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dc.contributor.authorBarklem, PS
dc.contributor.authorOsorio, Y
dc.contributor.authorFursa, DV
dc.contributor.authorBray, I
dc.contributor.authorZatsarinny, O
dc.contributor.authorBartschat, K
dc.contributor.authorJerkstrand, A
dc.date.accessioned2020-10-13T01:19:24Z
dc.date.available2020-10-13T01:19:24Z
dc.date.issued2017
dc.identifier.issn1432-0746en_US
dc.identifier.doi10.1051/0004-6361/201730864en_US
dc.identifier.urihttp://hdl.handle.net/10072/398310
dc.description.abstractResults of calculations for inelastic e+Mg effective collision strengths for the lowest 25 physical states of Mg i (up to 3s6p1P), and thus 300 transitions, from the convergent close-coupling (CCC) and the B-spline R-matrix (BSR) methods are presented. At temperatures of interest, ~5000 K, the results of the two calculations differ on average by only 4%, with a scatter of 27%. As the methods are independent, this suggests that the calculations provide datasets for e+Mg collisions accurate to this level. Comparison with the commonly used dataset compiled by Mauas et al. (1988, ApJ, 330, 1008), covering 25 transitions among 12 states, suggests the Mauas et al. data are on average ~57% too low, and with a very large scatter of a factor of ~6.5. In particular the collision strength for the transition corresponding to the Mg i intercombination line at 457 nm is significantly underestimated by Mauas et al., which has consequences for models that employ this dataset. In giant stars the new data leads to a stronger line compared to previous non-LTE calculations, and thus a reduction in the non-LTE abundance correction by ~0.1 dex (~25%). A non-LTE calculation in a supernova ejecta model shows this line becomes significantly stronger, by a factor of around two, alleviating the discrepancy where the 457 nm line in typical models with Mg/O ratios close to solar tended to be too weak compared to observations.en_US
dc.description.peerreviewedYesen_US
dc.languageEnglishen_US
dc.language.isoeng
dc.publisherEDP Sciencesen_US
dc.relation.ispartofpagefrom11en_US
dc.relation.ispartofjournalAstronomy & Astrophysicsen_US
dc.relation.ispartofvolume606en_US
dc.subject.fieldofresearchAstronomical and Space Sciencesen_US
dc.subject.fieldofresearchcode0201en_US
dc.subject.keywordsScience & Technologyen_US
dc.subject.keywordsPhysical Sciencesen_US
dc.subject.keywordsAstronomy & Astrophysicsen_US
dc.subject.keywordsatomic dataen_US
dc.subject.keywordsatomic processesen_US
dc.titleInelastic e+Mg collision data and its impact on modelling stellar and supernova spectraen_US
dc.typeJournal articleen_US
dc.type.descriptionC1 - Articlesen_US
dcterms.bibliographicCitationBarklem, PS; Osorio, Y; Fursa, DV; Bray, I; Zatsarinny, O; Bartschat, K; Jerkstrand, A, Inelastic e+Mg collision data and its impact on modelling stellar and supernova spectra, Astronomy & Astrophysics, 2017, 606, pp. 11en_US
dc.date.updated2020-10-13T01:01:25Z
dc.description.versionVersion of Record (VoR)en_US
gro.rights.copyright© 2017 EDP Sciences. The attached file is reproduced here in accordance with the copyright policy of the publisher. The original publication is available at www.europhysicsnews.org/en_US
gro.hasfulltextFull Text
gro.griffith.authorBartschat, Klaus


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