First Chromospheric Activity and Doppler Imaging Study of PW And Using a New Doppler Imaging Code: SpotDIPy

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dc.authoridMontes, David/0000-0002-7779-238X
dc.authoridSenavci, Hakan Volkan/0000-0002-8961-277X
dc.authoridIsik, Emre/0000-0001-6163-0653
dc.authoridBAHAR, ENGIN/0000-0001-9119-2316
dc.authoridXiang, Yue/0000-0001-6580-9378
dc.contributor.authorBahar, Engin
dc.contributor.authorSenavci, Hakan V.
dc.contributor.authorIsik, Emre
dc.contributor.authorHussain, Gaitee A. J.
dc.contributor.authorKochukhov, Oleg
dc.contributor.authorMontes, David
dc.contributor.authorXiang, Yue
dc.date.accessioned2025-02-20T08:42:13Z
dc.date.available2025-02-20T08:42:13Z
dc.date.issued2024
dc.departmentTürk-Alman Üniversitesien_US
dc.description.abstractMeasuring the coverage of dark spots on cool stars is important to understanding how stellar magnetic activity scales with the rotation rate and convection zone depth. In this respect, it is crucial to infer surface magnetic patterns on G and K stars, to reveal solar-like stellar dynamos in action. Molecular bands serve as invaluable indicators of cool spots on the surfaces of stars, as they play a crucial role in enabling accurate assessments of the extent of spot coverage across the stellar surface. Therefore, more reliable surface images can be obtained considering the inversion of atomic lines with molecular bands. In this context, we simultaneously carry out Doppler imaging (DI) using atomic lines as well as titanium oxide band profiles of PW And (K2 V) and also investigate chromospheric activity indicators for the first time in the literature, using high-resolution spectra. The surface spot distribution obtained from the inversion process represents both atomic line and TiO-band profiles quite accurately. The chromospheric emission is also correlated with photospheric spot coverage, except during a possible flare event during the observations. We detect frequent flare activity, using TESS photometry. We also introduce a new open-source, Python-based DI code SpotDIPy that allows performing surface reconstructions of single stars using the maximum entropy method. We test the code by comparing surface reconstruction simulations with the extensively used DoTS code. We show that the surface brightness distribution maps reconstructed via both codes using the same simulated data are consistent with each other.
dc.description.sponsorshipScientific And Technological Research Council of Turkiye (TUBIdot;TAK) [1001-115F033]; Agencia Estatal de Investigacion of the Spanish Ministerio de Ciencia e Innovacion [PID2019-109522GB-C5[1:4]]; Swedish Research Council [2019-03548]; Swedish Research Council [2019-03548] Funding Source: Swedish Research Council
dc.description.sponsorshipWe would like to thank the referee, Dr. Klaus Strassmeier, whose critical comments led to substantial improvement of the manuscript. H.V.& Scedil;. acknowledges the support by The Scientific And Technological Research Council of Turkiye (TUB & Idot;TAK) through project No. 1001-115F033. D.M. acknowledges financial support from the Agencia Estatal de Investigacion of the Spanish Ministerio de Ciencia e Innovacion through project No. PID2019-109522GB-C5[1:4]/AEI/10.13039/501100011033. O.K. acknowledges support from the Swedish Research Council (project No. 2019-03548).
dc.identifier.doi10.3847/1538-4357/ad055d
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.issue1en_US
dc.identifier.scopus2-s2.0-85181120385
dc.identifier.scopusqualityQ1
dc.identifier.urihttps://doi.org/10.3847/1538-4357/ad055d
dc.identifier.urihttps://hdl.handle.net/20.500.12846/1561
dc.identifier.volume960en_US
dc.identifier.wosWOS:001128967000001
dc.identifier.wosqualityQ1
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherIop Publishing Ltd
dc.relation.ispartofAstrophysical Journal
dc.relation.publicationcategoryMakale - Uluslararası Hakemli Dergi - Kurum Öğretim Elemanı
dc.rightsinfo:eu-repo/semantics/openAccess
dc.snmzKA_WOS_20250220
dc.subjectRadial-Velocitiesen_US
dc.subjectYoungen_US
dc.subjectStarsen_US
dc.subjectAstropyen_US
dc.subjectDistributionsen_US
dc.subjectSpectroscopyen_US
dc.subjectAlgorithmen_US
dc.subjectPackageen_US
dc.subjectProjecten_US
dc.subjectMembersen_US
dc.titleFirst Chromospheric Activity and Doppler Imaging Study of PW And Using a New Doppler Imaging Code: SpotDIPy
dc.typeArticle

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