![]() ![]() Among all these phenomena, plasma jets, defined as collimated plasma beams (for a review, see Raouafi et al. Plasma ejections are continuously observed in different forms, such as coronal mass ejections (CMEs), filament eruptions, or plasma jets. Understanding the mechanisms that underlie the acceleration of electrons in the lower solar corona and their subsequent access to interplanetary space is essential to answering unsolved questions in heliophysics that form part of the main science questions of the Solar Orbiter and Parker Solar Probe missions. Subscribe to A&A to support open access publication. This article is published in open access under the Subscribe-to-Open model. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License ( ), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Within the framework of the interchange reconnection model, we conclude that the energy release site observed above-the-loop corresponds to the electron acceleration site, corroborating that interchange reconnection is a viable candidate for particle acceleration in the low corona on field lines open to interplanetary space. Three-dimensional (3D) stereoscopic reconstructions of the propagating jet highlight that the ejected plasma moves along a curved trajectory.Ĭonclusions. During the flare, the same region spatially coincides with the origin of the coronal jet. Moreover, this region is moving toward higher altitudes over time (∼30 km s −1). From Earth’s vantage point, the microflare is seen near the limb, revealing the coronal energy release site above the flare loop in EUV, which, from STIX spectroscopic analysis, turns out to be hot (i.e., at roughly the same temperature of the flare). This microflare features prominent hard X-ray (HXR) nonthermal emission down to at least 10 keV and a spectrum that is much harder than usual for a microflare with γ = 2.9 ± 0.3. The event under investigation satisfies the classical picture of the onset time of the acceleration of electrons coinciding with the jet and the radio type III bursts. ![]() Multi-wavelength timing analysis combined with UV/EUV imagery and X-ray spectroscopy by Solar Orbiter/STIX (Spectrometer/Telescope for Imaging X-rays) is used to investigate the origin of the observed emission during different flare phases. This study takes advantage of three different vantage points, Solar Orbiter, STEREO-A, and Earth, with observations drawn from eight different instruments, ranging from radio to X-ray. We aim to investigate the electron acceleration and energy release sites as well as the manner in which accelerated electrons access the interplanetary space in the case of the SOLT18:05 event, a GOES A8 class microflare associated with a coronal jet. One of the main science questions of the Solar Orbiter and Parker Solar Probe missions deals with understanding how electrons in the lower solar corona are accelerated and how they subsequently access interplanetary space.Īims. Space Sciences Laboratory, University of California, 7 Gauss Way, 94720 Berkeley, USAĬontext. Physikalisch-Meteorologisches Observatorium Davos, World Radiation Center, 7260 Davos Dorf, Switzerland IRSOL Istituto Ricerche Solari “Aldo e Cele Daccó”, Università della Svizzera italiana, via PatocLocarno, Switzerland Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany Kanzelhöhe Observatory for Solar and Environmental Research, University of Graz, KanzelhTreffen, Austria Skolkovo Institute of Science and Technology, Bolshoy Boulevard 30, bld. Institute of Physics, University of Graz, UniversitätsplGraz, Austria School of Earth and Space Sciences, Peking University, Beijing 100871, PR China ![]() Institute for Data Science, University of Applied Sciences and Arts Northwestern Switzerland (FHNW), BahnhofstraWindisch, SwitzerlandĮ-mail: for Particle Physics and Astrophysics (IPA), Swiss Federal Institute of Technology in Zurich (ETHZ), Wolfgang-Pauli-StraZurich, Switzerland Dickson 4, Olena Podladchikova 7, Christian Monstein 8, Alexander Warmuth 7, Frédéric Schuller 7, Louise Harra 2 ,9 and Säm Krucker 1 ,10 Veronig 4 ,6, Hannah Collier 1 ,2, Ewan C.
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