Modelling the light variability of the Ap star epsilon Ursae Majoris

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dc.contributor.author Shulyak, D.
dc.contributor.author Krtička, Jiří
dc.contributor.author Mikulášek, Zdeněk
dc.contributor.author Kochukhov, O.
dc.contributor.author Lüftinger, T.
dc.date.accessioned 2011-01-12T07:46:32Z
dc.date.available 2011-01-12T07:46:32Z
dc.date.issued 2010
dc.identifier.citation Astronomy & astrophysics. 2010, vol. 524, art. no. A66. en
dc.identifier.issn 0004-6361
dc.identifier.issn 1432-0746
dc.identifier.uri http://hdl.handle.net/10084/83556
dc.description.abstract Aims. We simulate the light variability of the Ap star ε UMa using the observed surface distributions of Fe, Cr, Ca, Mn, Mg, Sr, and Ti obtained with the help of the Doppler imaging technique. Methods. Using all photometric data available, we specified light variations of ε UMa modulated by its rotation from far UV to IR. We employed the LLmodels stellar model atmosphere code to predict the light variability in different photometric systems. Results. The rotational period of ε UMa is refined to 5088631(18). It is shown that the observed light variability can be explained as a result of the redistribution of radiative flux from the UV spectral region to the visual caused by the inhomogeneous surface distribution of chemical elements. Among seven mapped elements, only Fe and Cr contribute significantly to the amplitude of the observed light variability. In general, we find very good agreement between theory and observations. We confirm the important role of Fe and Cr in determining the magnitude of the well-known depression around 5200 Å by analyzing the peculiar a-parameter. Finally, we show that the abundance spots of considered elements cannot explain the observed variabilities in near UV and β index, which probably have other causes. Conclusions. The inhomogeneous surface distribution of chemical elements can explain most of the observed light variability of the A-type CP star ε UMa. en
dc.language.iso en en
dc.publisher EDP Sciences en
dc.relation.ispartofseries Astronomy & astrophysics en
dc.relation.uri http://dx.doi.org/10.1051/0004-6361/201015094 en
dc.subject stars: chemically peculiar en
dc.subject stars: variables: general en
dc.subject stars: atmospheres en
dc.subject stars: individual: ε UMa en
dc.title Modelling the light variability of the Ap star epsilon Ursae Majoris en
dc.type Article en
dc.identifier.location Není ve fondu ÚK en
dc.identifier.doi 10.1051/0004-6361/201015094
dc.identifier.wos 000284625300056

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