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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/2306.05481">arXiv:2306.05481</a> <span> [<a href="https://arxiv.org/pdf/2306.05481">pdf</a>, <a href="https://arxiv.org/format/2306.05481">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="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/10.3847/25c2cfeb.754285cf">10.3847/25c2cfeb.754285cf <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Small Platforms, High Return: The Need to Enhance Investment in Small Satellites for Focused Science, Career Development, and Improved Equity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Mason%2C+J+P">James Paul Mason</a>, <a href="/search/physics?searchtype=author&query=Begbie%2C+R+G">Robert G. Begbie</a>, <a href="/search/physics?searchtype=author&query=Bowen%2C+M">Maitland Bowen</a>, <a href="/search/physics?searchtype=author&query=Caspi%2C+A">Amir Caspi</a>, <a href="/search/physics?searchtype=author&query=Chamberlin%2C+P+C">Phillip C. Chamberlin</a>, <a href="/search/physics?searchtype=author&query=Chandran%2C+A">Amal Chandran</a>, <a href="/search/physics?searchtype=author&query=Cohen%2C+I">Ian Cohen</a>, <a href="/search/physics?searchtype=author&query=DeLuca%2C+E+E">Edward E. DeLuca</a>, <a href="/search/physics?searchtype=author&query=de+Wijn%2C+A+G">Alfred G. de Wijn</a>, <a href="/search/physics?searchtype=author&query=Dissauer%2C+K">Karin Dissauer</a>, <a href="/search/physics?searchtype=author&query=Eparvier%2C+F">Francis Eparvier</a>, <a href="/search/physics?searchtype=author&query=Filwett%2C+R">Rachael Filwett</a>, <a href="/search/physics?searchtype=author&query=Gibson%2C+S">Sarah Gibson</a>, <a href="/search/physics?searchtype=author&query=Gilly%2C+C+R">Chris R. Gilly</a>, <a href="/search/physics?searchtype=author&query=Herde%2C+V">Vicki Herde</a>, <a href="/search/physics?searchtype=author&query=Ho%2C+G">George Ho</a>, <a href="/search/physics?searchtype=author&query=Hospodarsky%2C+G">George Hospodarsky</a>, <a href="/search/physics?searchtype=author&query=Jaynes%2C+A">Allison Jaynes</a>, <a href="/search/physics?searchtype=author&query=Jones%2C+A+R">Andrew R. Jones</a>, <a href="/search/physics?searchtype=author&query=Kasper%2C+J+C">Justin C. Kasper</a>, <a href="/search/physics?searchtype=author&query=Kohnert%2C+R">Rick Kohnert</a>, <a href="/search/physics?searchtype=author&query=Lee%2C+Z">Zoe Lee</a>, <a href="/search/physics?searchtype=author&query=Mason%2C+E+I">E. I. Mason</a>, <a href="/search/physics?searchtype=author&query=Merkel%2C+A">Aimee Merkel</a>, <a href="/search/physics?searchtype=author&query=Mesquita%2C+R">Rafael Mesquita</a> , et al. (11 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="2306.05481v1-abstract-short" style="display: inline;"> In the next decade, there is an opportunity for very high return on investment of relatively small budgets by elevating the priority of smallsat funding in heliophysics. We've learned in the past decade that these missions perform exceptionally well by traditional metrics, e.g., papers/year/\$M (Spence et al. 2022 -- arXiv:2206.02968). It is also well established that there is a "leaky pipeline" r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.05481v1-abstract-full').style.display = 'inline'; document.getElementById('2306.05481v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.05481v1-abstract-full" style="display: none;"> In the next decade, there is an opportunity for very high return on investment of relatively small budgets by elevating the priority of smallsat funding in heliophysics. We've learned in the past decade that these missions perform exceptionally well by traditional metrics, e.g., papers/year/\$M (Spence et al. 2022 -- arXiv:2206.02968). It is also well established that there is a "leaky pipeline" resulting in too little diversity in leadership positions (see the National Academies Report at https://www.nationalacademies.org/our-work/increasing-diversity-in-the-leadership-of-competed-space-missions). Prioritizing smallsat funding would significantly increase the number of opportunities for new leaders to learn -- a crucial patch for the pipeline and an essential phase of career development. At present, however, there are far more proposers than the available funding can support, leading to selection ratios that can be as low as 6% -- in the bottom 0.5th percentile of selection ratios across the history of ROSES. Prioritizing SmallSat funding and substantially increasing that selection ratio are the fundamental recommendations being made by this white paper. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.05481v1-abstract-full').style.display = 'none'; document.getElementById('2306.05481v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">White paper submitted to the Decadal Survey for Solar and Space Physics (Heliophysics) 2024-2033; 6 pages, 1 figure</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Bulletin of the AAS, Vol. 55, Issue 3, Whitepaper #268 (6pp); 2023 July 31 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.02228">arXiv:2210.02228</a> <span> [<a href="https://arxiv.org/pdf/2210.02228">pdf</a>, <a href="https://arxiv.org/format/2210.02228">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/10.1051/0004-6361/202244248">10.1051/0004-6361/202244248 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Tracking magnetic flux and helicity from Sun to Earth -- Multi-spacecraft analysis of a magnetic cloud and its solar source </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Thalmann%2C+J+K">J. K. Thalmann</a>, <a href="/search/physics?searchtype=author&query=Dumbovic%2C+M">M. Dumbovic</a>, <a href="/search/physics?searchtype=author&query=Dissauer%2C+K">K. Dissauer</a>, <a href="/search/physics?searchtype=author&query=Podladchikova%2C+T">T. Podladchikova</a>, <a href="/search/physics?searchtype=author&query=Chikunova%2C+G">G. Chikunova</a>, <a href="/search/physics?searchtype=author&query=Temmer%2C+M">M. Temmer</a>, <a href="/search/physics?searchtype=author&query=Dickson%2C+E">E. Dickson</a>, <a href="/search/physics?searchtype=author&query=Veronig%2C+A+M">A. M. Veronig</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.02228v1-abstract-short" style="display: inline;"> We analyze the complete chain of effects caused by a solar eruptive event in order to better understand the dynamic evolution of magnetic-field related quantities in interplanetary space, in particular that of magnetic flux and helicity. We study a series of connected events (a confined C4.5 flare, a flare-less filament eruption and a double-peak M-class flare) that originated in NOAA active regio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.02228v1-abstract-full').style.display = 'inline'; document.getElementById('2210.02228v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.02228v1-abstract-full" style="display: none;"> We analyze the complete chain of effects caused by a solar eruptive event in order to better understand the dynamic evolution of magnetic-field related quantities in interplanetary space, in particular that of magnetic flux and helicity. We study a series of connected events (a confined C4.5 flare, a flare-less filament eruption and a double-peak M-class flare) that originated in NOAA active region (AR) 12891 on 2021 November 1 and November 2. We deduce the magnetic structure of AR 12891 using stereoscopy and nonlinear force-free (NLFF) magnetic field modeling, allowing us to identify a coronal flux rope and to estimate its axial flux and helicity. Additionally, we compute reconnection fluxes based on flare ribbon and coronal dimming signatures from remote sensing imagery. Comparison to corresponding quantities of the associated magnetic cloud (MC), deduced from in-situ measurements from Solar Orbiter and near-Earth spacecraft, allows us to draw conclusions on the evolution of the associated interplanetary coronal mass ejection (ICME). The latter are aided through the application of geometric fitting techniques (graduated cylindrical shell modeling; GCS) and interplanetary propagation models (drag based ensemble modeling; DBEM) to the ICME. NLFF modeling suggests the host AR's magnetic structure in the form of a left-handed (negative-helicity) sheared arcade/flux rope reaching to altitudes of 8-10 Mm above photospheric levels, in close agreement with the corresponding stereoscopic estimate. Revealed from GCS and DBEM modeling, the ejected flux rope propagated in a self-similar expanding manner through interplanetary space. Comparison of magnetic fluxes and helicities processed by magnetic reconnection in the solar source region and the respective budgets of the MC indicate a considerable contribution from the eruptive process, though the pre-eruptive budgets appear of relevance too. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.02228v1-abstract-full').style.display = 'none'; document.getElementById('2210.02228v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 9 Figures, 3 Tables, 1 Movie; accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 669, A72 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.06116">arXiv:2012.06116</a> <span> [<a href="https://arxiv.org/pdf/2012.06116">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> Earth-affecting Solar Transients: A Review of Progresses in Solar Cycle 24 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Zhang%2C+J">Jie Zhang</a>, <a href="/search/physics?searchtype=author&query=Temmer%2C+M">Manuela Temmer</a>, <a href="/search/physics?searchtype=author&query=Gopalswamy%2C+N">Nat Gopalswamy</a>, <a href="/search/physics?searchtype=author&query=Malandraki%2C+O">Olga Malandraki</a>, <a href="/search/physics?searchtype=author&query=Nitta%2C+N+V">Nariaki V. Nitta</a>, <a href="/search/physics?searchtype=author&query=Patsourakos%2C+S">Spiros Patsourakos</a>, <a href="/search/physics?searchtype=author&query=Shen%2C+F">Fang Shen</a>, <a href="/search/physics?searchtype=author&query=Vr%C5%A1nak%2C+B">Bojan Vr拧nak</a>, <a href="/search/physics?searchtype=author&query=Wang%2C+Y">Yuming Wang</a>, <a href="/search/physics?searchtype=author&query=Webb%2C+D">David Webb</a>, <a href="/search/physics?searchtype=author&query=Desai%2C+M+I">Mihir I. Desai</a>, <a href="/search/physics?searchtype=author&query=Dissauer%2C+K">Karin Dissauer</a>, <a href="/search/physics?searchtype=author&query=Dresing%2C+N">Nina Dresing</a>, <a href="/search/physics?searchtype=author&query=Dumbovi%C4%87%2C+M">Mateja Dumbovi膰</a>, <a href="/search/physics?searchtype=author&query=Feng%2C+X">Xueshang Feng</a>, <a href="/search/physics?searchtype=author&query=Heinemann%2C+S+G">Stephan G. Heinemann</a>, <a href="/search/physics?searchtype=author&query=Laurenza%2C+M">Monica Laurenza</a>, <a href="/search/physics?searchtype=author&query=Lugaz%2C+N">No茅 Lugaz</a>, <a href="/search/physics?searchtype=author&query=Zhuang%2C+B">Bin Zhuang</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="2012.06116v1-abstract-short" style="display: inline;"> This review article summarizes the advancement in the studies of Earth-affecting solar transients in the last decade that encompasses most of solar cycle 24. The Sun Earth is an integrated physical system in which the space environment of the Earth sustains continuous influence from mass, magnetic field and radiation energy output of the Sun in varying time scales from minutes to millennium. This… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.06116v1-abstract-full').style.display = 'inline'; document.getElementById('2012.06116v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.06116v1-abstract-full" style="display: none;"> This review article summarizes the advancement in the studies of Earth-affecting solar transients in the last decade that encompasses most of solar cycle 24. The Sun Earth is an integrated physical system in which the space environment of the Earth sustains continuous influence from mass, magnetic field and radiation energy output of the Sun in varying time scales from minutes to millennium. This article addresses short time scale events, from minutes to days that directly cause transient disturbances in the Earth space environment and generate intense adverse effects on advanced technological systems of human society. Such transient events largely fall into the following four types: (1) solar flares, (2) coronal mass ejections (CMEs) including their interplanetary counterparts ICMEs, (3) solar energetic particle (SEP) events, and (4) stream interaction regions (SIRs) including corotating interaction regions (CIRs). In the last decade, the unprecedented multi viewpoint observations of the Sun from space, enabled by STEREO Ahead/Behind spacecraft in combination with a suite of observatories along the Sun-Earth lines, have provided much more accurate and global measurements of the size, speed, propagation direction and morphology of CMEs in both 3-D and over a large volume in the heliosphere. Several advanced MHD models have been developed to simulate realistic CME events from the initiation on the Sun until their arrival at 1 AU. Much progress has been made on detailed kinematic and dynamic behaviors of CMEs, including non-radial motion, rotation and deformation of CMEs, CME-CME interaction, and stealth CMEs and problematic ICMEs. The knowledge about SEPs has also been significantly improved. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.06116v1-abstract-full').style.display = 'none'; document.getElementById('2012.06116v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">Review article, 184 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/2006.11707">arXiv:2006.11707</a> <span> [<a href="https://arxiv.org/pdf/2006.11707">pdf</a>, <a href="https://arxiv.org/ps/2006.11707">ps</a>, <a href="https://arxiv.org/format/2006.11707">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/10.3847/2041-8213/ab9ec5">10.3847/2041-8213/ab9ec5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Solar Flare-CME Coupling Throughout Two Acceleration Phases of a Fast CME </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Gou%2C+T">Tingyu Gou</a>, <a href="/search/physics?searchtype=author&query=Veronig%2C+A+M">Astrid M. Veronig</a>, <a href="/search/physics?searchtype=author&query=Liu%2C+R">Rui Liu</a>, <a href="/search/physics?searchtype=author&query=Zhuang%2C+B">Bin Zhuang</a>, <a href="/search/physics?searchtype=author&query=Dumbovic%2C+M">Mateja Dumbovic</a>, <a href="/search/physics?searchtype=author&query=Podladchikova%2C+T">Tatiana Podladchikova</a>, <a href="/search/physics?searchtype=author&query=Reid%2C+H+A+S">Hamish A. S. Reid</a>, <a href="/search/physics?searchtype=author&query=Temmer%2C+M">Manuela Temmer</a>, <a href="/search/physics?searchtype=author&query=Dissauer%2C+K">Karin Dissauer</a>, <a href="/search/physics?searchtype=author&query=Vrsnak%2C+B">Bojan Vrsnak</a>, <a href="/search/physics?searchtype=author&query=Wang%2C+Y">Yuming 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="2006.11707v1-abstract-short" style="display: inline;"> Solar flares and coronal mass ejections (CMEs) are closely coupled through magnetic reconnection. CMEs are usually accelerated impulsively within the low solar corona, synchronized with the impulsive flare energy release. We investigate the dynamic evolution of a fast CME and its associated X2.8 flare occurring on 2013 May 13. The CME experiences two distinct phases of enhanced acceleration, an im… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.11707v1-abstract-full').style.display = 'inline'; document.getElementById('2006.11707v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.11707v1-abstract-full" style="display: none;"> Solar flares and coronal mass ejections (CMEs) are closely coupled through magnetic reconnection. CMEs are usually accelerated impulsively within the low solar corona, synchronized with the impulsive flare energy release. We investigate the dynamic evolution of a fast CME and its associated X2.8 flare occurring on 2013 May 13. The CME experiences two distinct phases of enhanced acceleration, an impulsive one with a peak value of ~5 km s$^{-2}$ followed by an extended phase with accelerations up to 0.7 km s$^{-2}$. The two-phase CME dynamics is associated with a two-episode flare energy release. While the first episode is consistent with the "standard" eruption of a magnetic flux rope, the second episode of flare energy release is initiated by the reconnection of a large-scale loop in the aftermath of the eruption and produces stronger nonthermal emission up to $纬$-rays. In addition, this long-duration flare reveals clear signs of ongoing magnetic reconnection during the decay phase, evidenced by extended HXR bursts with energies up to 100--300 keV and intermittent downflows of reconnected loops for >4 hours. The observations reveal that the two-step flare reconnection substantially contributes to the two-phase CME acceleration, and the impulsive CME acceleration precedes the most intense flare energy release. The implications of this non-standard flare/CME observation are discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.11707v1-abstract-full').style.display = 'none'; document.getElementById('2006.11707v1-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 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">accepted for publication in ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1911.10817">arXiv:1911.10817</a> <span> [<a href="https://arxiv.org/pdf/1911.10817">pdf</a>, <a href="https://arxiv.org/format/1911.10817">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/ab6216">10.3847/1538-4365/ab6216 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CME-CME Interactions as Sources of CME Geo-effectiveness: The Formation of the Complex Ejecta and Intense Geomagnetic Storm in Early September 2017 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Scolini%2C+C">Camilla Scolini</a>, <a href="/search/physics?searchtype=author&query=Chan%C3%A9%2C+E">Emmanuel Chan茅</a>, <a href="/search/physics?searchtype=author&query=Temmer%2C+M">Manuela Temmer</a>, <a href="/search/physics?searchtype=author&query=Kilpua%2C+E+K+J">Emilia K. J. Kilpua</a>, <a href="/search/physics?searchtype=author&query=Dissauer%2C+K">Karin Dissauer</a>, <a href="/search/physics?searchtype=author&query=Veronig%2C+A+M">Astrid M. Veronig</a>, <a href="/search/physics?searchtype=author&query=Palmerio%2C+E">Erika Palmerio</a>, <a href="/search/physics?searchtype=author&query=Pomoell%2C+J">Jens Pomoell</a>, <a href="/search/physics?searchtype=author&query=Dumbovi%C4%87%2C+M">Mateja Dumbovi膰</a>, <a href="/search/physics?searchtype=author&query=Guo%2C+J">Jingnan Guo</a>, <a href="/search/physics?searchtype=author&query=Rodriguez%2C+L">Luciano Rodriguez</a>, <a href="/search/physics?searchtype=author&query=Poedts%2C+S">Stefaan Poedts</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1911.10817v1-abstract-short" style="display: inline;"> Coronal mass ejections (CMEs) are the primary sources of intense disturbances at Earth, where their geo-effectiveness is largely determined by their dynamic pressure and internal magnetic field, which can be significantly altered during interactions with other CMEs in interplanetary space. We analyse three successive CMEs that erupted from the Sun during September 4-6, 2017, investigating the role… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.10817v1-abstract-full').style.display = 'inline'; document.getElementById('1911.10817v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.10817v1-abstract-full" style="display: none;"> Coronal mass ejections (CMEs) are the primary sources of intense disturbances at Earth, where their geo-effectiveness is largely determined by their dynamic pressure and internal magnetic field, which can be significantly altered during interactions with other CMEs in interplanetary space. We analyse three successive CMEs that erupted from the Sun during September 4-6, 2017, investigating the role of CME-CME interactions as source of the associated intense geomagnetic storm (Dst_min=-142 nT on September 7). To quantify the impact of interactions on the (geo-)effectiveness of individual CMEs, we perform global heliospheric simulations with the EUHFORIA model, using observation-based initial parameters with the additional purpose of validating the predictive capabilities of the model for complex CME events. The simulations show that around 0.45 AU, the shock driven by the September 6 CME started compressing a preceding magnetic ejecta formed by the merging of two CMEs launched on September 4, significantly amplifying its Bz until a maximum factor of 2.8 around 0.9 AU. The following gradual conversion of magnetic energy into kinetic and thermal components reduced the Bz amplification until its almost complete disappearance around 1.8 AU. We conclude that a key factor at the origin of the intense storm triggered by the September 4-6, 2017 CMEs was their arrival at Earth during the phase of maximum Bz amplification. Our analysis highlights how the amplification of the magnetic field of individual CMEs in space-time due to interaction processes can be characterised by a growth, a maximum, and a decay phase, suggesting that the time interval between the CME eruptions and their relative speeds are critical factors in determining the resulting impact of complex CMEs at various heliocentric distances (helio-effectiveness). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.10817v1-abstract-full').style.display = 'none'; document.getElementById('1911.10817v1-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, 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/1908.10161">arXiv:1908.10161</a> <span> [<a href="https://arxiv.org/pdf/1908.10161">pdf</a>, <a href="https://arxiv.org/format/1908.10161">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/10.1007/s11207-019-1515-6">10.1007/s11207-019-1515-6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CME -- HSS interaction and characteristics tracked from Sun to Earth </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Heinemann%2C+S+G">Stephan G. Heinemann</a>, <a href="/search/physics?searchtype=author&query=Temmer%2C+M">Manuela Temmer</a>, <a href="/search/physics?searchtype=author&query=Farrugia%2C+C+J">Charles J. Farrugia</a>, <a href="/search/physics?searchtype=author&query=Dissauer%2C+K">Karin Dissauer</a>, <a href="/search/physics?searchtype=author&query=Kay%2C+C">Christina Kay</a>, <a href="/search/physics?searchtype=author&query=Wiegelmann%2C+T">Thomas Wiegelmann</a>, <a href="/search/physics?searchtype=author&query=Dumbovi%C4%87%2C+M">Mateja Dumbovi膰</a>, <a href="/search/physics?searchtype=author&query=Veronig%2C+A+M">Astrid M. Veronig</a>, <a href="/search/physics?searchtype=author&query=Podladchikova%2C+T">Tatiana Podladchikova</a>, <a href="/search/physics?searchtype=author&query=Hofmeister%2C+S+J">Stefan J. Hofmeister</a>, <a href="/search/physics?searchtype=author&query=Lugaz%2C+N">No茅 Lugaz</a>, <a href="/search/physics?searchtype=author&query=Carcaboso%2C+F">Fernando Carcaboso</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="1908.10161v1-abstract-short" style="display: inline;"> In a thorough study, we investigate the origin of a remarkable plasma and magnetic field configuration observed in situ on June 22, 2011 near L1, which appears to be a magnetic ejecta (ME) and a shock signature engulfed by a solar wind high-speed stream (HSS). We identify the signatures as an Earth-directed coronal mass ejection (CME), associated with a C7.7 flare on June 21, 2011, and its interac… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.10161v1-abstract-full').style.display = 'inline'; document.getElementById('1908.10161v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.10161v1-abstract-full" style="display: none;"> In a thorough study, we investigate the origin of a remarkable plasma and magnetic field configuration observed in situ on June 22, 2011 near L1, which appears to be a magnetic ejecta (ME) and a shock signature engulfed by a solar wind high-speed stream (HSS). We identify the signatures as an Earth-directed coronal mass ejection (CME), associated with a C7.7 flare on June 21, 2011, and its interaction with a HSS, which emanates from a coronal hole (CH) close to the launch site of the CME. The results indicate that the major interaction between the CME and the HSS starts at a height of 1.3 Rsun up to 3 Rsun. Over that distance range, the CME undergoes a strong north-eastward deflection of at least 30 degrees due to the open magnetic field configuration of the CH. We perform a comprehensive analysis for the CME-HSS event using multi-viewpoint data (from the Solar TErrestrial RElations Observatories, the Solar and Heliospheric Observatory and the Solar Dynamics Observatory), and combined modeling efforts (nonlinear force-free field modeling, Graduated Cylindrical Shell CME modeling, and the Forecasting a CMEs Altered Trajectory ForeCAT model). We aim at better understanding its early evolution and interaction process as well as its interplanetary propagation and related in situ signatures, and finally the resulting impact on the Earth's magnetosphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.10161v1-abstract-full').style.display = 'none'; document.getElementById('1908.10161v1-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 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">Accepted in Solar Physics on August 26, 2019</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1906.02532">arXiv:1906.02532</a> <span> [<a href="https://arxiv.org/pdf/1906.02532">pdf</a>, <a href="https://arxiv.org/format/1906.02532">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab27ca">10.3847/1538-4357/ab27ca <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Unusual plasma and particle signatures at Mars and STEREO-A related to CME-CME interaction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Dumbovic%2C+M">Mateja Dumbovic</a>, <a href="/search/physics?searchtype=author&query=Guo%2C+J">Jingnan Guo</a>, <a href="/search/physics?searchtype=author&query=Temmer%2C+M">Manuela Temmer</a>, <a href="/search/physics?searchtype=author&query=Mays%2C+M+L">M. Leila Mays</a>, <a href="/search/physics?searchtype=author&query=Veronig%2C+A">Astrid Veronig</a>, <a href="/search/physics?searchtype=author&query=Heinemann%2C+S">Stephan Heinemann</a>, <a href="/search/physics?searchtype=author&query=Dissauer%2C+K">Karin Dissauer</a>, <a href="/search/physics?searchtype=author&query=Hofmeister%2C+S">Stefan Hofmeister</a>, <a href="/search/physics?searchtype=author&query=Halekas%2C+J">Jasper Halekas</a>, <a href="/search/physics?searchtype=author&query=M%C3%B6stl%2C+C">Christian M枚stl</a>, <a href="/search/physics?searchtype=author&query=Amerstorfer%2C+T">Tanja Amerstorfer</a>, <a href="/search/physics?searchtype=author&query=Hinterreiter%2C+J">J眉rgen Hinterreiter</a>, <a href="/search/physics?searchtype=author&query=Banjac%2C+S">Sasa Banjac</a>, <a href="/search/physics?searchtype=author&query=Herbst%2C+K">Konstantin Herbst</a>, <a href="/search/physics?searchtype=author&query=Wang%2C+Y">Yuming Wang</a>, <a href="/search/physics?searchtype=author&query=Holzknecht%2C+L">Lukas Holzknecht</a>, <a href="/search/physics?searchtype=author&query=Leitner%2C+M">Martin Leitner</a>, <a href="/search/physics?searchtype=author&query=Wimmer-Schweingruber%2C+R+F">Robert F. Wimmer-Schweingruber</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="1906.02532v1-abstract-short" style="display: inline;"> On July 25 2017 a multi-step Forbush decrease (FD) with the remarkable total amplitude of more than 15\% was observed by MSL/RAD at Mars. We find that these particle signatures are related to very pronounced plasma and magnetic field signatures detected in situ by STEREO-A on July 24 2017, with a higher than average total magnetic field strength reaching more than 60 nT. In the observed time perio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.02532v1-abstract-full').style.display = 'inline'; document.getElementById('1906.02532v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.02532v1-abstract-full" style="display: none;"> On July 25 2017 a multi-step Forbush decrease (FD) with the remarkable total amplitude of more than 15\% was observed by MSL/RAD at Mars. We find that these particle signatures are related to very pronounced plasma and magnetic field signatures detected in situ by STEREO-A on July 24 2017, with a higher than average total magnetic field strength reaching more than 60 nT. In the observed time period STEREO-A was at a relatively small longitudinal separation (46 degrees) to Mars and both were located at the back side of the Sun as viewed from Earth. We analyse a number of multi-spacecraft and multi-instrument (both in situ and remote-sensing) observations, and employ modelling to understand these signatures. We find that the solar sources are two CMEs which erupted on July 23 2017 from the same source region on the back side of the Sun as viewed from Earth. Moreover, we find that the two CMEs interact non-uniformly, inhibiting the expansion of one of the CMEs in STEREO-A direction, whereas allowing it to expand more freely in the Mars direction. The interaction of the two CMEs with the ambient solar wind adds up to the complexity of the event, resulting in a long, sub-structured interplanetary disturbance at Mars, where different sub-structures correspond to different steps of the FD, adding-up to a globally large-amplitude FD. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.02532v1-abstract-full').style.display = 'none'; document.getElementById('1906.02532v1-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 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">25 pages, 9 figures</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: 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