Forward modelling of brightness variations in Sun-like stars II. Light curves and variability

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dc.authoridShapiro, Alexander/0000-0002-8842-5403
dc.authoridReinhold, Timo/0000-0002-1299-1994
dc.contributor.authorNemec, N. -E.
dc.contributor.authorShapiro, A. I.
dc.contributor.authorIsik, E.
dc.contributor.authorSolanki, S. K.
dc.contributor.authorReinhold, T.
dc.date.accessioned2025-02-20T08:42:17Z
dc.date.available2025-02-20T08:42:17Z
dc.date.issued2023
dc.departmentTürk-Alman Üniversitesien_US
dc.description.abstractContext. The amplitude and morphology of light curves of Sun-like stars change substantially with increasing rotation rate: brightness variations are amplified and become more regular. This has not been explained so far.Aims. We develop a modelling approach for calculating brightness variations of stars with various rotation rates and use it to explain the observed trends in stellar photometric variability.Methods. We combined numerical simulations of magnetic flux emergence and transport with a model for stellar brightness variability to calculate synthetic light curves of stars as observed by the Kepler telescope. We computed the distribution of the magnetic flux on the stellar surface for various rotation rates and degrees of active-region nesting (i.e. the tendency of active regions to emerge in the vicinity of recently emerged regions). Using the resulting maps of the magnetic flux, we computed the rotational variability of our simulated stellar light curves as a function of rotation rate and nesting of magnetic features and compared our calculations to Kepler observations.Results. We show that both the rotation rate and the degree of nesting have a strong impact on the amplitude and morphology of stellar light curves. In order to explain the variability of most of the Kepler targets with known rotation rates, we need to increase the degree of nesting to values that are much higher than the values on the Sun.Conclusions. The suggested increase in nesting with the rotation rate can provide clues about the flux emergence process for high levels of stellar activity.
dc.description.sponsorshipEuropean Research Council under the European Union's Horizon 2020 research and innovation program [715947]
dc.description.sponsorshipThe research leading to this paper has received funding from the European Research Council under the European Union's Horizon 2020 research and innovation program (grant agreement No. 715947).
dc.identifier.doi10.1051/0004-6361/202244412
dc.identifier.issn0004-6361
dc.identifier.issn1432-0746
dc.identifier.scopus2-s2.0-85153050136
dc.identifier.scopusqualityQ1
dc.identifier.urihttps://doi.org/10.1051/0004-6361/202244412
dc.identifier.urihttps://hdl.handle.net/20.500.12846/1626
dc.identifier.volume672en_US
dc.identifier.wosWOS:000973403600007
dc.identifier.wosqualityQ1
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherEdp Sciences S A
dc.relation.ispartofAstronomy & Astrophysics
dc.relation.publicationcategoryMakale - Uluslararası Hakemli Dergi - Kurum Öğretim Elemanı
dc.rightsinfo:eu-repo/semantics/openAccess
dc.snmzKA_WOS_20250220
dc.subjectstars: activityen_US
dc.subjectstars: generalen_US
dc.subjectstars: rotationen_US
dc.subjectstars: magnetic fielden_US
dc.subjectstars: solar-typeen_US
dc.titleForward modelling of brightness variations in Sun-like stars II. Light curves and variability
dc.typeArticle

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