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Surface mapping of magnetic hot stars: Theories versus observations
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Observational Astronomy.
2018 (English)In: CONTRIBUTIONS OF THE ASTRONOMICAL OBSERVATORY SKALNATE PLESO, ISSN 1335-1842, Vol. 48, no 1, p. 58-65Article in journal (Refereed) Published
Abstract [en]

This review summarises results of recent magnetic and chemical abundance surface mapping studies of early-type stars. We discuss main trends uncovered by observational investigations and consider reliability of spectropolarimetric inversion techniques used to infer these results. A critical assessment of theoretical attempts to interpret empirical magnetic and chemical maps in the framework of, respectively, the fossil field and atomic diffusion theories is also presented. This confrontation of theory and observations demonstrates that 3D MHD models of fossil field relaxation are successful in matching the observed range of surface magnetic field geometries. At the same time, even the most recent time-dependent atomic diffusion calculations fail to reproduce diverse horizontal abundance distributions found in real magnetic hot stars.

Place, publisher, year, edition, pages
SLOVAK ACADEMY SCIENCES ASTRONOMICAL INST , 2018. Vol. 48, no 1, p. 58-65
Keywords [en]
stars: atmospheres, stars: chemically peculiar, stars: magnetic fields, starspots
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:uu:diva-357772ISI: 000432791300006OAI: oai:DiVA.org:uu-357772DiVA, id: diva2:1241058
Funder
Knut and Alice Wallenberg FoundationSwedish Research CouncilSwedish National Space BoardAvailable from: 2018-08-22 Created: 2018-08-22 Last updated: 2018-08-22Bibliographically approved

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CiteExportLink to record
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Citation style
  • apa
  • ieee
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  • vancouver
  • Other style
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  • de-DE
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  • en-US
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Output format
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