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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/2501.02163">arXiv:2501.02163</a> <span> [<a href="https://arxiv.org/pdf/2501.02163">pdf</a>, <a href="https://arxiv.org/format/2501.02163">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> <p class="title is-5 mathjax"> Differentiating the acceleration mechanisms in the slow and Alfv茅nic slow solar wind </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rivera%2C+Y+J">Yeimy J. Rivera</a>, <a href="/search/astro-ph?searchtype=author&query=Badman%2C+S+T">Samuel T. Badman</a>, <a href="/search/astro-ph?searchtype=author&query=Verniero%2C+J+L">J. L. Verniero</a>, <a href="/search/astro-ph?searchtype=author&query=Varesano%2C+T">Tania Varesano</a>, <a href="/search/astro-ph?searchtype=author&query=Stevens%2C+M+L">Michael L. Stevens</a>, <a href="/search/astro-ph?searchtype=author&query=Stawarz%2C+J+E">Julia E. Stawarz</a>, <a href="/search/astro-ph?searchtype=author&query=Reeves%2C+K+K">Katharine K. Reeves</a>, <a href="/search/astro-ph?searchtype=author&query=Raines%2C+J+M">Jim M. Raines</a>, <a href="/search/astro-ph?searchtype=author&query=Raymond%2C+J+C">John C. Raymond</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=Livi%2C+S+A">Stefano A. Livi</a>, <a href="/search/astro-ph?searchtype=author&query=Lepri%2C+S+T">Susan T. Lepri</a>, <a href="/search/astro-ph?searchtype=author&query=Landi%2C+E">Enrico Landi</a>, <a href="/search/astro-ph?searchtype=author&query=Halekas%2C+J+S">Jasper. S. Halekas</a>, <a href="/search/astro-ph?searchtype=author&query=Ervin%2C+T">Tamar Ervin</a>, <a href="/search/astro-ph?searchtype=author&query=Dewey%2C+R+M">Ryan M. Dewey</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marco%2C+R">Rossana De Marco</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=Dakeyo%2C+J">Jean-Baptiste Dakeyo</a>, <a href="/search/astro-ph?searchtype=author&query=Bale%2C+S+D">Stuart D. Bale</a>, <a href="/search/astro-ph?searchtype=author&query=Alterman%2C+B+L">B. L. Alterman</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="2501.02163v1-abstract-short" style="display: inline;"> In the corona, plasma is accelerated to hundreds of kilometers per second, and heated to temperatures hundreds of times hotter than the Sun's surface, before it escapes to form the solar wind. Decades of space-based experiments have shown that the energization process does not stop after it escapes. Instead, the solar wind continues to accelerate and it cools far more slowly than a freely-expandin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.02163v1-abstract-full').style.display = 'inline'; document.getElementById('2501.02163v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.02163v1-abstract-full" style="display: none;"> In the corona, plasma is accelerated to hundreds of kilometers per second, and heated to temperatures hundreds of times hotter than the Sun's surface, before it escapes to form the solar wind. Decades of space-based experiments have shown that the energization process does not stop after it escapes. Instead, the solar wind continues to accelerate and it cools far more slowly than a freely-expanding adiabatic gas. Recent work suggests that fast solar wind requires additional momentum beyond what can be provided by the observed thermal pressure gradients alone whereas it is sufficient for the slowest wind. The additional acceleration for fast wind can be provided through an Alfv茅n wave pressure gradient. Beyond this fast-slow categorization, however, a subset of slow solar wind exhibits high Alfv茅nicity that suggest Alfv茅n waves could play a larger role in its acceleration compared to conventional slow wind outflows. Through a well-timed conjunction between Solar Orbiter and Parker Solar Probe, we trace the energetics of slow wind to compare with a neighboring Alfv茅nic slow solar wind stream. An analysis that integrates remote and heliospheric properties and modeling of the two distinct solar wind streams finds Alfv茅nic slow solar wind behaves like fast wind, where a wave pressure gradient is required to reconcile its full acceleration, while non-Alfv茅nic slow wind can be driven by its non-adiabatic electron and proton thermal pressure gradients. Derived coronal conditions of the source region indicate good model compatibility but extended coronal observations are required to effectively trace solar wind energetics below Parker's orbit. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.02163v1-abstract-full').style.display = 'none'; document.getElementById('2501.02163v1-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> 3 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">20 pages, 9 figures, accepted for publication to ApJ on January 3, 2025</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.04885">arXiv:2412.04885</a> <span> [<a href="https://arxiv.org/pdf/2412.04885">pdf</a>, <a href="https://arxiv.org/format/2412.04885">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> <p class="title is-5 mathjax"> Impact of Two-Population $伪$-particle Distributions on Plasma Stability </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Martinovi%C4%87%2C+M+M">Mihailo M. Martinovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Klein%2C+K+G">Kristopher G. Klein</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marco%2C+R">Rossana De Marco</a>, <a href="/search/astro-ph?searchtype=author&query=Verscharen%2C+D">Daniel Verscharen</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=Bruno%2C+R">Roberto Bruno</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="2412.04885v1-abstract-short" style="display: inline;"> The stability of weakly collisional plasmas is well represented by linear theory, and the generated waves play an essential role in the thermodynamics of these systems. The velocity distribution functions (VDF) characterizing kinetic particle behavior are commonly represented as a sum of anisotropic bi-Maxwellians. For the majority of in situ observations of solar wind plasmas enabled by heliosphe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.04885v1-abstract-full').style.display = 'inline'; document.getElementById('2412.04885v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.04885v1-abstract-full" style="display: none;"> The stability of weakly collisional plasmas is well represented by linear theory, and the generated waves play an essential role in the thermodynamics of these systems. The velocity distribution functions (VDF) characterizing kinetic particle behavior are commonly represented as a sum of anisotropic bi-Maxwellians. For the majority of in situ observations of solar wind plasmas enabled by heliospheric missions, a three bi-Maxwellian model is commonly applied for the ions, assuming that the VDF consists of a proton core, proton beam, and a single He ($伪$) particle population, each with their own density, bulk velocity, and anisotropic temperature. Resolving an $伪$-beam component was generally not possible due to instrumental limitations. The Solar Orbiter Solar Wind Analyser Proton and Alpha Sensor (SWA PAS) resolves velocity space with sufficient coverage and accuracy to routinely characterize secondary $伪$ populations consistently. This design makes the SWA PAS dataset ideal for examining effects of the $伪$-particle beam on the plasma's kinetic stability. We test the wave signatures observed in the magnetic field power spectrum at ion scales and compare them to the predictions from linear plasma theory, Doppler-shifted into the spacecraft reference frame. We find that taking into account the $伪$-particle beam component is necessary to predict the coherent wave signatures in the observed power spectra, emphasizing the importance of separating the $伪$-particle populations as is traditionally done for protons. Moreover, we demonstrate that the drifts of beam components are responsible for the majority of the modes that propagate in oblique direction to the magnetic field, while their temperature anisotropies are the primary source of parallel Fast Magnetosonic Modes in the solar wind. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.04885v1-abstract-full').style.display = 'none'; document.getElementById('2412.04885v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.00365">arXiv:2412.00365</a> <span> [<a href="https://arxiv.org/pdf/2412.00365">pdf</a>, <a href="https://arxiv.org/format/2412.00365">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> <p class="title is-5 mathjax"> Cross Helicity and the Helium Abundance as a Metric of Solar Wind Heating and Acceleration: Characterizing the Transition from Magnetically Closed to Magnetically Open Solar Wind Sources and Identifying the Origin of the Alf茅nic Slow Wind </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Alterman%2C+B+L">B. L. Alterman</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Amicis%2C+R">R. D'Amicis</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="2412.00365v1-abstract-short" style="display: inline;"> The two-state solar wind paradigm is based on observations showing that slow and fast solar wind have distinct properties like helium abundances, kinetic signatures, elemental composition, and charge-state ratios. Nominally, the fast wind originates from solar sources that are continuously magnetically open to the heliosphere like coronal holes while the slow wind is from solar sources that are on… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.00365v1-abstract-full').style.display = 'inline'; document.getElementById('2412.00365v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.00365v1-abstract-full" style="display: none;"> The two-state solar wind paradigm is based on observations showing that slow and fast solar wind have distinct properties like helium abundances, kinetic signatures, elemental composition, and charge-state ratios. Nominally, the fast wind originates from solar sources that are continuously magnetically open to the heliosphere like coronal holes while the slow wind is from solar sources that are only intermittently open to the heliosphere like helmet streamers and pseudostreamers. The Alfv茅nic slow wind is an emerging 3rd class of solar wind that challenges the two-state fast/slow paradigm. It has slow wind speeds but is highly Alfv茅nic, i.e. has a high correlation between velocity and magnetic field fluctuations along with low compressibility typical of Alfv茅n waves, which is typically observed in fast wind. Its other properties are also more similar to the fast than slow wind. From 28 years of Wind observations at 1 AU, we derive the solar wind helium abundance ($A_\mathrm{He}$), Alfv茅nicity ($\left|蟽_c\right|$), and solar wind speed ($v_\mathrm{sw}$). Characterizing vsw as a function of $\left|蟽_c\right|$ and $A_\mathrm{He}$, we show that the maximum solar wind speed for plasma accelerated in source regions that are intermittently open is faster than the minimum solar wind speed for plasma accelerated in continuously open regions. We infer that the Alfv茅nic slow wind is likely solar wind originating from open-field regions with speeds below the maximum solar wind speed for plasma from intermittently open regions. We then discuss possible implications for solar wind heating and acceleration. Finally, we utilize the combination of helium abundance and normalized cross helicity to present a novel solar wind categorization scheme. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.00365v1-abstract-full').style.display = 'none'; document.getElementById('2412.00365v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.16513">arXiv:2411.16513</a> <span> [<a href="https://arxiv.org/pdf/2411.16513">pdf</a>, <a href="https://arxiv.org/format/2411.16513">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> <p class="title is-5 mathjax"> Coronal hole picoflare jets are the progenitors of both the fast and the Alfv茅nic slow solar wind </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chitta%2C+L+P">L. P. Chitta</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+Z">Z. Huang</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Amicis%2C+R">R. D'Amicis</a>, <a href="/search/astro-ph?searchtype=author&query=Calchetti%2C+D">D. Calchetti</a>, <a href="/search/astro-ph?searchtype=author&query=Zhukov%2C+A+N">A. N. Zhukov</a>, <a href="/search/astro-ph?searchtype=author&query=Kraaikamp%2C+E">E. Kraaikamp</a>, <a href="/search/astro-ph?searchtype=author&query=Verbeeck%2C+C">C. Verbeeck</a>, <a href="/search/astro-ph?searchtype=author&query=Cuadrado%2C+R+A">R. Aznar Cuadrado</a>, <a href="/search/astro-ph?searchtype=author&query=Hirzberger%2C+J">J. Hirzberger</a>, <a href="/search/astro-ph?searchtype=author&query=Berghmans%2C+D">D. Berghmans</a>, <a href="/search/astro-ph?searchtype=author&query=Horbury%2C+T+S">T. S. Horbury</a>, <a href="/search/astro-ph?searchtype=author&query=Solanki%2C+S+K">S. K. Solanki</a>, <a href="/search/astro-ph?searchtype=author&query=Owen%2C+C+J">C. J. Owen</a>, <a href="/search/astro-ph?searchtype=author&query=Harra%2C+L">L. Harra</a>, <a href="/search/astro-ph?searchtype=author&query=Peter%2C+H">H. Peter</a>, <a href="/search/astro-ph?searchtype=author&query=Sch%C3%BChle%2C+U">U. Sch眉hle</a>, <a href="/search/astro-ph?searchtype=author&query=Teriaca%2C+L">L. Teriaca</a>, <a href="/search/astro-ph?searchtype=author&query=Louarn%2C+P">P. Louarn</a>, <a href="/search/astro-ph?searchtype=author&query=Livi%2C+S">S. Livi</a>, <a href="/search/astro-ph?searchtype=author&query=Giunta%2C+A+S">A. S. Giunta</a>, <a href="/search/astro-ph?searchtype=author&query=Hassler%2C+D+M">D. M. Hassler</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y+-">Y. -M. Wang</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="2411.16513v1-abstract-short" style="display: inline;"> The solar wind, classified by its bulk speed and the Alfv茅nic nature of its fluctuations, generates the heliosphere. The elusive physical processes responsible for the generation of the different types of the wind are a topic of active debate. Recent observations revealed intermittent jets with kinetic energy in the picoflare range, emerging from dark areas of a polar coronal hole threaded by open… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.16513v1-abstract-full').style.display = 'inline'; document.getElementById('2411.16513v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.16513v1-abstract-full" style="display: none;"> The solar wind, classified by its bulk speed and the Alfv茅nic nature of its fluctuations, generates the heliosphere. The elusive physical processes responsible for the generation of the different types of the wind are a topic of active debate. Recent observations revealed intermittent jets with kinetic energy in the picoflare range, emerging from dark areas of a polar coronal hole threaded by open magnetic field lines. These could substantially contribute to the solar wind. However, their ubiquity and direct links to the solar wind have not been established. Here we report a unique set of remote-sensing and in-situ observations from the Solar Orbiter spacecraft, that establish a unified picture of the fast and Alfv茅nic slow wind, connected to the similar widespread picoflare jet activity in two coronal holes. Radial expansion of coronal holes ultimately regulates the speed of the emerging wind. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.16513v1-abstract-full').style.display = 'none'; document.getElementById('2411.16513v1-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> 25 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">Accepted for publication in Astronomy and Astrophysics. Online animations available at https://owncloud.gwdg.de/index.php/s/ytjcW4Um1I6W2oZ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.10819">arXiv:2306.10819</a> <span> [<a href="https://arxiv.org/pdf/2306.10819">pdf</a>, <a href="https://arxiv.org/format/2306.10819">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> <p class="title is-5 mathjax"> Coronal Heating Rate in the Slow Solar Wind </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Telloni%2C+D">Daniele Telloni</a>, <a href="/search/astro-ph?searchtype=author&query=Romoli%2C+M">Marco Romoli</a>, <a href="/search/astro-ph?searchtype=author&query=Velli%2C+M">Marco Velli</a>, <a href="/search/astro-ph?searchtype=author&query=Zank%2C+G+P">Gary P. Zank</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+L">Laxman Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Downs%2C+C">Cooper Downs</a>, <a href="/search/astro-ph?searchtype=author&query=Burtovoi%2C+A">Aleksandr Burtovoi</a>, <a href="/search/astro-ph?searchtype=author&query=Susino%2C+R">Roberto Susino</a>, <a href="/search/astro-ph?searchtype=author&query=Spadaro%2C+D">Daniele Spadaro</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+L">Lingling Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Liberatore%2C+A">Alessandro Liberatore</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+C">Chen Shi</a>, <a href="/search/astro-ph?searchtype=author&query=De+Leo%2C+Y">Yara De Leo</a>, <a href="/search/astro-ph?searchtype=author&query=Abbo%2C+L">Lucia Abbo</a>, <a href="/search/astro-ph?searchtype=author&query=Frassati%2C+F">Federica Frassati</a>, <a href="/search/astro-ph?searchtype=author&query=Jerse%2C+G">Giovanna Jerse</a>, <a href="/search/astro-ph?searchtype=author&query=Landini%2C+F">Federico Landini</a>, <a href="/search/astro-ph?searchtype=author&query=Nicolini%2C+G">Gianalfredo Nicolini</a>, <a href="/search/astro-ph?searchtype=author&query=Pancrazzi%2C+M">Maurizio Pancrazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Russano%2C+G">Giuliana Russano</a>, <a href="/search/astro-ph?searchtype=author&query=Sasso%2C+C">Clementina Sasso</a>, <a href="/search/astro-ph?searchtype=author&query=Andretta%2C+V">Vincenzo Andretta</a>, <a href="/search/astro-ph?searchtype=author&query=Da+Deppo%2C+V">Vania Da Deppo</a>, <a href="/search/astro-ph?searchtype=author&query=Fineschi%2C+S">Silvano Fineschi</a>, <a href="/search/astro-ph?searchtype=author&query=Grimani%2C+C">Catia Grimani</a> , et al. (37 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="2306.10819v1-abstract-short" style="display: inline;"> This Letter reports the first observational estimate of the heating rate in the slowly expanding solar corona. The analysis exploits the simultaneous remote and local observations of the same coronal plasma volume with the Solar Orbiter/Metis and the Parker Solar Probe instruments, respectively, and relies on the basic solar wind magnetohydrodynamic equations. As expected, energy losses are a mino… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.10819v1-abstract-full').style.display = 'inline'; document.getElementById('2306.10819v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.10819v1-abstract-full" style="display: none;"> This Letter reports the first observational estimate of the heating rate in the slowly expanding solar corona. The analysis exploits the simultaneous remote and local observations of the same coronal plasma volume with the Solar Orbiter/Metis and the Parker Solar Probe instruments, respectively, and relies on the basic solar wind magnetohydrodynamic equations. As expected, energy losses are a minor fraction of the solar wind energy flux, since most of the energy dissipation that feeds the heating and acceleration of the coronal flow occurs much closer to the Sun than the heights probed in the present study, which range from 6.3 to 13.3 solar radii. The energy deposited to the supersonic wind is then used to explain the observed slight residual wind acceleration and to maintain the plasma in a non-adiabatic state. As derived in the Wentzel-Kramers-Brillouin limit, the present energy transfer rate estimates provide a lower limit, which can be very useful in refining the turbulence-based modeling of coronal heating and subsequent solar wind acceleration. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.10819v1-abstract-full').style.display = 'none'; document.getElementById('2306.10819v1-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> 19 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </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/2303.12192">arXiv:2303.12192</a> <span> [<a href="https://arxiv.org/pdf/2303.12192">pdf</a>, <a href="https://arxiv.org/format/2303.12192">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/acc653">10.3847/1538-4357/acc653 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observational Evidence of S-Web Source of the Slow Solar Wind </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Baker%2C+D">D. Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Demoulin%2C+P">P. Demoulin</a>, <a href="/search/astro-ph?searchtype=author&query=Yardley%2C+S+L">S. L. Yardley</a>, <a href="/search/astro-ph?searchtype=author&query=Mihailescu%2C+T">T. Mihailescu</a>, <a href="/search/astro-ph?searchtype=author&query=van+Driel-Gesztelyi%2C+L">L. van Driel-Gesztelyi</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Amicis%2C+R">R. D'Amicis</a>, <a href="/search/astro-ph?searchtype=author&query=Long%2C+D+M">D. M. Long</a>, <a href="/search/astro-ph?searchtype=author&query=To%2C+A+S+H">A. S. H. To</a>, <a href="/search/astro-ph?searchtype=author&query=Owen%2C+C+J">C. J. Owen</a>, <a href="/search/astro-ph?searchtype=author&query=Horbury%2C+T+S">T. S. Horbury</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D+H">D. H. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Perrone%2C+D">D. Perrone</a>, <a href="/search/astro-ph?searchtype=author&query=French%2C+R+J">R. J. French</a>, <a href="/search/astro-ph?searchtype=author&query=James%2C+A+W">A. W. James</a>, <a href="/search/astro-ph?searchtype=author&query=Janvier%2C+M">M. Janvier</a>, <a href="/search/astro-ph?searchtype=author&query=Matthews%2C+S">S. Matthews</a>, <a href="/search/astro-ph?searchtype=author&query=Stangalini%2C+M">M. Stangalini</a>, <a href="/search/astro-ph?searchtype=author&query=Valori%2C+G">G. Valori</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+P">P. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Cuadrado%2C+R+A">R. Anzar Cuadrado</a>, <a href="/search/astro-ph?searchtype=author&query=Peter%2C+H">H. Peter</a>, <a href="/search/astro-ph?searchtype=author&query=Schuehle%2C+U">U. Schuehle</a>, <a href="/search/astro-ph?searchtype=author&query=Harra%2C+L">L. Harra</a>, <a href="/search/astro-ph?searchtype=author&query=Barczynski%2C+K">K. Barczynski</a>, <a href="/search/astro-ph?searchtype=author&query=Berghmans%2C+D">D. Berghmans</a> , et al. (3 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="2303.12192v1-abstract-short" style="display: inline;"> From 2022 March 18-21, active region (AR) 12967 was tracked simultaneously by Solar Orbiter (SO) at 0.35 au and Hinode/EIS at Earth. During this period, strong blue-shifted plasma upflows were observed along a thin, dark corridor of open field originating at the AR's leading polarity and continuing towards the southern extension of the northern polar coronal hole. A potential field source surface… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.12192v1-abstract-full').style.display = 'inline'; document.getElementById('2303.12192v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.12192v1-abstract-full" style="display: none;"> From 2022 March 18-21, active region (AR) 12967 was tracked simultaneously by Solar Orbiter (SO) at 0.35 au and Hinode/EIS at Earth. During this period, strong blue-shifted plasma upflows were observed along a thin, dark corridor of open field originating at the AR's leading polarity and continuing towards the southern extension of the northern polar coronal hole. A potential field source surface (PFSS) model shows large lateral expansion of the open magnetic field along the corridor. Squashing factor Q-maps of the large scale topology further confirm super-radial expansion in support of the S-Web theory for the slow wind. The thin corridor of upflows is identified as the source region of a slow solar wind stream characterised by approx. 300 km s-1 velocities, low proton temperatures of approx. 5 eV, extremely high density over 100 cm-3, and a short interval of moderate Alfvenicity accompanied by switchback events. When connectivity changes from the corridor to the eastern side of the AR, the in situ plasma parameters of the slow wind indicate a distinctly different source region. These observations provide strong evidence that the narrow open field corridors, forming part of the S-Web, produce extreme properties in their associated solar wind streams. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.12192v1-abstract-full').style.display = 'none'; document.getElementById('2303.12192v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.10545">arXiv:2302.10545</a> <span> [<a href="https://arxiv.org/pdf/2302.10545">pdf</a>, <a href="https://arxiv.org/format/2302.10545">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/acb693">10.3847/1538-4357/acb693 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Does Turbulence along the Coronal Current Sheet Drive Ion Cyclotron Waves? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Telloni%2C+D">Daniele Telloni</a>, <a href="/search/astro-ph?searchtype=author&query=Zank%2C+G+P">Gary P. Zank</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+L">Laxman Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+L">Lingling Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Susino%2C+R">Roberto Susino</a>, <a href="/search/astro-ph?searchtype=author&query=Antonucci%2C+E">Ester Antonucci</a>, <a href="/search/astro-ph?searchtype=author&query=Fineschi%2C+S">Silvano Fineschi</a>, <a href="/search/astro-ph?searchtype=author&query=Stangalini%2C+M">Marco Stangalini</a>, <a href="/search/astro-ph?searchtype=author&query=Grimani%2C+C">Catia Grimani</a>, <a href="/search/astro-ph?searchtype=author&query=Sorriso-Valvo%2C+L">Luca Sorriso-Valvo</a>, <a href="/search/astro-ph?searchtype=author&query=Verscharen%2C+D">Daniel Verscharen</a>, <a href="/search/astro-ph?searchtype=author&query=Marino%2C+R">Raffaele Marino</a>, <a href="/search/astro-ph?searchtype=author&query=Giordano%2C+S">Silvio Giordano</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=Perrone%2C+D">Denise Perrone</a>, <a href="/search/astro-ph?searchtype=author&query=Carbone%2C+F">Francesco Carbone</a>, <a href="/search/astro-ph?searchtype=author&query=Liberatore%2C+A">Alessandro Liberatore</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+R">Roberto Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Zimbardo%2C+G">Gaetano Zimbardo</a>, <a href="/search/astro-ph?searchtype=author&query=Romoli%2C+M">Marco Romoli</a>, <a href="/search/astro-ph?searchtype=author&query=Andretta%2C+V">Vincenzo Andretta</a>, <a href="/search/astro-ph?searchtype=author&query=Da+Deppo%2C+V">Vania Da Deppo</a>, <a href="/search/astro-ph?searchtype=author&query=Heinzel%2C+P">Petr Heinzel</a>, <a href="/search/astro-ph?searchtype=author&query=Moses%2C+J+D">John D. Moses</a>, <a href="/search/astro-ph?searchtype=author&query=Naletto%2C+G">Giampiero Naletto</a> , et al. (10 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="2302.10545v1-abstract-short" style="display: inline;"> Evidence for the presence of ion cyclotron waves, driven by turbulence, at the boundaries of the current sheet is reported in this paper. By exploiting the full potential of the joint observations performed by Parker Solar Probe and the Metis coronagraph on board Solar Orbiter, local measurements of the solar wind can be linked with the large-scale structures of the solar corona. The results sugge… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.10545v1-abstract-full').style.display = 'inline'; document.getElementById('2302.10545v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.10545v1-abstract-full" style="display: none;"> Evidence for the presence of ion cyclotron waves, driven by turbulence, at the boundaries of the current sheet is reported in this paper. By exploiting the full potential of the joint observations performed by Parker Solar Probe and the Metis coronagraph on board Solar Orbiter, local measurements of the solar wind can be linked with the large-scale structures of the solar corona. The results suggest that the dynamics of the current sheet layers generates turbulence, which in turn creates a sufficiently strong temperature anisotropy to make the solar-wind plasma unstable to anisotropy-driven instabilities such as the Alfv茅n ion-cyclotron, mirror-mode, and firehose instabilities. The study of the polarization state of high-frequency magnetic fluctuations reveals that ion cyclotron waves are indeed present along the current sheet, thus linking the magnetic topology of the remotely imaged coronal source regions with the wave bursts observed in situ. The present results may allow improvement of state-of-the-art models based on the ion cyclotron mechanism, providing new insights into the processes involved in coronal heating. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.10545v1-abstract-full').style.display = 'none'; document.getElementById('2302.10545v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, 2023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.02727">arXiv:2301.02727</a> <span> [<a href="https://arxiv.org/pdf/2301.02727">pdf</a>, <a href="https://arxiv.org/format/2301.02727">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/10.1007/s11214-023-00952-4">10.1007/s11214-023-00952-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Parker Solar Probe: Four Years of Discoveries at Solar Cycle Minimum </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Raouafi%2C+N+E">N. E. Raouafi</a>, <a href="/search/astro-ph?searchtype=author&query=Matteini%2C+L">L. Matteini</a>, <a href="/search/astro-ph?searchtype=author&query=Squire%2C+J">J. Squire</a>, <a href="/search/astro-ph?searchtype=author&query=Badman%2C+S+T">S. T. Badman</a>, <a href="/search/astro-ph?searchtype=author&query=Velli%2C+M">M. Velli</a>, <a href="/search/astro-ph?searchtype=author&query=Klein%2C+K+G">K. G. Klein</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+C+H+K">C. H. K. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Matthaeus%2C+W+H">W. H. Matthaeus</a>, <a href="/search/astro-ph?searchtype=author&query=Szabo%2C+A">A. Szabo</a>, <a href="/search/astro-ph?searchtype=author&query=Linton%2C+M">M. Linton</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+R+C">R. C. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Szalay%2C+J+R">J. R. Szalay</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+R">R. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Decker%2C+R+B">R. B. Decker</a>, <a href="/search/astro-ph?searchtype=author&query=Akhavan-Tafti%2C+M">M. Akhavan-Tafti</a>, <a href="/search/astro-ph?searchtype=author&query=Agapitov%2C+O+V">O. V. Agapitov</a>, <a href="/search/astro-ph?searchtype=author&query=Bale%2C+S+D">S. D. Bale</a>, <a href="/search/astro-ph?searchtype=author&query=Bandyopadhyay%2C+R">R. Bandyopadhyay</a>, <a href="/search/astro-ph?searchtype=author&query=Battams%2C+K">K. Battams</a>, <a href="/search/astro-ph?searchtype=author&query=Ber%C4%8Di%C4%8D%2C+L">L. Ber膷i膷</a>, <a href="/search/astro-ph?searchtype=author&query=Bourouaine%2C+S">S. Bourouaine</a>, <a href="/search/astro-ph?searchtype=author&query=Bowen%2C+T">T. Bowen</a>, <a href="/search/astro-ph?searchtype=author&query=Cattell%2C+C">C. Cattell</a>, <a href="/search/astro-ph?searchtype=author&query=Chandran%2C+B+D+G">B. D. G. Chandran</a>, <a href="/search/astro-ph?searchtype=author&query=Chhiber%2C+R">R. Chhiber</a> , et al. (32 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="2301.02727v1-abstract-short" style="display: inline;"> Launched on 12 Aug. 2018, NASA's Parker Solar Probe had completed 13 of its scheduled 24 orbits around the Sun by Nov. 2022. The mission's primary science goal is to determine the structure and dynamics of the Sun's coronal magnetic field, understand how the solar corona and wind are heated and accelerated, and determine what processes accelerate energetic particles. Parker Solar Probe returned a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.02727v1-abstract-full').style.display = 'inline'; document.getElementById('2301.02727v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.02727v1-abstract-full" style="display: none;"> Launched on 12 Aug. 2018, NASA's Parker Solar Probe had completed 13 of its scheduled 24 orbits around the Sun by Nov. 2022. The mission's primary science goal is to determine the structure and dynamics of the Sun's coronal magnetic field, understand how the solar corona and wind are heated and accelerated, and determine what processes accelerate energetic particles. Parker Solar Probe returned a treasure trove of science data that far exceeded quality, significance, and quantity expectations, leading to a significant number of discoveries reported in nearly 700 peer-reviewed publications. The first four years of the 7-year primary mission duration have been mostly during solar minimum conditions with few major solar events. Starting with orbit 8 (i.e., 28 Apr. 2021), Parker flew through the magnetically dominated corona, i.e., sub-Alfv茅nic solar wind, which is one of the mission's primary objectives. In this paper, we present an overview of the scientific advances made mainly during the first four years of the Parker Solar Probe mission, which go well beyond the three science objectives that are: (1) Trace the flow of energy that heats and accelerates the solar corona and solar wind; (2) Determine the structure and dynamics of the plasma and magnetic fields at the sources of the solar wind; and (3) Explore mechanisms that accelerate and transport energetic particles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.02727v1-abstract-full').style.display = 'none'; document.getElementById('2301.02727v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 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">157 pages, 65 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Space Science Reviews 2023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.16972">arXiv:2211.16972</a> <span> [<a href="https://arxiv.org/pdf/2211.16972">pdf</a>, <a href="https://arxiv.org/format/2211.16972">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/10.3847/1538-4357/acb93c">10.3847/1538-4357/acb93c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First analysis of in-situ observation of surface Alfv茅n waves in ICME flux rope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Raghav%2C+A">Anil Raghav</a>, <a href="/search/astro-ph?searchtype=author&query=Dhamane%2C+O">Omkar Dhamane</a>, <a href="/search/astro-ph?searchtype=author&query=Shaikh%2C+Z">Zubair Shaikh</a>, <a href="/search/astro-ph?searchtype=author&query=Azmi%2C+N">Naba Azmi</a>, <a href="/search/astro-ph?searchtype=author&query=Manjrekar%2C+A">Ankita Manjrekar</a>, <a href="/search/astro-ph?searchtype=author&query=Panchal%2C+U">Utsav Panchal</a>, <a href="/search/astro-ph?searchtype=author&query=Ghag%2C+K">Kalpesh Ghag</a>, <a href="/search/astro-ph?searchtype=author&query=Telloni%2C+D">Daniele Telloni</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=Tari%2C+P">Prathmesh Tari</a>, <a href="/search/astro-ph?searchtype=author&query=Gurav%2C+A">Akshata Gurav</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.16972v3-abstract-short" style="display: inline;"> Alfv茅n waves (AWs) are inevitable in space and astrophysical plasma. Their crucial role in various physical processes, occurring in plasma, has triggered intense research in solar-terrestrial physics. Simulation studies have proposed the generation of AWs along the surface of a cylindrical flux rope, referred to as Surface AWs (SAWs); however the observational verification of this distinct wave ha… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.16972v3-abstract-full').style.display = 'inline'; document.getElementById('2211.16972v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.16972v3-abstract-full" style="display: none;"> Alfv茅n waves (AWs) are inevitable in space and astrophysical plasma. Their crucial role in various physical processes, occurring in plasma, has triggered intense research in solar-terrestrial physics. Simulation studies have proposed the generation of AWs along the surface of a cylindrical flux rope, referred to as Surface AWs (SAWs); however the observational verification of this distinct wave has been elusive to date. We report the first \textit{in-situ} observation of SAWs in an interplanetary coronal mass ejection flux rope. We apply the Wal茅n test to identify them. The Elsasser variables are used to estimate the characterization of these SAWs. They may be excited by the movement of the flux rope's foot points or by instabilities along the plasma magnetic cloud's boundaries. Here, the change in plasma density or field strength in the surface-aligned magnetic field may trigger SAWs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.16972v3-abstract-full').style.display = 'none'; document.getElementById('2211.16972v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.03090">arXiv:2206.03090</a> <span> [<a href="https://arxiv.org/pdf/2206.03090">pdf</a>, <a href="https://arxiv.org/format/2206.03090">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/10.3847/2041-8213/ac8104">10.3847/2041-8213/ac8104 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observation of Magnetic Switchback in the Solar Corona </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Telloni%2C+D">Daniele Telloni</a>, <a href="/search/astro-ph?searchtype=author&query=Zank%2C+G+P">Gary P. Zank</a>, <a href="/search/astro-ph?searchtype=author&query=Stangalini%2C+M">Marco Stangalini</a>, <a href="/search/astro-ph?searchtype=author&query=Downs%2C+C">Cooper Downs</a>, <a href="/search/astro-ph?searchtype=author&query=Liang%2C+H">Haoming Liang</a>, <a href="/search/astro-ph?searchtype=author&query=Nakanotani%2C+M">Masaru Nakanotani</a>, <a href="/search/astro-ph?searchtype=author&query=Andretta%2C+V">Vincenzo Andretta</a>, <a href="/search/astro-ph?searchtype=author&query=Antonucci%2C+E">Ester Antonucci</a>, <a href="/search/astro-ph?searchtype=author&query=Sorriso-Valvo%2C+L">Luca Sorriso-Valvo</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+L">Laxman Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+L">Lingling Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Marino%2C+R">Raffaele Marino</a>, <a href="/search/astro-ph?searchtype=author&query=Susino%2C+R">Roberto Susino</a>, <a href="/search/astro-ph?searchtype=author&query=Grimani%2C+C">Catia Grimani</a>, <a href="/search/astro-ph?searchtype=author&query=Fabi%2C+M">Michele Fabi</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=Perrone%2C+D">Denise Perrone</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+R">Roberto Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Carbone%2C+F">Francesco Carbone</a>, <a href="/search/astro-ph?searchtype=author&query=Mancuso%2C+S">Salvatore Mancuso</a>, <a href="/search/astro-ph?searchtype=author&query=Romoli%2C+M">Marco Romoli</a>, <a href="/search/astro-ph?searchtype=author&query=Da+Deppo%2C+V">Vania Da Deppo</a>, <a href="/search/astro-ph?searchtype=author&query=Fineschi%2C+S">Silvano Fineschi</a>, <a href="/search/astro-ph?searchtype=author&query=Heinzel%2C+P">Petr Heinzel</a>, <a href="/search/astro-ph?searchtype=author&query=Moses%2C+J+D">John D. Moses</a> , et al. (27 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="2206.03090v2-abstract-short" style="display: inline;"> Switchbacks are sudden, large radial deflections of the solar wind magnetic field, widely revealed in interplanetary space by the Parker Solar Probe. The switchbacks' formation mechanism and sources are still unresolved, although candidate mechanisms include Alfv茅nic turbulence, shear-driven Kelvin-Helmholtz instabilities, interchange reconnection, and geometrical effects related to the Parker spi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.03090v2-abstract-full').style.display = 'inline'; document.getElementById('2206.03090v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.03090v2-abstract-full" style="display: none;"> Switchbacks are sudden, large radial deflections of the solar wind magnetic field, widely revealed in interplanetary space by the Parker Solar Probe. The switchbacks' formation mechanism and sources are still unresolved, although candidate mechanisms include Alfv茅nic turbulence, shear-driven Kelvin-Helmholtz instabilities, interchange reconnection, and geometrical effects related to the Parker spiral. This Letter presents observations from the Metis coronagraph onboard Solar Orbiter of a single large propagating S-shaped vortex, interpreted as first evidence of a switchback in the solar corona. It originated above an active region with the related loop system bounded by open-field regions to the East and West. Observations, modeling, and theory provide strong arguments in favor of the interchange reconnection origin of switchbacks. Metis measurements suggest that the initiation of the switchback may also be an indicator of the origin of slow solar wind. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.03090v2-abstract-full').style.display = 'none'; document.getElementById('2206.03090v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.11232">arXiv:2109.11232</a> <span> [<a href="https://arxiv.org/pdf/2109.11232">pdf</a>, <a href="https://arxiv.org/format/2109.11232">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/10.1051/0004-6361/202141149">10.1051/0004-6361/202141149 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Magnetic reconnection as a mechanism to produce multiple protonpopulations and beams locally in the solar wind </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lavraud%2C+B">B. Lavraud</a>, <a href="/search/astro-ph?searchtype=author&query=Kieokaew%2C+R">R. Kieokaew</a>, <a href="/search/astro-ph?searchtype=author&query=Fargette%2C+N">N. Fargette</a>, <a href="/search/astro-ph?searchtype=author&query=Louarn%2C+P">P. Louarn</a>, <a href="/search/astro-ph?searchtype=author&query=Fedorov%2C+A">A. Fedorov</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+N">N. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Fruit%2C+G">G. Fruit</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%A9not%2C+V">V. G茅not</a>, <a href="/search/astro-ph?searchtype=author&query=R%C3%A9ville%2C+V">V. R茅ville</a>, <a href="/search/astro-ph?searchtype=author&query=Rouillard%2C+A+P">A. P. Rouillard</a>, <a href="/search/astro-ph?searchtype=author&query=Plotnikov%2C+I">I. Plotnikov</a>, <a href="/search/astro-ph?searchtype=author&query=Penou%2C+E">E. Penou</a>, <a href="/search/astro-ph?searchtype=author&query=Barthe%2C+A">A. Barthe</a>, <a href="/search/astro-ph?searchtype=author&query=Prech%2C+L">L. Prech</a>, <a href="/search/astro-ph?searchtype=author&query=Owen%2C+C+J">C. J. Owen</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+R">R. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Allegrini%2C+F">F. Allegrini</a>, <a href="/search/astro-ph?searchtype=author&query=Berthomier%2C+M">M. Berthomier</a>, <a href="/search/astro-ph?searchtype=author&query=Kataria%2C+D">D. Kataria</a>, <a href="/search/astro-ph?searchtype=author&query=Livi%2C+S">S. Livi</a>, <a href="/search/astro-ph?searchtype=author&query=Raines%2C+J+M">J. M. Raines</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Amicis%2C+R">R. D'Amicis</a>, <a href="/search/astro-ph?searchtype=author&query=Eastwood%2C+J+P">J. P. Eastwood</a>, <a href="/search/astro-ph?searchtype=author&query=Froment%2C+C">C. Froment</a>, <a href="/search/astro-ph?searchtype=author&query=Laker%2C+R">R. Laker</a> , et al. (15 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="2109.11232v1-abstract-short" style="display: inline;"> Context. Spacecraft observations early revealed frequent multiple proton populations in the solar wind. Decades of research on their origin have focused on processes such as magnetic reconnection in the low corona and wave-particle interactions in the corona and locally in the solar wind.Aims.This study aims to highlight that multiple proton populations and beams are also produced by magnetic reco… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.11232v1-abstract-full').style.display = 'inline'; document.getElementById('2109.11232v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.11232v1-abstract-full" style="display: none;"> Context. Spacecraft observations early revealed frequent multiple proton populations in the solar wind. Decades of research on their origin have focused on processes such as magnetic reconnection in the low corona and wave-particle interactions in the corona and locally in the solar wind.Aims.This study aims to highlight that multiple proton populations and beams are also produced by magnetic reconnection occurring locally in the solar wind. Methods. We use high resolution Solar Orbiter proton velocity distribution function measurements, complemented by electron and magnetic field data, to analyze the association of multiple proton populations and beams with magnetic reconnection during a period of slow Alfv茅nic solar wind on 16 July 2020. Results. At least 6 reconnecting current sheets with associated multiple proton populations and beams, including a case of magnetic reconnection at a switchback boundary, are found during this day. This represents 2% of the measured distribution functions. We discuss how this proportion may be underestimated, and how it may depend on solar wind type and distance from the Sun. Conclusions. Although suggesting a likely small contribution, but which remains to be quantitatively assessed, Solar Orbiter observations show that magnetic reconnection must be considered as one of the mechanisms that produce multiple proton populations and beams locally in the solar wind. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.11232v1-abstract-full').style.display = 'none'; document.getElementById('2109.11232v1-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 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.13344">arXiv:2106.13344</a> <span> [<a href="https://arxiv.org/pdf/2106.13344">pdf</a>, <a href="https://arxiv.org/format/2106.13344">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/10.1051/0004-6361/202140980">10.1051/0004-6361/202140980 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First light observations of the solar wind in the outer corona with the Metis coronagraph </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Romoli%2C+M">M. Romoli</a>, <a href="/search/astro-ph?searchtype=author&query=Antonucci%2C+E">E. Antonucci</a>, <a href="/search/astro-ph?searchtype=author&query=Andretta%2C+V">V. Andretta</a>, <a href="/search/astro-ph?searchtype=author&query=Capuano%2C+G+E">G. E. Capuano</a>, <a href="/search/astro-ph?searchtype=author&query=Da+Deppo%2C+V">V. Da Deppo</a>, <a href="/search/astro-ph?searchtype=author&query=De+Leo%2C+Y">Y. De Leo</a>, <a href="/search/astro-ph?searchtype=author&query=Downs%2C+C">C. Downs</a>, <a href="/search/astro-ph?searchtype=author&query=Fineschi%2C+S">S. Fineschi</a>, <a href="/search/astro-ph?searchtype=author&query=Heinzel%2C+P">P. Heinzel</a>, <a href="/search/astro-ph?searchtype=author&query=Landini%2C+F">F. Landini</a>, <a href="/search/astro-ph?searchtype=author&query=Liberatore%2C+A">A. Liberatore</a>, <a href="/search/astro-ph?searchtype=author&query=Naletto%2C+G">G. Naletto</a>, <a href="/search/astro-ph?searchtype=author&query=Nicolini%2C+G">G. Nicolini</a>, <a href="/search/astro-ph?searchtype=author&query=Pancrazzi%2C+M">M. Pancrazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Sasso%2C+C">C. Sasso</a>, <a href="/search/astro-ph?searchtype=author&query=Spadaro%2C+D">D. Spadaro</a>, <a href="/search/astro-ph?searchtype=author&query=Susino%2C+R">R. Susino</a>, <a href="/search/astro-ph?searchtype=author&query=Telloni%2C+D">D. Telloni</a>, <a href="/search/astro-ph?searchtype=author&query=Teriaca%2C+L">L. Teriaca</a>, <a href="/search/astro-ph?searchtype=author&query=Uslenghi%2C+M">M. Uslenghi</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y+M">Y. M. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Bemporad%2C+A">A. Bemporad</a>, <a href="/search/astro-ph?searchtype=author&query=Capobianco%2C+G">G. Capobianco</a>, <a href="/search/astro-ph?searchtype=author&query=Casti%2C+M">M. Casti</a>, <a href="/search/astro-ph?searchtype=author&query=Fabi%2C+M">M. Fabi</a> , et al. (43 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="2106.13344v1-abstract-short" style="display: inline;"> The investigation of the wind in the solar corona initiated with the observations of the resonantly scattered UV emission of the coronal plasma obtained with UVCS-SOHO, designed to measure the wind outflow speed by applying the Doppler dimming diagnostics. Metis on Solar Orbiter complements the UVCS spectroscopic observations, performed during solar activity cycle 23, by simultaneously imaging the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.13344v1-abstract-full').style.display = 'inline'; document.getElementById('2106.13344v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.13344v1-abstract-full" style="display: none;"> The investigation of the wind in the solar corona initiated with the observations of the resonantly scattered UV emission of the coronal plasma obtained with UVCS-SOHO, designed to measure the wind outflow speed by applying the Doppler dimming diagnostics. Metis on Solar Orbiter complements the UVCS spectroscopic observations, performed during solar activity cycle 23, by simultaneously imaging the polarized visible light and the HI Ly-alpha corona in order to obtain high-spatial and temporal resolution maps of the outward velocity of the continuously expanding solar atmosphere. The Metis observations, on May 15, 2020, provide the first HI Ly-alpha images of the extended corona and the first instantaneous map of the speed of the coronal plasma outflows during the minimum of solar activity and allow us to identify the layer where the slow wind flow is observed. The polarized visible light (580-640 nm), and the UV HI Ly-alpha (121.6 nm) coronal emissions, obtained with the two Metis channels, are combined in order to measure the dimming of the UV emission relative to a static corona. This effect is caused by the outward motion of the coronal plasma along the direction of incidence of the chromospheric photons on the coronal neutral hydrogen. The plasma outflow velocity is then derived as a function of the measured Doppler dimming. The static corona UV emission is simulated on the basis of the plasma electron density inferred from the polarized visible light. This study leads to the identification, in the velocity maps of the solar corona, of the high-density layer about +/-10 deg wide, centered on the extension of a quiet equatorial streamer present at the East limb where the slowest wind flows at about (160 +/- 18) km/s from 4 Rs to 6 Rs. Beyond the boundaries of the high-density layer, the wind velocity rapidly increases, marking the transition between slow and fast wind in the corona. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.13344v1-abstract-full').style.display = 'none'; document.getElementById('2106.13344v1-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> 24 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A, 2021, Forthcoming article </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.02578">arXiv:2010.02578</a> <span> [<a href="https://arxiv.org/pdf/2010.02578">pdf</a>, <a href="https://arxiv.org/ps/2010.02578">ps</a>, <a href="https://arxiv.org/format/2010.02578">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/10.3847/1538-4357/abc480">10.3847/1538-4357/abc480 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Coherent events at ion scales in the inner Heliosphere: \textit{Parker Solar Probe} observations during the first Encounter </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Perrone%2C+D">Denise Perrone</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+R">Roberto Bruno</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=Telloni%2C+D">Daniele Telloni</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marco%2C+R">Rossana De Marco</a>, <a href="/search/astro-ph?searchtype=author&query=Stangalini%2C+M">Marco Stangalini</a>, <a href="/search/astro-ph?searchtype=author&query=Perri%2C+S">Silvia Perri</a>, <a href="/search/astro-ph?searchtype=author&query=Pezzi%2C+O">Oreste Pezzi</a>, <a href="/search/astro-ph?searchtype=author&query=Alexandrova%2C+O">Olga Alexandrova</a>, <a href="/search/astro-ph?searchtype=author&query=Bale%2C+S+D">Stuart D. Bale</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="2010.02578v1-abstract-short" style="display: inline;"> \textit{Parker Solar Probe} has shown the ubiquitous presence of strong magnetic field deflections, namely switchbacks, during its first perihelion where it was embedded in a highly Alfv茅nic slow stream. Here, we study the turbulent magnetic fluctuations around ion scales in three intervals characterized by a different switchback activity, identified by the behaviour of the magnetic field radial c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.02578v1-abstract-full').style.display = 'inline'; document.getElementById('2010.02578v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.02578v1-abstract-full" style="display: none;"> \textit{Parker Solar Probe} has shown the ubiquitous presence of strong magnetic field deflections, namely switchbacks, during its first perihelion where it was embedded in a highly Alfv茅nic slow stream. Here, we study the turbulent magnetic fluctuations around ion scales in three intervals characterized by a different switchback activity, identified by the behaviour of the magnetic field radial component, $B_r$. \textit{Quiet} ($B_r$ does not show significant fluctuations), \textit{weak} ($B_r$ has strong fluctuations but no reversals) and \textit{strong} ($B_r$ has full reversals) periods show a different behaviour also for ion quantities and Alfv茅nicity. However, the spectral analysis shows that each stream is characterized by the typical Kolmogorov/Kraichnan power law in the inertial range, followed by a break around the characteristic ion scales. This frequency range is characterized by strong intermittent activity, with the presence of non-compressive coherent structures, such as current sheets and vortex-like structures, and wave packets, identified as ion cyclotron modes. Although, all these intermittent events have been detected in the three periods, they have a different influence in each of them. Current sheets are dominant in the \textit{strong} period, wave packets are the most common in the \textit{quiet} interval; while, in the \textit{weak} period, a mixture of vortices and wave packets is observed. This work provides an insight into the heating problem in collisionless plasmas, fitting in the context of the new solar missions, and, especially for \textit{Solar Orbiter}, which will allow an accurate magnetic connectivity analysis, to link the presence of different intermittent events to the source region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.02578v1-abstract-full').style.display = 'none'; document.getElementById('2010.02578v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.10772">arXiv:2009.10772</a> <span> [<a href="https://arxiv.org/pdf/2009.10772">pdf</a>, <a href="https://arxiv.org/format/2009.10772">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202038445">10.1051/0004-6361/202038445 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Solar Orbiter Science Activity Plan: translating solar and heliospheric physics questions into action </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zouganelis%2C+I">I. Zouganelis</a>, <a href="/search/astro-ph?searchtype=author&query=De+Groof%2C+A">A. De Groof</a>, <a href="/search/astro-ph?searchtype=author&query=Walsh%2C+A+P">A. P. Walsh</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+D+R">D. R. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Mueller%2C+D">D. Mueller</a>, <a href="/search/astro-ph?searchtype=author&query=Cyr%2C+O+C+S">O. C. St Cyr</a>, <a href="/search/astro-ph?searchtype=author&query=Auchere%2C+F">F. Auchere</a>, <a href="/search/astro-ph?searchtype=author&query=Berghmans%2C+D">D. Berghmans</a>, <a href="/search/astro-ph?searchtype=author&query=Fludra%2C+A">A. Fludra</a>, <a href="/search/astro-ph?searchtype=author&query=Horbury%2C+T+S">T. S. Horbury</a>, <a href="/search/astro-ph?searchtype=author&query=Howard%2C+R+A">R. A. Howard</a>, <a href="/search/astro-ph?searchtype=author&query=Krucker%2C+S">S. Krucker</a>, <a href="/search/astro-ph?searchtype=author&query=Maksimovic%2C+M">M. Maksimovic</a>, <a href="/search/astro-ph?searchtype=author&query=Owen%2C+C+J">C. J. Owen</a>, <a href="/search/astro-ph?searchtype=author&query=Rodriiguez-Pacheco%2C+J">J. Rodriiguez-Pacheco</a>, <a href="/search/astro-ph?searchtype=author&query=Romoli%2C+M">M. Romoli</a>, <a href="/search/astro-ph?searchtype=author&query=Solanki%2C+S+K">S. K. Solanki</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+C">C. Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez%2C+L">L. Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Lefort%2C+J">J. Lefort</a>, <a href="/search/astro-ph?searchtype=author&query=Osuna%2C+P">P. Osuna</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+H+R">H. R. Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Nieves-Chinchilla%2C+T">T. Nieves-Chinchilla</a>, <a href="/search/astro-ph?searchtype=author&query=Abbo%2C+L">L. Abbo</a>, <a href="/search/astro-ph?searchtype=author&query=Alexandrova%2C+O">O. Alexandrova</a> , et al. (160 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="2009.10772v1-abstract-short" style="display: inline;"> Solar Orbiter is the first space mission observing the solar plasma both in situ and remotely, from a close distance, in and out of the ecliptic. The ultimate goal is to understand how the Sun produces and controls the heliosphere, filling the Solar System and driving the planetary environments. With six remote-sensing and four in-situ instrument suites, the coordination and planning of the operat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.10772v1-abstract-full').style.display = 'inline'; document.getElementById('2009.10772v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.10772v1-abstract-full" style="display: none;"> Solar Orbiter is the first space mission observing the solar plasma both in situ and remotely, from a close distance, in and out of the ecliptic. The ultimate goal is to understand how the Sun produces and controls the heliosphere, filling the Solar System and driving the planetary environments. With six remote-sensing and four in-situ instrument suites, the coordination and planning of the operations are essential to address the following four top-level science questions: (1) What drives the solar wind and where does the coronal magnetic field originate? (2) How do solar transients drive heliospheric variability? (3) How do solar eruptions produce energetic particle radiation that fills the heliosphere? (4) How does the solar dynamo work and drive connections between the Sun and the heliosphere? Maximising the mission's science return requires considering the characteristics of each orbit, including the relative position of the spacecraft to Earth (affecting downlink rates), trajectory events (such as gravitational assist manoeuvres), and the phase of the solar activity cycle. Furthermore, since each orbit's science telemetry will be downloaded over the course of the following orbit, science operations must be planned at mission level, rather than at the level of individual orbits. It is important to explore the way in which those science questions are translated into an actual plan of observations that fits into the mission, thus ensuring that no opportunities are missed. First, the overarching goals are broken down into specific, answerable questions along with the required observations and the so-called Science Activity Plan (SAP) is developed to achieve this. The SAP groups objectives that require similar observations into Solar Orbiter Observing Plans (SOOPs), resulting in a strategic, top-level view of the optimal opportunities for science observations during the mission lifetime. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.10772v1-abstract-full').style.display = 'none'; document.getElementById('2009.10772v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">20 pages, 1 figure, accepted by Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 642, A3 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1911.08462">arXiv:1911.08462</a> <span> [<a href="https://arxiv.org/pdf/1911.08462">pdf</a>, <a href="https://arxiv.org/format/1911.08462">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201935338">10.1051/0004-6361/201935338 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Metis: the Solar Orbiter visible light and ultraviolet coronal imager </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Antonucci%2C+E">Ester Antonucci</a>, <a href="/search/astro-ph?searchtype=author&query=Romoli%2C+M">Marco Romoli</a>, <a href="/search/astro-ph?searchtype=author&query=Andretta%2C+V">Vincenzo Andretta</a>, <a href="/search/astro-ph?searchtype=author&query=Fineschi%2C+S">Silvano Fineschi</a>, <a href="/search/astro-ph?searchtype=author&query=Heinzel%2C+P">Petr Heinzel</a>, <a href="/search/astro-ph?searchtype=author&query=Moses%2C+J+D">J. Daniel Moses</a>, <a href="/search/astro-ph?searchtype=author&query=Naletto%2C+G">Giampiero Naletto</a>, <a href="/search/astro-ph?searchtype=author&query=Nicolini%2C+G">Gianalfredo Nicolini</a>, <a href="/search/astro-ph?searchtype=author&query=Spadaro%2C+D">Daniele Spadaro</a>, <a href="/search/astro-ph?searchtype=author&query=Teriaca%2C+L">Luca Teriaca</a>, <a href="/search/astro-ph?searchtype=author&query=Berlicki%2C+A">Arkadiusz Berlicki</a>, <a href="/search/astro-ph?searchtype=author&query=Capobianco%2C+G">Gerardo Capobianco</a>, <a href="/search/astro-ph?searchtype=author&query=Crescenzio%2C+G">Giuseppe Crescenzio</a>, <a href="/search/astro-ph?searchtype=author&query=Da+Deppo%2C+V">Vania Da Deppo</a>, <a href="/search/astro-ph?searchtype=author&query=Focardi%2C+M">Mauro Focardi</a>, <a href="/search/astro-ph?searchtype=author&query=Frassetto%2C+F">Fabio Frassetto</a>, <a href="/search/astro-ph?searchtype=author&query=Heerlein%2C+K">Klaus Heerlein</a>, <a href="/search/astro-ph?searchtype=author&query=Landini%2C+F">Federico Landini</a>, <a href="/search/astro-ph?searchtype=author&query=Magli%2C+E">Enrico Magli</a>, <a href="/search/astro-ph?searchtype=author&query=Malvezzi%2C+A+M">Andrea Marco Malvezzi</a>, <a href="/search/astro-ph?searchtype=author&query=Massone%2C+G">Giuseppe Massone</a>, <a href="/search/astro-ph?searchtype=author&query=Melich%2C+R">Radek Melich</a>, <a href="/search/astro-ph?searchtype=author&query=Nicolosi%2C+P">Piergiorgio Nicolosi</a>, <a href="/search/astro-ph?searchtype=author&query=Noci%2C+G">Giancarlo Noci</a>, <a href="/search/astro-ph?searchtype=author&query=Pancrazzi%2C+M">Maurizio Pancrazzi</a> , et al. (78 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="1911.08462v1-abstract-short" style="display: inline;"> Metis is the first solar coronagraph designed for a space mission capable of performing simultaneous imaging of the off-limb solar corona in both visible and UV light. The observations obtained with Metis aboard the Solar Orbiter ESA-NASA observatory will enable us to diagnose, with unprecedented temporal coverage and spatial resolution, the structures and dynamics of the full corona from 1.7… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.08462v1-abstract-full').style.display = 'inline'; document.getElementById('1911.08462v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.08462v1-abstract-full" style="display: none;"> Metis is the first solar coronagraph designed for a space mission capable of performing simultaneous imaging of the off-limb solar corona in both visible and UV light. The observations obtained with Metis aboard the Solar Orbiter ESA-NASA observatory will enable us to diagnose, with unprecedented temporal coverage and spatial resolution, the structures and dynamics of the full corona from 1.7 $R_\odot$ to about 9 $R_\odot$. Due to the uniqueness of the Solar Orbiter mission profile, Metis will be able to observe the solar corona from a close vantage point (down to 0.28 AU), achieving out-of-ecliptic views with the increase of the orbit inclination over time. Moreover, observations near perihelion, during the phase of lower rotational velocity of the solar surface relative to the spacecraft, will allow longer-term studies of the coronal features. Thanks to a novel occultation design and a combination of a UV interference coating of the mirrors and a spectral bandpass filter, Metis images the solar corona simultaneously in the visible light band, between 580 and 640 nm, and in the UV H I Lyman-伪 line at 121.6 nm. The coronal images in both the UV Lyman-伪 and polarised visible light are obtained at high spatial resolution with a spatial scale down to about 2000 km and 15000 km at perihelion, in the cases of the visible and UV light, respectively. A temporal resolution down to 1 second can be achieved when observing coronal fluctuations in visible light. The Metis measurements will allow for complete characterisation of the main physical parameters and dynamics of the electron and neutral hydrogen/proton plasma components of the corona in the region where the solar wind undergoes acceleration and where the onset and initial propagation of coronal mass ejections take place, thus significantly improving our understanding of the region connecting the Sun to the heliosphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.08462v1-abstract-full').style.display = 'none'; document.getElementById('1911.08462v1-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 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.02206">arXiv:1908.02206</a> <span> [<a href="https://arxiv.org/pdf/1908.02206">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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> </div> </div> <p class="title is-5 mathjax"> A Case for Electron-Astrophysics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Verscharen%2C+D">Daniel Verscharen</a>, <a href="/search/astro-ph?searchtype=author&query=Wicks%2C+R+T">Robert T. Wicks</a>, <a href="/search/astro-ph?searchtype=author&query=Alexandrova%2C+O">Olga Alexandrova</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+R">Roberto Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Burgess%2C+D">David Burgess</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+C+H+K">Christopher H. K. Chen</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=De+Keyser%2C+J">Johan De Keyser</a>, <a href="/search/astro-ph?searchtype=author&query=de+Wit%2C+T+D">Thierry Dudok de Wit</a>, <a href="/search/astro-ph?searchtype=author&query=Franci%2C+L">Luca Franci</a>, <a href="/search/astro-ph?searchtype=author&query=He%2C+J">Jiansen He</a>, <a href="/search/astro-ph?searchtype=author&query=Henri%2C+P">Pierre Henri</a>, <a href="/search/astro-ph?searchtype=author&query=Kasahara%2C+S">Satoshi Kasahara</a>, <a href="/search/astro-ph?searchtype=author&query=Khotyaintsev%2C+Y">Yuri Khotyaintsev</a>, <a href="/search/astro-ph?searchtype=author&query=Klein%2C+K+G">Kristopher G. Klein</a>, <a href="/search/astro-ph?searchtype=author&query=Lavraud%2C+B">Benoit Lavraud</a>, <a href="/search/astro-ph?searchtype=author&query=Maruca%2C+B+A">Bennett A. Maruca</a>, <a href="/search/astro-ph?searchtype=author&query=Maksimovic%2C+M">Milan Maksimovic</a>, <a href="/search/astro-ph?searchtype=author&query=Plaschke%2C+F">Ferdinand Plaschke</a>, <a href="/search/astro-ph?searchtype=author&query=Poedts%2C+S">Stefaan Poedts</a>, <a href="/search/astro-ph?searchtype=author&query=Reynolds%2C+C+S">Chirstopher S. Reynolds</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts%2C+O">Owen Roberts</a>, <a href="/search/astro-ph?searchtype=author&query=Sahraoui%2C+F">Fouad Sahraoui</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+S">Shinji Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Salem%2C+C+S">Chadi S. Salem</a> , et al. (5 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="1908.02206v1-abstract-short" style="display: inline;"> A grand-challenge problem at the forefront of physics is to understand how energy is transported and transformed in plasmas. This fundamental research priority encapsulates the conversion of plasma-flow and electromagnetic energies into particle energy, either as heat or some other form of energisation. The smallest characteristic scales, at which electron dynamics determines the plasma behaviour,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.02206v1-abstract-full').style.display = 'inline'; document.getElementById('1908.02206v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.02206v1-abstract-full" style="display: none;"> A grand-challenge problem at the forefront of physics is to understand how energy is transported and transformed in plasmas. This fundamental research priority encapsulates the conversion of plasma-flow and electromagnetic energies into particle energy, either as heat or some other form of energisation. The smallest characteristic scales, at which electron dynamics determines the plasma behaviour, are the next frontier in space and astrophysical plasma research. The analysis of astrophysical processes at these scales lies at the heart of the field of electron-astrophysics. Electron scales are the ultimate bottleneck for dissipation of plasma turbulence, which is a fundamental process not understood in the electron-kinetic regime. Since electrons are the most numerous and most mobile plasma species in fully ionised plasmas and are strongly guided by the magnetic field, their thermal properties couple very efficiently to global plasma dynamics and thermodynamics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.02206v1-abstract-full').style.display = 'none'; document.getElementById('1908.02206v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2019. </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">White Paper for the Voyage 2050 Long-Term Plan in the ESA Science Programme; 27 pages</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1907.02646">arXiv:1907.02646</a> <span> [<a href="https://arxiv.org/pdf/1907.02646">pdf</a>, <a href="https://arxiv.org/format/1907.02646">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="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/10.1093/mnras/stz3422">10.1093/mnras/stz3422 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The origin of slow Alfv茅nic solar wind at solar minimum </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Stansby%2C+D">D. Stansby</a>, <a href="/search/astro-ph?searchtype=author&query=Matteini%2C+L">L. Matteini</a>, <a href="/search/astro-ph?searchtype=author&query=Horbury%2C+T+S">T. S. Horbury</a>, <a href="/search/astro-ph?searchtype=author&query=Perrone%2C+D">D. Perrone</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Amicis%2C+R">R. D'Amicis</a>, <a href="/search/astro-ph?searchtype=author&query=Ber%C4%8Di%C4%8D%2C+L">L. Ber膷i膷</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="1907.02646v2-abstract-short" style="display: inline;"> Although the origins of slow solar wind are unclear, there is increasing evidence that at least some of it is released in a steady state on over-expanded coronal hole magnetic field lines. This type of slow wind has similar properties to the fast solar wind, including a high degree of Alfv茅nicity. In this study a combination of proton, alpha particle, and electron measurements are used to investig… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.02646v2-abstract-full').style.display = 'inline'; document.getElementById('1907.02646v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1907.02646v2-abstract-full" style="display: none;"> Although the origins of slow solar wind are unclear, there is increasing evidence that at least some of it is released in a steady state on over-expanded coronal hole magnetic field lines. This type of slow wind has similar properties to the fast solar wind, including a high degree of Alfv茅nicity. In this study a combination of proton, alpha particle, and electron measurements are used to investigate the kinetic properties of a single interval of slow Alfv茅nic wind at 0.35 AU. It is shown that this slow Alfv茅nic interval is characterised by high alpha particle abundances, pronounced alpha-proton differential streaming, strong proton beams, and large alpha to proton temperature ratios. These are all features observed consistently in the fast solar wind, adding evidence that at least some Alfv茅nic slow solar wind also originates in coronal holes. Observed differences between speed, mass flux, and electron temperature between slow Alfv茅nic and fast winds are explained by differing magnetic field geometry in the lower corona. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.02646v2-abstract-full').style.display = 'none'; document.getElementById('1907.02646v2-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> 27 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 July, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1812.01899">arXiv:1812.01899</a> <span> [<a href="https://arxiv.org/pdf/1812.01899">pdf</a>, <a href="https://arxiv.org/format/1812.01899">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="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</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/10.1093/mnras/sty3329">10.1093/mnras/sty3329 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On slow solar wind with high Alfv茅nicity: from composition and microphysics to spectral properties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%27Amicis%2C+R">Raffaella D'Amicis</a>, <a href="/search/astro-ph?searchtype=author&query=Matteini%2C+L">Lorenzo Matteini</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+R">Roberto Bruno</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="1812.01899v1-abstract-short" style="display: inline;"> Alfv茅nic fluctuations are very common features in the solar wind and are found especially within the main portion of fast wind streams while the slow wind usually is less Alfv茅nic and more variable. In general, fast and slow wind show many differences which span from the large scale structure to small scale phenomena including also a different turbulent behaviour. Recent studies, however, have sho… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.01899v1-abstract-full').style.display = 'inline'; document.getElementById('1812.01899v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.01899v1-abstract-full" style="display: none;"> Alfv茅nic fluctuations are very common features in the solar wind and are found especially within the main portion of fast wind streams while the slow wind usually is less Alfv茅nic and more variable. In general, fast and slow wind show many differences which span from the large scale structure to small scale phenomena including also a different turbulent behaviour. Recent studies, however, have shown that even slow wind can be sometimes highly Alfv茅nic with fluctuations as large as those of the fast wind. The present study is devoted to present many facets of this Alfv茅nic slow solar wind including for example the study of the source regions and their connection to coronal structures, large-scale properties and micro-scale phenomena and also impact on the spectral features. This study will be conducted performing a comparative analysis with the typical slow wind and with the fast wind. It has been found that the fast wind and the Alfv茅nic slow wind share common characteristics, probably attributable to their similar solar origin, i.e. coronal-hole solar wind. Given these similarities, it is suggested that in the Alfv茅nic slow wind a major role is played by the super-radial expansion responsible for the lower velocity. Relevant implications of these new findings for the upcoming Solar Orbiter and Solar Probe Plus missions, and more in general for turbulence measurements close to the Sun, will be discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.01899v1-abstract-full').style.display = 'none'; document.getElementById('1812.01899v1-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 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2018. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1411.3473">arXiv:1411.3473</a> <span> [<a href="https://arxiv.org/pdf/1411.3473">pdf</a>, <a href="https://arxiv.org/ps/1411.3473">ps</a>, <a href="https://arxiv.org/format/1411.3473">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/786/1/53">10.1088/0004-637X/786/1/53 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radial evolution of intermittency of density fluctuations in the fast solar wind </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+R">R. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Telloni%2C+D">D. Telloni</a>, <a href="/search/astro-ph?searchtype=author&query=Primavera%2C+L">L. Primavera</a>, <a href="/search/astro-ph?searchtype=author&query=Pietropaolo%2C+E">E. Pietropaolo</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Amicis%2C+R">R. D'Amicis</a>, <a href="/search/astro-ph?searchtype=author&query=Sorriso-Valvo%2C+L">L. Sorriso-Valvo</a>, <a href="/search/astro-ph?searchtype=author&query=Carbone%2C+V">V. Carbone</a>, <a href="/search/astro-ph?searchtype=author&query=Malara%2C+F">F. Malara</a>, <a href="/search/astro-ph?searchtype=author&query=Veltri%2C+P">P. Veltri</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="1411.3473v1-abstract-short" style="display: inline;"> We study the radial evolution of intermittency of density fluctuations in the fast solar wind. The study is performed analyzing the plasma density measurements provided by Helios 2 in the inner heliosphere between $0.3$ and $0.9$ AU. The analysis is carried out by means of a complete set of diagnostic tools, including the flatness factor at different time scales to estimate intermittency, the Kolm… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.3473v1-abstract-full').style.display = 'inline'; document.getElementById('1411.3473v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1411.3473v1-abstract-full" style="display: none;"> We study the radial evolution of intermittency of density fluctuations in the fast solar wind. The study is performed analyzing the plasma density measurements provided by Helios 2 in the inner heliosphere between $0.3$ and $0.9$ AU. The analysis is carried out by means of a complete set of diagnostic tools, including the flatness factor at different time scales to estimate intermittency, the Kolmogorov-Smirnov test to estimate the degree of intermittency, and the Fourier transform to estimate the power spectral densities of these fluctuations. Density fluctuations within fast wind are rather intermittent and their level of intermittency, together with the amplitude of intermittent events, decreases with distance from the Sun, at odds with intermittency of both magnetic field and all the other plasma parameters. Furthermore, the intermittent events are strongly correlated, exhibiting temporal clustering. This indicates that the mechanism underlying their generation departs from a time-varying Poisson process. A remarkable, qualitative similarity with the behavior of plasma density fluctuations obtained from a numerical study of the nonlinear evolution of parametric instability in the solar wind supports the idea that this mechanism has an important role in governing density fluctuations in the inner heliosphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.3473v1-abstract-full').style.display = 'none'; document.getElementById('1411.3473v1-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 November, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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> 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