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dc.date.accessioned2018-02-16T09:43:45Z
dc.date.available2018-02-16T09:43:45Z
dc.date.created2017-03-28T10:54:06Z
dc.date.issued2017
dc.identifier.citationKowalski, Adam F. Allred, Joel C. Daw, A. Cauzzi, Gianna Carlsson, Mats . The atmospheric response to high nonthermal electron beam fluxes in solar flares. I. modeling the brightest NUV footpoints in the X1 solar flare of 2014 March 29. The Astrophysical Journal. 2017, 836(1)
dc.identifier.urihttp://hdl.handle.net/10852/60154
dc.description.abstractThe 2014 March 29 X1 solar flare (SOL20140329T17:48) produced bright continuum emission in the far- and near-ultraviolet (NUV) and highly asymmetric chromospheric emission lines, providing long-sought constraints on the heating mechanisms of the lower atmosphere in solar flares. We analyze the continuum and emission line data from the Interface Region Imaging Spectrograph (IRIS) of the brightest flaring magnetic footpoints in this flare. We compare the NUV spectra of the brightest pixels to new radiative-hydrodynamic predictions calculated with the RADYN code using constraints on a nonthermal electron beam inferred from the collisional thick-target modeling of hard X-ray data from Reuven Ramaty High Energy Solar Spectroscopic Imager. We show that the atmospheric response to a high beam flux density satisfactorily achieves the observed continuum brightness in the NUV. The NUV continuum emission in this flare is consistent with hydrogen (Balmer) recombination radiation that originates from low optical depth in a dense chromospheric condensation and from the stationary beam-heated layers just below the condensation. A model producing two flaring regions (a condensation and stationary layers) in the lower atmosphere is also consistent with the asymmetric Fe ii chromospheric emission line profiles observed in the impulsive phase. © 2017. The American Astronomical Society. All rights reserved.en_US
dc.languageEN
dc.language.isoenen_US
dc.publisherUniversity of Chicago Press
dc.titleThe atmospheric response to high nonthermal electron beam fluxes in solar flares. I. modeling the brightest NUV footpoints in the X1 solar flare of 2014 March 29en_US
dc.typeJournal articleen_US
dc.creator.authorKowalski, Adam F.
dc.creator.authorAllred, Joel C.
dc.creator.authorDaw, A.
dc.creator.authorCauzzi, Gianna
dc.creator.authorCarlsson, Mats
cristin.unitcode185,15,3,0
cristin.unitnameInstitutt for teoretisk astrofysikk
cristin.ispublishedtrue
cristin.fulltextoriginal
cristin.qualitycode2
dc.identifier.cristin1461633
dc.identifier.bibliographiccitationinfo:ofi/fmt:kev:mtx:ctx&ctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=The Astrophysical Journal&rft.volume=836&rft.spage=&rft.date=2017
dc.identifier.jtitleThe Astrophysical Journal
dc.identifier.volume836
dc.identifier.issue1
dc.identifier.pagecount27
dc.identifier.doihttp://dx.doi.org/10.3847/1538-4357/836/1/12
dc.identifier.urnURN:NBN:no-62813
dc.type.documentTidsskriftartikkelen_US
dc.type.peerreviewedPeer reviewed
dc.source.issn0004-637X
dc.identifier.fulltextFulltext https://www.duo.uio.no/bitstream/handle/10852/60154/1/Kowalski%252BAllred%252BDaw%252BCauzzi%252Betal2017.pdf
dc.type.versionPublishedVersion
cristin.articleid12
dc.relation.projectNOTUR/NORSTORE/nn2834k
dc.relation.projectNFR/230938


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