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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/2305.06106">arXiv:2305.06106</a> <span> [<a href="https://arxiv.org/pdf/2305.06106">pdf</a>, <a href="https://arxiv.org/format/2305.06106">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> </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/acd44e">10.3847/1538-4357/acd44e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Merging of a Coronal Dimming and the Southern Polar Coronal Hole </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ngampoopun%2C+N">Nawin Ngampoopun</a>, <a href="/search/astro-ph?searchtype=author&query=Long%2C+D+M">David M. Long</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+D">Deborah Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Green%2C+L+M">Lucie M. Green</a>, <a href="/search/astro-ph?searchtype=author&query=Yardley%2C+S+L">Stephanie L. Yardley</a>, <a href="/search/astro-ph?searchtype=author&query=James%2C+A+W">Alexander W. James</a>, <a href="/search/astro-ph?searchtype=author&query=To%2C+A+S+H">Andy S. H. To</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="2305.06106v1-abstract-short" style="display: inline;"> We report on the merging between the southern polar coronal hole and an adjacent coronal dimming induced by a coronal mass ejection on 2022 March 18, resulting in the merged region persisting for at least 72 hrs. We use remote sensing data from multiple co-observing spacecraft to understand the physical processes during this merging event. The evolution of the merger is examined using Extreme-Ultr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.06106v1-abstract-full').style.display = 'inline'; document.getElementById('2305.06106v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.06106v1-abstract-full" style="display: none;"> We report on the merging between the southern polar coronal hole and an adjacent coronal dimming induced by a coronal mass ejection on 2022 March 18, resulting in the merged region persisting for at least 72 hrs. We use remote sensing data from multiple co-observing spacecraft to understand the physical processes during this merging event. The evolution of the merger is examined using Extreme-UltraViolet (EUV) images obtained from the Atmospheric Imaging Assembly onboard the Solar Dynamic Observatory and Extreme Ultraviolet Imager onboard the Solar Orbiter spacecraft. The plasma dynamics are quantified using spectroscopic data obtained from the EUV Imaging Spectrometer onboard Hinode. The photospheric magnetograms from the Helioseismic and Magnetic Imager are used to derive magnetic field properties. To our knowledge, this work is the first spectroscopical analysis of the merging of two open-field structures. We find that the coronal hole and the coronal dimming become indistinguishable after the merging. The upflow speeds inside the coronal dimming become more similar to that of a coronal hole, with a mixture of plasma upflows and downflows observable after the merging. The brightening of bright points and the appearance of coronal jets inside the merged region further imply ongoing reconnection processes. We propose that component reconnection between the coronal hole and coronal dimming fields plays an important role during this merging event, as the footpoint switching resulting from the reconnection allows the coronal dimming to intrude onto the boundary of the southern polar coronal hole. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.06106v1-abstract-full').style.display = 'none'; document.getElementById('2305.06106v1-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 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">17 pages, 8 figures, accepted for publication 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/2304.09570">arXiv:2304.09570</a> <span> [<a href="https://arxiv.org/pdf/2304.09570">pdf</a>, <a href="https://arxiv.org/format/2304.09570">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/10.3847/1538-4365/acd24b">10.3847/1538-4365/acd24b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Slow Solar Wind Connection Science during Solar Orbiter's First Close Perihelion Passage </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yardley%2C+S+L">Stephanie L. Yardley</a>, <a href="/search/astro-ph?searchtype=author&query=Owen%2C+C+J">Christopher J. Owen</a>, <a href="/search/astro-ph?searchtype=author&query=Long%2C+D+M">David M. Long</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+D">Deborah Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D+H">David H. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Polito%2C+V">Vanessa Polito</a>, <a href="/search/astro-ph?searchtype=author&query=Green%2C+L+M">Lucie M. Green</a>, <a href="/search/astro-ph?searchtype=author&query=Matthews%2C+S">Sarah Matthews</a>, <a href="/search/astro-ph?searchtype=author&query=Owens%2C+M">Mathew Owens</a>, <a href="/search/astro-ph?searchtype=author&query=Lockwood%2C+M">Mike Lockwood</a>, <a href="/search/astro-ph?searchtype=author&query=Stansby%2C+D">David Stansby</a>, <a href="/search/astro-ph?searchtype=author&query=James%2C+A+W">Alexander W. James</a>, <a href="/search/astro-ph?searchtype=author&query=Valori%2C+G">Gherado Valori</a>, <a href="/search/astro-ph?searchtype=author&query=Giunta%2C+A">Alessandra Giunta</a>, <a href="/search/astro-ph?searchtype=author&query=Janvier%2C+M">Miho Janvier</a>, <a href="/search/astro-ph?searchtype=author&query=Ngampoopun%2C+N">Nawin Ngampoopun</a>, <a href="/search/astro-ph?searchtype=author&query=Mihailescu%2C+T">Teodora Mihailescu</a>, <a href="/search/astro-ph?searchtype=author&query=To%2C+A+S+H">Andy S. H. To</a>, <a href="/search/astro-ph?searchtype=author&query=van+Driel-Gesztelyi%2C+L">Lidia van Driel-Gesztelyi</a>, <a href="/search/astro-ph?searchtype=author&query=Demoulin%2C+P">Pascal Demoulin</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Amicis%2C+R">Raffaella D'Amicis</a>, <a href="/search/astro-ph?searchtype=author&query=French%2C+R+J">Ryan J. French</a>, <a href="/search/astro-ph?searchtype=author&query=Suen%2C+G+H+H">Gabriel H. H. Suen</a>, <a href="/search/astro-ph?searchtype=author&query=Roulliard%2C+A+P">Alexis P. Roulliard</a>, <a href="/search/astro-ph?searchtype=author&query=Pinto%2C+R+F">Rui F. Pinto</a> , et al. (54 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.09570v2-abstract-short" style="display: inline;"> The Slow Solar Wind Connection Solar Orbiter Observing Plan (Slow Wind SOOP) was developed to utilise the extensive suite of remote sensing and in situ instruments on board the ESA/NASA Solar Orbiter mission to answer significant outstanding questions regarding the origin and formation of the slow solar wind. The Slow Wind SOOP was designed to link remote sensing and in situ measurements of slow w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.09570v2-abstract-full').style.display = 'inline'; document.getElementById('2304.09570v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.09570v2-abstract-full" style="display: none;"> The Slow Solar Wind Connection Solar Orbiter Observing Plan (Slow Wind SOOP) was developed to utilise the extensive suite of remote sensing and in situ instruments on board the ESA/NASA Solar Orbiter mission to answer significant outstanding questions regarding the origin and formation of the slow solar wind. The Slow Wind SOOP was designed to link remote sensing and in situ measurements of slow wind originating at open-closed field boundaries. The SOOP ran just prior to Solar Orbiter's first close perihelion passage during two remote sensing windows (RSW1 and RSW2) between 2022 March 3-6 and 2022 March 17-22, while Solar Orbiter was at a heliocentric distance of 0.55-0.51 and 0.38-0.34 au from the Sun, respectively. Coordinated observation campaigns were also conducted by Hinode and IRIS. The magnetic connectivity tool was used, along with low latency in situ data, and full-disk remote sensing observations, to guide the target pointing of Solar Orbiter. Solar Orbiter targeted an active region complex during RSW1, the boundary of a coronal hole, and the periphery of a decayed active region during RSW2. Post-observation analysis using the magnetic connectivity tool along with in situ measurements from MAG and SWA/PAS, show that slow solar wind, with velocities between 210 and 600 km/s, arrived at the spacecraft originating from two out of the three of the target regions. The Slow Wind SOOP, despite presenting many challenges, was very successful, providing a blueprint for planning future observation campaigns that rely on the magnetic connectivity of Solar Orbiter. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.09570v2-abstract-full').style.display = 'none'; document.getElementById('2304.09570v2-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">24 pages, 10 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/2301.02034">arXiv:2301.02034</a> <span> [<a href="https://arxiv.org/pdf/2301.02034">pdf</a>, <a href="https://arxiv.org/format/2301.02034">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> </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/acb0c9">10.3847/1538-4357/acb0c9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-stage reconnection powering a solar coronal jet </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Long%2C+D+M">David M. Long</a>, <a href="/search/astro-ph?searchtype=author&query=Chitta%2C+L+P">Lakshmi Pradeep Chitta</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+D">Deborah Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Hannah%2C+I+G">Iain G. Hannah</a>, <a href="/search/astro-ph?searchtype=author&query=Ngampoopun%2C+N">Nawin Ngampoopun</a>, <a href="/search/astro-ph?searchtype=author&query=Berghmans%2C+D">David Berghmans</a>, <a href="/search/astro-ph?searchtype=author&query=Zhukov%2C+A+N">Andrei N. Zhukov</a>, <a href="/search/astro-ph?searchtype=author&query=Teriaca%2C+L">Luca Teriaca</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="2301.02034v1-abstract-short" style="display: inline;"> Coronal jets are short-lived eruptive features commonly observed in polar coronal holes and are thought to play a key role in the transfer of mass and energy into the solar corona. We describe unique contemporaneous observations of a coronal blowout jet seen by the Extreme Ultraviolet Imager onboard the Solar Orbiter spacecraft (SO/EUI) and the Atmospheric Imaging Assembly onboard the Solar Dynami… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.02034v1-abstract-full').style.display = 'inline'; document.getElementById('2301.02034v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.02034v1-abstract-full" style="display: none;"> Coronal jets are short-lived eruptive features commonly observed in polar coronal holes and are thought to play a key role in the transfer of mass and energy into the solar corona. We describe unique contemporaneous observations of a coronal blowout jet seen by the Extreme Ultraviolet Imager onboard the Solar Orbiter spacecraft (SO/EUI) and the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory (SDO/AIA). The coronal jet erupted from the south polar coronal hole, and was observed with high spatial and temporal resolution by both instruments. This enabled identification of the different stages of a breakout reconnection process producing the observed jet. We find bulk plasma flow kinematics of ~100-200 km/s across the lifetime of its observed propagation, with a distinct kink in the jet where it impacted and was subsequently guided by a nearby polar plume. We also identify a faint faster feature ahead of the bulk plasma motion propagating with a velocity of ~715 km/s which we attribute to untwisting of newly reconnected field lines during the eruption. A Differential Emission Measure (DEM) analysis using the SDO/AIA observations revealed a very weak jet signal, indicating that the erupting material was likely much cooler than the coronal passbands used to derive the DEM. This is consistent with the very bright appearance of the jet in the Lyman-$伪$ passband observed by SO/EUI. The DEM was used to estimate the radiative thermal energy of the source region of the coronal jet, finding a value of $\sim2\times10^{24}$ ergs, comparable to the energy of a nanoflare. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.02034v1-abstract-full').style.display = 'none'; document.getElementById('2301.02034v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">12 pages, 6 figures, accepted for publication 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/2110.08506">arXiv:2110.08506</a> <span> [<a href="https://arxiv.org/pdf/2110.08506">pdf</a>, <a href="https://arxiv.org/format/2110.08506">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/10.3847/1538-4357/ac2ee3">10.3847/1538-4357/ac2ee3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Domains of Magnetic Pressure Balance in Parker Solar Probe Observations of the Solar Wind </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ruffolo%2C+D">David Ruffolo</a>, <a href="/search/astro-ph?searchtype=author&query=Ngampoopun%2C+N">Nawin Ngampoopun</a>, <a href="/search/astro-ph?searchtype=author&query=Bhora%2C+Y+R">Yash R. Bhora</a>, <a href="/search/astro-ph?searchtype=author&query=Thepthong%2C+P">Panisara Thepthong</a>, <a href="/search/astro-ph?searchtype=author&query=Pongkitiwanichakul%2C+P">Peera Pongkitiwanichakul</a>, <a href="/search/astro-ph?searchtype=author&query=Matthaeus%2C+W+H">William H. Matthaeus</a>, <a href="/search/astro-ph?searchtype=author&query=Chhiber%2C+R">Rohit Chhiber</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="2110.08506v1-abstract-short" style="display: inline;"> The Parker Solar Probe (PSP) spacecraft is performing the first in situ exploration of the solar wind within 0.2 au of the Sun. Initial observations confirmed the Alfv茅nic nature of aligned fluctuations of the magnetic field B and velocity V in solar wind plasma close to the Sun, in domains of nearly constant magnetic field magnitude $|{\bf B}|$, i.e., approximate magnetic pressure balance. Such d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.08506v1-abstract-full').style.display = 'inline'; document.getElementById('2110.08506v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.08506v1-abstract-full" style="display: none;"> The Parker Solar Probe (PSP) spacecraft is performing the first in situ exploration of the solar wind within 0.2 au of the Sun. Initial observations confirmed the Alfv茅nic nature of aligned fluctuations of the magnetic field B and velocity V in solar wind plasma close to the Sun, in domains of nearly constant magnetic field magnitude $|{\bf B}|$, i.e., approximate magnetic pressure balance. Such domains are interrupted by particularly strong fluctuations, including but not limited to radial field (polarity) reversals, known as switchbacks. It has been proposed that nonlinear Kelvin-Helmholtz instabilities form near magnetic boundaries in the nascent solar wind leading to extensive shear-driven dynamics, strong turbulent fluctuations including switchbacks, and mixing layers that involve domains of approximate magnetic pressure balance. In this work we identify and analyze various aspects of such domains using data from the first five PSP solar encounters. The filling fraction of domains, a measure of Alfv茅nicity, varies from median values of 90% within 0.2 au to 38% outside 0.9 au, with strong fluctuations. We find an inverse association between the mean domain duration and plasma $尾$. We examine whether the mean domain duration is also related to the crossing time of spatial structures frozen into the solar wind flow for extreme cases of the aspect ratio. Our results are inconsistent with long, thin domains aligned along the radial or Parker spiral direction, and compatible with isotropic domains, which is consistent with prior observations of isotropic density fluctuations or ``flocculae'' in the solar wind. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.08506v1-abstract-full').style.display = 'none'; document.getElementById('2110.08506v1-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 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">16 pages, 10 figures, accepted by the Astrophysical Journal</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span 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