuations are present. We find that the energy cascade rate in Jupiter's magnetosheath is at least two orders of magnitude (100 times) smaller than the corresponding typical value in the Earth's magnetosheath. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.05386v2-abstract-full').style.display = 'none'; document.getElementById('2209.05386v2-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> 31 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To be published in The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1706.04322">arXiv:1706.04322</a> <span> [<a href="https://arxiv.org/pdf/1706.04322">pdf</a>, <a href="https://arxiv.org/ps/1706.04322">ps</a>, <a href="https://arxiv.org/format/1706.04322">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1002/2015JA021762">10.1002/2015JA021762 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Modeling Transport of Energetic Particles in Corotating Interaction Region -- A case Study </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Zhao%2C+L">Lulu Zhao</a>, <a href="/search/physics?searchtype=author&query=Li%2C+G">Gang Li</a>, <a href="/search/physics?searchtype=author&query=Ebert%2C+R+W">R. W. Ebert</a>, <a href="/search/physics?searchtype=author&query=Dayeh%2C+M+A">M. A. Dayeh</a>, <a href="/search/physics?searchtype=author&query=Desai%2C+M+I">M. I. Desai</a>, <a href="/search/physics?searchtype=author&query=Mason%2C+G+M">G. M. Mason</a>, <a href="/search/physics?searchtype=author&query=Wu%2C+Z">Zhao Wu</a>, <a href="/search/physics?searchtype=author&query=Chen%2C+Y">Yao Chen</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="1706.04322v1-abstract-short" style="display: inline;"> We investigate energetic particle transport in Corotating Interaction Regions (CIRs) through a case study. The CIR event we study occurred on $2008$ February $08$ and was observed by both the Advanced Composition Explorer (ACE) and the twin Solar TErrestrial RElations Observatory (STEREO)-B spacecraft. An in-situ reverse shock was observed by STEREO-B ($1.0$ AU) but not ACE ($0.98$ AU). Using STER… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.04322v1-abstract-full').style.display = 'inline'; document.getElementById('1706.04322v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1706.04322v1-abstract-full" style="display: none;"> We investigate energetic particle transport in Corotating Interaction Regions (CIRs) through a case study. The CIR event we study occurred on $2008$ February $08$ and was observed by both the Advanced Composition Explorer (ACE) and the twin Solar TErrestrial RElations Observatory (STEREO)-B spacecraft. An in-situ reverse shock was observed by STEREO-B ($1.0$ AU) but not ACE ($0.98$ AU). Using STEREO-B observations and assuming the CIR structure does not vary significantly in the corotating frame, we estimate the shock location at later times for both the STEREO-B and ACE observations. Further assuming the accelerated particle spectral shape at the shock does not vary with shock location, we calculate the particle differential intensities as observed by ACE and STEREO-B at two different times by solving the focused transport equation using a Monte-Carlo simulation. We assume that particles move along Parker's field and experience no cross-field diffusion. We find that the modulation of sub-MeV/nucleon particles is significant. To obtain reasonable comparisons between the simulations and the observations by both ACE and STEREO-B, one has to assume that the CIR shock can accelerate more particles at a larger heliocentric distance than at a smaller heliocentric distance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.04322v1-abstract-full').style.display = 'none'; document.getElementById('1706.04322v1-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 June, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">Published in JGR</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J. Geophys. Res. Space Physics, 121, 77-92 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1605.03922">arXiv:1605.03922</a> <span> [<a href="https://arxiv.org/pdf/1605.03922">pdf</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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/0004-637X/828/2/106">10.3847/0004-637X/828/2/106 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectral properties of large gradual solar energetic particle events - II -Systematic Q/M-dependence of heavy ion spectral breaks </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Desai%2C+M+I">M. I. Desai</a>, <a href="/search/physics?searchtype=author&query=Mason%2C+G+M">G. M. Mason</a>, <a href="/search/physics?searchtype=author&query=Dayeh%2C+M+A">M. A. Dayeh</a>, <a href="/search/physics?searchtype=author&query=Ebert%2C+R+W">R. W. Ebert</a>, <a href="/search/physics?searchtype=author&query=McComas%2C+D+J">D. J. McComas</a>, <a href="/search/physics?searchtype=author&query=Li%2C+G">G. Li</a>, <a href="/search/physics?searchtype=author&query=Cohen%2C+C+M+S">C. M. S. Cohen</a>, <a href="/search/physics?searchtype=author&query=Mewaldt%2C+R+A">R. A. Mewaldt</a>, <a href="/search/physics?searchtype=author&query=Schwadron%2C+N+A">N. A. Schwadron</a>, <a href="/search/physics?searchtype=author&query=Smith%2C+C+W">C. W. Smith</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="1605.03922v1-abstract-short" style="display: inline;"> We fit the $\sim$0.1-500 MeV/nucleon H-Fe spectra in 46 large SEP events surveyed by Desai et al. (2016) with the double power-law Band function to obtain a normalization constant, low- and high-energy parameters $纬_a$ and $纬_b$; and break energy $E_B$. We also calculate the low-energy power-law spectral slope $纬_1$. We find that: 1) $纬_a$, $纬_1$, and $纬_b$ are species-independent within a given S… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.03922v1-abstract-full').style.display = 'inline'; document.getElementById('1605.03922v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.03922v1-abstract-full" style="display: none;"> We fit the $\sim$0.1-500 MeV/nucleon H-Fe spectra in 46 large SEP events surveyed by Desai et al. (2016) with the double power-law Band function to obtain a normalization constant, low- and high-energy parameters $纬_a$ and $纬_b$; and break energy $E_B$. We also calculate the low-energy power-law spectral slope $纬_1$. We find that: 1) $纬_a$, $纬_1$, and $纬_b$ are species-independent within a given SEP event, and the spectra steepen with increasing energy; 2) $E_B$'s are well ordered by Q/M ratio, and decrease systematically with decreasing Q/M, scaling as (Q/M)$^伪$ with $伪$ varying between $\sim$0.2-3; 3) $伪$ is well correlated with Fe/O at $\sim$0.16-0.23 MeV/nucleon and CME speed; 4) In most events: $伪<$1.4, the spectra steepen significantly at higher energy with $纬_b$-$纬_a >$3; and 5) Seven out of 9 extreme SEP events (associated with faster CMEs and GLEs) are Fe-rich, have $伪>$1.4, have flatter spectra at low and high energies with $纬_b$-$纬_a <$3. The species-independence of $纬_a$, $纬_1$, and $纬_b$ and the systematic Q/M dependence of $E_B$ within an event, as well as the range of values for $伪$ suggest that the formation of double power-laws in SEP events occurs primarily due to diffusive acceleration at near-Sun CME shocks and not due to scattering in the interplanetary turbulence. In most events, the Q/M-dependence of $E_B$ is consistent with the equal diffusion coefficient condition while the event-to-event variations in $伪$ are probably driven by differences in the near-shock wave intensity spectra, which are flatter than the Kolmogorov turbulence spectrum but still weaker compared to that inferred for the extreme events. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.03922v1-abstract-full').style.display = 'none'; document.getElementById('1605.03922v1-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> 12 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2016. </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">49 pages, 13 figures, 3 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1401.2214">arXiv:1401.2214</a> <span> [<a href="https://arxiv.org/pdf/1401.2214">pdf</a>, <a href="https://arxiv.org/ps/1401.2214">ps</a>, <a href="https://arxiv.org/format/1401.2214">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/10.1088/0004-637X/781/1/17">10.1088/0004-637X/781/1/17 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observation of Energetic particles between a pair of Corotating Interaction Regions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Wu%2C+Z">Z. Wu</a>, <a href="/search/physics?searchtype=author&query=Chen%2C+Y">Y. Chen</a>, <a href="/search/physics?searchtype=author&query=Li%2C+G">G. Li</a>, <a href="/search/physics?searchtype=author&query=Zhao%2C+L+L">L. L. Zhao</a>, <a href="/search/physics?searchtype=author&query=Ebert%2C+R+W">R. W. Ebert</a>, <a href="/search/physics?searchtype=author&query=Desai%2C+M+I">M. I. Desai</a>, <a href="/search/physics?searchtype=author&query=Mason%2C+G+M">G. M. Mason</a>, <a href="/search/physics?searchtype=author&query=Lavraud%2C+B">B. Lavraud</a>, <a href="/search/physics?searchtype=author&query=Zhao%2C+L">L. Zhao</a>, <a href="/search/physics?searchtype=author&query=Liu%2C+Y+C+-">Y. C. -M. Liu</a>, <a href="/search/physics?searchtype=author&query=Guo%2C+F">F. Guo</a>, <a href="/search/physics?searchtype=author&query=Tang%2C+C+L">C. L. Tang</a>, <a href="/search/physics?searchtype=author&query=Landi%2C+E">E. Landi</a>, <a href="/search/physics?searchtype=author&query=Sauvaud%2C+J">J. Sauvaud</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="1401.2214v1-abstract-short" style="display: inline;"> We report observations of the acceleration and trapping of energetic ions and electrons between a pair of corotating interaction regions (CIRs). The event occurred in Carrington Rotation 2060. Observed at spacecraft STEREO-B, the two CIRs were separated by less than 5 days. In contrast to other CIR events, the fluxes of energetic ions and electrons in this event reached their maxima between the tr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.2214v1-abstract-full').style.display = 'inline'; document.getElementById('1401.2214v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1401.2214v1-abstract-full" style="display: none;"> We report observations of the acceleration and trapping of energetic ions and electrons between a pair of corotating interaction regions (CIRs). The event occurred in Carrington Rotation 2060. Observed at spacecraft STEREO-B, the two CIRs were separated by less than 5 days. In contrast to other CIR events, the fluxes of energetic ions and electrons in this event reached their maxima between the trailing-edge of the first CIR and the leading edge of the second CIR. The radial magnetic field (Br) reversed its sense and the anisotropy of the flux also changed from sunward to anti-sunward between the two CIRs. Furthermore, there was an extended period of counter-streaming suprathermal electrons between the two CIRs. Similar observations for this event were also obtained for ACE and STEREO-A. We conjecture that these observations were due to a "U-shape" large scale magnetic field topology connecting the reverse shock of the first CIR and the forward shock of the second CIR. Such a disconnected U-shaped magnetic field topology may have formed due to magnetic reconnection in the upper corona. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.2214v1-abstract-full').style.display = 'none'; document.getElementById('1401.2214v1-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 January, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2014. </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 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