Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/8184
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dc.contributor.authorSterling, Alphonse C-
dc.contributor.authorMoore, Ronald L-
dc.contributor.authorPanesar, Navdeep K-
dc.contributor.authorSamanta, T-
dc.contributor.authorTiwari, Sanjiv K-
dc.contributor.authorSavage, Sabrina L-
dc.date.accessioned2023-04-26T08:24:28Z-
dc.date.available2023-04-26T08:24:28Z-
dc.date.issued2023-03-
dc.identifier.citationFrontiers in Astronomy and Space Sciences, Vol. 10, 49en_US
dc.identifier.issn2296-987X-
dc.identifier.urihttp://hdl.handle.net/2248/8184-
dc.descriptionOpen Accessen_US
dc.descriptionThis is an open-access article distributed under the terms of the Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) and the copyright owner(s) are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms.-
dc.description.abstractSolar coronal jets are frequently occurring collimated ejections of solar plasma, originating from magnetically mixed polarity locations on the Sun of size scale comparable to that of a supergranule. Many, if not most, coronal jets are produced by eruptions of small-scale filaments, or minifilaments, whose magnetic field reconnects both with itself and also with surrounding coronal field. There is evidence that minifilament eruptions are a scaled-down version of typical filament eruptions that produce solar flares and coronal mass ejections (CMEs). Moreover, the magnetic processes building up to and triggering minifilament eruptions, which is often flux cancelation, might similarly build up and trigger the larger filaments to erupt. Thus, detailed study of coronal jets will inform us of the physics leading to, triggering, and driving the larger eruptions. Additionally, such studies potentially can inform us of smaller-scale coronal-jet-like features, such as jetlets and perhaps some spicules, that might work the same way as coronal jets. We propose a high-resolution (∼0 ′′ . 1 pixels), high-cadence (∼5 s) EUV-solar-imaging mission for the upcoming decades, that would be dedicated to observations of features of the coronal-jet size scale, and smaller-scale solar features produced by similar physics. Such a mission could provide invaluable insight into the operation of larger features such as CMEs that produce significant Space Weather disturbances, and also smaller-scale features that could be important for coronal heating, solar wind acceleration, and heliospheric features such as the magnetic switchbacks that are frequently observed in the solar wind.en_US
dc.language.isoenen_US
dc.publisherFrontiersen_US
dc.relation.urihttps://doi.org/10.3389/fspas.2023.1117870-
dc.rights© 2023 Sterling, Moore, Panesar, Samanta, Tiwari and Savage.-
dc.subjectSolar filament eruptionsen_US
dc.subjectSolar coronaen_US
dc.subjectSolar X-ray emissionen_US
dc.subjectSolar extreme ultraviolet emissionen_US
dc.subjectSolar coronal jetsen_US
dc.subjectSolar magnetic activityen_US
dc.titleFuture high-resolution and high-cadence observations for unraveling small-scale explosive solar featuresen_US
dc.typeArticleen_US
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