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dc.contributor.authorDe Pontieu, Bart
dc.contributor.authorTesta, Paola
dc.contributor.authorMartínez-Sykora, Juan
dc.contributor.authorAntolin, Patrick
dc.contributor.authorKarampelas, Konstantinos
dc.contributor.authorHansteen, Viggo
dc.contributor.authorRempel, Matthias
dc.contributor.authorCheung, Mark C. M.
dc.contributor.authorReale, Fabio
dc.contributor.authorDanilovic, Sanja
dc.contributor.authorPagano, Paolo
dc.contributor.authorPolito, Vanessa
dc.contributor.authorDe Moortel, Ineke
dc.contributor.authorNóbrega-Siverio, Daniel
dc.contributor.authorVan Doorsselaere, Tom
dc.contributor.authorPetralia, Antonino
dc.contributor.authorAsgari-Targhi, Mahboubeh
dc.contributor.authorBoerner, Paul
dc.contributor.authorCarlsson, Mats
dc.contributor.authorChintzoglou, Georgios
dc.contributor.authorDaw, Adrian
dc.contributor.authorDeLuca, Edward
dc.contributor.authorGolub, Leon
dc.contributor.authorMatsumoto, Takuma
dc.contributor.authorUgarte-Urra, Ignacio
dc.contributor.authorMcIntosh, Scott W.
dc.contributor.authorthe MUSE team
dc.date.accessioned2022-02-15T11:30:14Z
dc.date.available2022-02-15T11:30:14Z
dc.date.issued2022-02-11
dc.identifier.citationDe Pontieu , B , Testa , P , Martínez-Sykora , J , Antolin , P , Karampelas , K , Hansteen , V , Rempel , M , Cheung , M C M , Reale , F , Danilovic , S , Pagano , P , Polito , V , De Moortel , I , Nóbrega-Siverio , D , Van Doorsselaere , T , Petralia , A , Asgari-Targhi , M , Boerner , P , Carlsson , M , Chintzoglou , G , Daw , A , DeLuca , E , Golub , L , Matsumoto , T , Ugarte-Urra , I , McIntosh , S W & the MUSE team 2022 , ' Probing the physics of the solar atmosphere with the Multi-slit Solar Explorer (MUSE). I. Coronal heating ' , Astrophysical Journal , vol. 926 , no. 1 , 52 . https://doi.org/10.3847/1538-4357/ac4222en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 277878585
dc.identifier.otherPURE UUID: 5b98092f-43a3-45af-b07b-2aa2db92312f
dc.identifier.otherJisc: 77610
dc.identifier.otherpublisher-id: apjac4222
dc.identifier.othermanuscript: ac4222
dc.identifier.otherother: aas34249
dc.identifier.otherORCID: /0000-0002-1452-9330/work/108508293
dc.identifier.otherScopus: 85125879466
dc.identifier.otherWOS: 000754065400001
dc.identifier.urihttp://hdl.handle.net/10023/24879
dc.descriptionFunding: I.D.M. has received support from the UK Science and Technology Facilities Council (Consolidated grant ST/K000950/1), the European Union Horizon 2020 research and innovation program (grant agreement No. 647214), and the Research Council of Norway through its Centres of Excellence scheme, project number 262622.en
dc.description.abstractThe Multi-slit Solar Explorer (MUSE) is a proposed mission composed of a multislit extreme ultraviolet (EUV) spectrograph (in three spectral bands around 171 Å, 284 Å, and 108 Å) and an EUV context imager (in two passbands around 195 Å and 304 Å). MUSE will provide unprecedented spectral and imaging diagnostics of the solar corona at high spatial (≤0.″5) and temporal resolution (down to ∼0.5 s for sit-and-stare observations), thanks to its innovative multislit design. By obtaining spectra in four bright EUV lines (Fe ix 171 Å, Fe xv 284 Å, Fe xix–Fe xxi 108 Å) covering a wide range of transition regions and coronal temperatures along 37 slits simultaneously, MUSE will, for the first time, “freeze” (at a cadence as short as 10 s) with a spectroscopic raster the evolution of the dynamic coronal plasma over a wide range of scales: from the spatial scales on which energy is released (≤0.″5) to the large-scale (∼170″ × 170″) atmospheric response. We use numerical modeling to showcase how MUSE will constrain the properties of the solar atmosphere on spatiotemporal scales (≤0.″5, ≤20 s) and the large field of view on which state-of-the-art models of the physical processes that drive coronal heating, flares, and coronal mass ejections (CMEs) make distinguishing and testable predictions. We describe the synergy between MUSE, the single-slit, high-resolution Solar-C EUVST spectrograph, and ground-based observatories (DKIST and others), and the critical role MUSE plays because of the multiscale nature of the physical processes involved. In this first paper, we focus on coronal heating mechanisms. An accompanying paper focuses on flares and CMEs.
dc.format.extent36
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rightsCopyright © 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.en
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleProbing the physics of the solar atmosphere with the Multi-slit Solar Explorer (MUSE). I. Coronal heatingen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorEuropean Research Councilen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.contributor.institutionUniversity of St Andrews. Office of the Principalen
dc.identifier.doihttps://doi.org/10.3847/1538-4357/ac4222
dc.description.statusPeer revieweden
dc.identifier.grantnumberST/K000950/1en
dc.identifier.grantnumber647214en


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