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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/2503.14823">arXiv:2503.14823</a> <span> [<a href="https://arxiv.org/pdf/2503.14823">pdf</a>, <a href="https://arxiv.org/format/2503.14823">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="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> Scaling of Particle Heating in Shocks and Magnetic Reconnection </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Oka%2C+M">Mitsuo Oka</a>, <a href="/search/physics?searchtype=author&query=Phan%2C+T+D">Tai D. Phan</a>, <a href="/search/physics?searchtype=author&query=%C3%98ieroset%2C+M">Marit 脴ieroset</a>, <a href="/search/physics?searchtype=author&query=Gershman%2C+D+J">Daniel J. Gershman</a>, <a href="/search/physics?searchtype=author&query=Torbert%2C+R+B">Roy B. Torbert</a>, <a href="/search/physics?searchtype=author&query=Burch%2C+J+L">James L. Burch</a>, <a href="/search/physics?searchtype=author&query=Angelopoulos%2C+V">Vassilis Angelopoulos</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="2503.14823v1-abstract-short" style="display: inline;"> Particles are heated efficiently through energy conversion processes such as shocks and magnetic reconnection in collisionless plasma environments. While empirical scaling laws for the temperature increase have been obtained, the precise mechanism of energy partition between ions and electrons remains unclear. Here we show, based on coupled theoretical and observational scaling analyses, that the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2503.14823v1-abstract-full').style.display = 'inline'; document.getElementById('2503.14823v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2503.14823v1-abstract-full" style="display: none;"> Particles are heated efficiently through energy conversion processes such as shocks and magnetic reconnection in collisionless plasma environments. While empirical scaling laws for the temperature increase have been obtained, the precise mechanism of energy partition between ions and electrons remains unclear. Here we show, based on coupled theoretical and observational scaling analyses, that the temperature increase, $螖T$, depends linearly on three factors: the available magnetic energy per particle, the Alfv茅n Mach number (or reconnection rate), and the characteristic spatial scale $L$. Based on statistical datasets obtained from Earth's plasma environment, we find that $L$ is on the order of (1) the ion gyro-radius for ion heating at shocks, (2) the ion inertial length for ion heating in magnetic reconnection, and (3) the hybrid inertial length for electron heating in both shocks and magnetic reconnection. With these scales, we derive the ion-to-electron ratios of temperature increase as $螖T_{\rm i}/螖T_{\rm e} = (3尾_{\rm i}/2)^{1/2}(m_{\rm i}/m_{\rm e})^{1/4}$ for shocks and $螖T_{\rm i}/螖T_{\rm e} = (m_{\rm i}/m_{\rm e})^{1/4}$ for magnetic reconnection, where $尾_{\rm i}$ is the ion plasma beta, and $m_{\rm i}$ and $ m_{\rm e}$ are the ion and electron particle masses, respectively. We anticipate that this study will serve as a starting point for a better understanding of particle heating in space plasmas, enabling more sophisticated modeling of its scaling and universality. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2503.14823v1-abstract-full').style.display = 'none'; document.getElementById('2503.14823v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 March, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">15 pages, 8 figures; accepted for publication in 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/2412.05974">arXiv:2412.05974</a> <span> [<a href="https://arxiv.org/pdf/2412.05974">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="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> <p class="title is-5 mathjax"> Relativistic Electron Acceleration and the 'Ankle' Spectral Feature in Earth's Magnetotail Reconnection </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Sun%2C+W">Weijie Sun</a>, <a href="/search/physics?searchtype=author&query=Oka%2C+M">Mitsuo Oka</a>, <a href="/search/physics?searchtype=author&query=%C3%98ieroset%2C+M">Marit 脴ieroset</a>, <a href="/search/physics?searchtype=author&query=Turner%2C+D+L">Drew L. Turner</a>, <a href="/search/physics?searchtype=author&query=Phan%2C+T">Tai Phan</a>, <a href="/search/physics?searchtype=author&query=Cohen%2C+I+J">Ian J. Cohen</a>, <a href="/search/physics?searchtype=author&query=Li%2C+X">Xiaocan Li</a>, <a href="/search/physics?searchtype=author&query=Huang%2C+J">Jia Huang</a>, <a href="/search/physics?searchtype=author&query=Smith%2C+A">Andy Smith</a>, <a href="/search/physics?searchtype=author&query=Slavin%2C+J+A">James A. Slavin</a>, <a href="/search/physics?searchtype=author&query=Poh%2C+G">Gangkai Poh</a>, <a href="/search/physics?searchtype=author&query=Genestreti%2C+K+J">Kevin J. Genestreti</a>, <a href="/search/physics?searchtype=author&query=Gershman%2C+D">Dan Gershman</a>, <a href="/search/physics?searchtype=author&query=Dokgo%2C+K">Kyunghwan. Dokgo</a>, <a href="/search/physics?searchtype=author&query=Le%2C+G">Guan Le</a>, <a href="/search/physics?searchtype=author&query=Nakamura%2C+R">Rumi Nakamura</a>, <a href="/search/physics?searchtype=author&query=Burch%2C+J+L">James L. Burch</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="2412.05974v1-abstract-short" style="display: inline;"> Electrons are accelerated to high, non-thermal energies during explosive energy-release events in space, such as magnetic reconnection. However, the properties and acceleration mechanisms of relativistic electrons directly associated with reconnection X-line are not well understood. This study utilizes Magnetospheric Multiscale (MMS) measurements to analyze the flux and spectral features of sub-re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.05974v1-abstract-full').style.display = 'inline'; document.getElementById('2412.05974v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.05974v1-abstract-full" style="display: none;"> Electrons are accelerated to high, non-thermal energies during explosive energy-release events in space, such as magnetic reconnection. However, the properties and acceleration mechanisms of relativistic electrons directly associated with reconnection X-line are not well understood. This study utilizes Magnetospheric Multiscale (MMS) measurements to analyze the flux and spectral features of sub-relativistic to relativistic (~ 80 to 560 keV) electrons during a magnetic reconnection event in Earth's magnetotail. This event provided a unique opportunity to measure the electrons directly energized by X-line as MMS stayed in the separatrix layer, where the magnetic field directly connects to the X-line, for approximately half of the observation period. Our analysis revealed that the fluxes of relativistic electrons were clearly enhanced within the separatrix layer, and the highest flux was directed away from the X-line, which suggested that these electrons originated directly from the X-line. Spectral analysis showed that these relativistic electrons deviated from the main plasma sheet population and exhibited an "ankle" feature similar to that observed in galactic cosmic rays. The contribution of "ankle" electrons to the total electron energy density increased from 0.1% to 1% in the separatrix layer, though the spectral slopes did not exhibit clear variations. Further analysis indicated that while these relativistic electrons originated from the X-line, they experienced a non-negligible degree of scattering during transport. These findings provide clear evidence that magnetic reconnection in Earth's magnetotail can efficiently energize relativistic electrons directly at the X-line, providing new insights into the complex processes governing electron dynamics during magnetic reconnection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.05974v1-abstract-full').style.display = 'none'; document.getElementById('2412.05974v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </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">23 pages, 5 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/2001.06048">arXiv:2001.06048</a> <span> [<a href="https://arxiv.org/pdf/2001.06048">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="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/10.3847/1538-4365/ab55ee">10.3847/1538-4365/ab55ee <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Parker Solar Probe In-Situ Observations of Magnetic Reconnection Exhausts During Encounter 1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Phan%2C+T+D">T. D. Phan</a>, <a href="/search/physics?searchtype=author&query=Bale%2C+S+D">S. D. Bale</a>, <a href="/search/physics?searchtype=author&query=Eastwood%2C+J+P">J. P. Eastwood</a>, <a href="/search/physics?searchtype=author&query=Lavraud%2C+B">B. Lavraud</a>, <a href="/search/physics?searchtype=author&query=Drake%2C+J+F">J. F. Drake</a>, <a href="/search/physics?searchtype=author&query=Oieroset%2C+M">M. Oieroset</a>, <a href="/search/physics?searchtype=author&query=Shay%2C+M+A">M. A. Shay</a>, <a href="/search/physics?searchtype=author&query=Pulupa%2C+M">M. Pulupa</a>, <a href="/search/physics?searchtype=author&query=Stevens%2C+M">M. Stevens</a>, <a href="/search/physics?searchtype=author&query=MacDowall%2C+R+J">R. J. MacDowall</a>, <a href="/search/physics?searchtype=author&query=Case%2C+A+W">A. W. Case</a>, <a href="/search/physics?searchtype=author&query=Larson%2C+D">D. Larson</a>, <a href="/search/physics?searchtype=author&query=Kasper%2C+J">J. Kasper</a>, <a href="/search/physics?searchtype=author&query=Whittlesey%2C+P">P. Whittlesey</a>, <a href="/search/physics?searchtype=author&query=Szabo%2C+A">A. Szabo</a>, <a href="/search/physics?searchtype=author&query=Korreck%2C+K+E">K. E. Korreck</a>, <a href="/search/physics?searchtype=author&query=Bonnell%2C+J+W">J. W. Bonnell</a>, <a href="/search/physics?searchtype=author&query=de+Wit%2C+T+D">T. Dudok de Wit</a>, <a href="/search/physics?searchtype=author&query=Goetz%2C+K">K. Goetz</a>, <a href="/search/physics?searchtype=author&query=Harvey%2C+P+R">P. R. Harvey</a>, <a href="/search/physics?searchtype=author&query=Horbury%2C+T+S">T. S. Horbury</a>, <a href="/search/physics?searchtype=author&query=Livi%2C+R">R. Livi</a>, <a href="/search/physics?searchtype=author&query=Malaspina%2C+D">D. Malaspina</a>, <a href="/search/physics?searchtype=author&query=Paulson%2C+K">K. Paulson</a>, <a href="/search/physics?searchtype=author&query=Raouafi%2C+N+E">N. E. Raouafi</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2001.06048v1-abstract-short" style="display: inline;"> Magnetic reconnection in current sheets converts magnetic energy into particle energy. The process may play an important role in the acceleration and heating of the solar wind close to the Sun. Observations from Parker Solar Probe provide a new opportunity to study this problem, as it measures the solar wind at unprecedented close distances to the Sun. During the 1st orbit, PSP encountered a large… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.06048v1-abstract-full').style.display = 'inline'; document.getElementById('2001.06048v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.06048v1-abstract-full" style="display: none;"> Magnetic reconnection in current sheets converts magnetic energy into particle energy. The process may play an important role in the acceleration and heating of the solar wind close to the Sun. Observations from Parker Solar Probe provide a new opportunity to study this problem, as it measures the solar wind at unprecedented close distances to the Sun. During the 1st orbit, PSP encountered a large number of current sheets in the solar wind through perihelion at 35.7 solar radii. We performed a comprehensive survey of these current sheets and found evidence for 21 reconnection exhausts. These exhausts were observed in heliospheric current sheets, coronal mass ejections, and regular solar wind. However, we find that the majority of current sheets encountered around perihelion, where the magnetic field was strongest and plasma beta was lowest, were Alfv茅nic structures associated with bursty radial jets and these current sheets did not appear to be undergoing local reconnection. We examined conditions around current sheets to address why some current sheets reconnected, while others did not. A key difference appears to be the degree of plasma velocity shear across the current sheets: The median velocity shear for the 21 reconnection exhausts was 24% of the Alfv茅n velocity shear, whereas the median shear across 43 Alfv茅nic current sheets examined was 71% of the Alfv茅n velocity shear. This finding could suggest that large, albeit sub-Alfv茅nic, velocity shears suppress reconnection. An alternative interpretation is that the Alfv茅nic current sheets are isolated rotational discontinuities which do not undergo local reconnection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.06048v1-abstract-full').style.display = 'none'; document.getElementById('2001.06048v1-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">In Press (accepted by ApJS on 2019-11-08) This paper is part of the Parker Solar Probe ApJS Special Issue Current citation: Phan, T. D., S. D. Bale, J. P. Eastwood, et al. (2019), Parker Solar Probe In-Situ Observations of Magnetic Reconnection Exhausts During Encounter 1, ApJS., in press, doi: 10.3847/1538-4365/ab55ee</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1602.08482">arXiv:1602.08482</a> <span> [<a href="https://arxiv.org/pdf/1602.08482">pdf</a>, <a href="https://arxiv.org/ps/1602.08482">ps</a>, <a href="https://arxiv.org/format/1602.08482">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/10.1002/2015JA022040">10.1002/2015JA022040 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> In-situ evidence of electron energization in the electron diffusion region of magnetotail reconnection </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Oka%2C+M">Mitsuo Oka</a>, <a href="/search/physics?searchtype=author&query=Phan%2C+T">Tai Phan</a>, <a href="/search/physics?searchtype=author&query=Oieroset%2C+M">Marit Oieroset</a>, <a href="/search/physics?searchtype=author&query=Angelopoulos%2C+V">Vassilis Angelopoulos</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="1602.08482v1-abstract-short" style="display: inline;"> Magnetic reconnection is an explosive energy-release process in laboratory, space and astrophysical plasmas. While magnetic fields can `break' and `reconnect' in a very small region called the electron diffusion region (EDR), there have been conflicting theories as to whether this region can be a place of rapid energization of plasmas. Here we report a fortuitous encounter of the EDR by THEMIS in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.08482v1-abstract-full').style.display = 'inline'; document.getElementById('1602.08482v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1602.08482v1-abstract-full" style="display: none;"> Magnetic reconnection is an explosive energy-release process in laboratory, space and astrophysical plasmas. While magnetic fields can `break' and `reconnect' in a very small region called the electron diffusion region (EDR), there have been conflicting theories as to whether this region can be a place of rapid energization of plasmas. Here we report a fortuitous encounter of the EDR by THEMIS in the Earth's magnetotail where significant heating and demagnetization of electrons were observed. Additional energization was observed on both sides (immediate upstream and downstream) of the EDR, leading to a total of more than an order of magnitude energization across this region. The results demonstrate that, despite its minuscule size, the EDR does indeed contribute to the overall process of electron energization via magnetic reconnection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.08482v1-abstract-full').style.display = 'none'; document.getElementById('1602.08482v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">10 pages, 7 figures; accepted by Journal of Geophysical Research</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1410.1206">arXiv:1410.1206</a> <span> [<a href="https://arxiv.org/pdf/1410.1206">pdf</a>, <a href="https://arxiv.org/ps/1410.1206">ps</a>, <a href="https://arxiv.org/format/1410.1206">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="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/10.1063/1.4904203">10.1063/1.4904203 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Electron Heating During Magnetic Reconnection: A Simulation Scaling Study </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Shay%2C+M+A">M. A. Shay</a>, <a href="/search/physics?searchtype=author&query=Haggerty%2C+C+C">C. C. Haggerty</a>, <a href="/search/physics?searchtype=author&query=Phan%2C+T+D">T. D. Phan</a>, <a href="/search/physics?searchtype=author&query=Drake%2C+J+F">J. F. Drake</a>, <a href="/search/physics?searchtype=author&query=Cassak%2C+P+A">P. A. Cassak</a>, <a href="/search/physics?searchtype=author&query=Wu%2C+P">P. Wu</a>, <a href="/search/physics?searchtype=author&query=Oieroset%2C+M">M. Oieroset</a>, <a href="/search/physics?searchtype=author&query=Swisdak%2C+M">M. Swisdak</a>, <a href="/search/physics?searchtype=author&query=Malakit%2C+K">K. Malakit</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="1410.1206v1-abstract-short" style="display: inline;"> Electron bulk heating during magnetic reconnection with symmetric inflow conditions is examined using kinetic particle-in-cell (PIC) simulations. The degree of electron heating is well correlated with the inflowing Alfv茅n speed $c_{Ar}$ based on the reconnecting magnetic field through the relation $螖T_e = 0.033 \,m_i\,c_{Ar}^2$, where $螖T_{e}$ is the increase in electron temperature. For the range… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1410.1206v1-abstract-full').style.display = 'inline'; document.getElementById('1410.1206v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1410.1206v1-abstract-full" style="display: none;"> Electron bulk heating during magnetic reconnection with symmetric inflow conditions is examined using kinetic particle-in-cell (PIC) simulations. The degree of electron heating is well correlated with the inflowing Alfv茅n speed $c_{Ar}$ based on the reconnecting magnetic field through the relation $螖T_e = 0.033 \,m_i\,c_{Ar}^2$, where $螖T_{e}$ is the increase in electron temperature. For the range of simulations performed, the heating shows almost no correlation with inflow total temperature $T_{tot} = T_i + T_e$ or plasma $尾$. An out-of-plane (guide) magnetic field of similar magnitude to the reconnecting field does not affect the total heating, but it does quench perpendicular heating, with almost all heating being in the parallel direction. These results are qualitatively consistent with a recent statistical survey of electron heating in the dayside magnetopause, which also found that $螖T_e$ was proportional to the inflowing Alfv茅n speed. The net electron heating varies very little with distance downstream of the x-line. The simulations show at most a very weak dependence of electron heating on the ion to electron mass ratio. In the antiparallel reconnection case, the largely parallel heating is eventually isotropized downstream due a scattering mechanism such as stochastic particle motion or instabilities. The study highlights key properties that must be satisfied by an electron heating mechanism: (1) Preferential heating in the parallel direction; (2) Heating proportional to $m_i\,c_{Ar}^2$; (3) At most a weak dependence on electron mass; and (4) An exhaust electron temperature that varies little with distance from the x-line. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1410.1206v1-abstract-full').style.display = 'none'; document.getElementById('1410.1206v1-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 October, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 1 table, 7 figures. Submitted to Physics of Plasmas</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

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