Non-LTE inversions of a confined X2.2 flare: I. Vector magnetic field in the photosphere and chromosphere : I. The vector magnetic field in the photosphere and chromosphere

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dc.contributor University of Helsinki, Department of Physics en
dc.contributor University of Helsinki, Space Physics Research Group en
dc.contributor.author Vissers, G. J. M.
dc.contributor.author Danilovic, S.
dc.contributor.author de la Cruz Rodriguez, J.
dc.contributor.author Leenaarts, J.
dc.contributor.author Morosin, R.
dc.contributor.author Diaz Baso, C.
dc.contributor.author Reid, A.
dc.contributor.author Pomoell, Jens
dc.contributor.author Price, Daniel
dc.contributor.author Inoue, S.
dc.date.accessioned 2021-01-14T14:00:01Z
dc.date.available 2021-01-14T14:00:01Z
dc.date.issued 2020-12-21
dc.identifier.citation Vissers , G J M , Danilovic , S , de la Cruz Rodriguez , J , Leenaarts , J , Morosin , R , Diaz Baso , C , Reid , A , Pomoell , J , Price , D & Inoue , S 2020 , ' Non-LTE inversions of a confined X2.2 flare: I. Vector magnetic field in the photosphere and chromosphere : I. The vector magnetic field in the photosphere and chromosphere ' , Astronomy & Astrophysics , vol. 645 , 1 . https://doi.org/10.1051/0004-6361/202038900 en
dc.identifier.issn 1432-0746
dc.identifier.other PURE: 151321247
dc.identifier.other PURE UUID: 9b9ad0bb-ad0e-4d0a-a47e-c463b9c337fe
dc.identifier.other WOS: 000601180900001
dc.identifier.other ORCID: /0000-0003-1175-7124/work/86937290
dc.identifier.other ORCID: /0000-0002-8065-2847/work/86940612
dc.identifier.uri http://hdl.handle.net/10138/324592
dc.description.abstract Obtaining the magnetic field vector accurately in the solar atmosphere is essential for studying changes in field topology during flares and to reliably model space weather. We tackle this problem by applying various inversion methods to a confined X2.2 flare in NOAA AR 12673 on September 6, 2017, comparing the photospheric and chromospheric magnetic field vector with those from two numerical models of this event. We obtain the photospheric field from Milne-Eddington (ME) and (non-)local thermal equilibrium (non-LTE) inversions of Hinode SOT/SP Fe I 6301.5Å and 6302.5Å. The chromospheric field is obtained from a spatially-regularised weak field approximation (WFA) and non-LTE inversions of Ca II 8542Å observed with CRISP at the Swedish 1-m Solar Telescope. The LTE- and non-LTE-inferred photospheric field components are strongly correlated throughout the atmosphere, with stronger field and higher temperatures in the non-LTE inversions. For the chromospheric field, the non-LTE inversions correlate well with the spatially-regularised WFA. We find strong-field patches of over 4.5 kG in the photosphere, co-located with similar concentrations exceeding 3 kG in the chromosphere. The obtained field strengths are up to 2-3 times higher than in the numerical models, with more concentrated and structured photosphere-to-chromosphere shear close to the polarity inversion line. The LTE and non-LTE Fe I inversions yield essentially the same photospheric field, while ME inversions fail to reproduce the field vector orientation where Fe I is in emission. Our inversions confirm the locations of flux rope footpoints that are predicted by numerical models. However, pre-processing and lower spatial resolution lead to weaker and smoother field in the models than what the data indicate. This emphasises the need for higher spatial resolution in the models to better constrain pre-eruptive flux ropes. en
dc.format.extent 15
dc.language.iso eng
dc.relation.ispartof Astronomy & Astrophysics
dc.relation.uri https://arxiv.org/abs/2009.01537
dc.rights en
dc.subject 115 Astronomy, Space science en
dc.title Non-LTE inversions of a confined X2.2 flare: I. Vector magnetic field in the photosphere and chromosphere : I. The vector magnetic field in the photosphere and chromosphere en
dc.type Article
dc.description.version Peer reviewed
dc.identifier.doi https://doi.org/10.1051/0004-6361/202038900
dc.type.uri info:eu-repo/semantics/other
dc.type.uri info:eu-repo/semantics/publishedVersion
dc.contributor.pbl
dc.contributor.pbl
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