Publication:
The behaviour of the excess Ca II H and K and H_ε emissions in chromospherically active binaries

dc.contributor.authorMontes Gutiérrez, David
dc.contributor.authorFernández Figueroa, María José
dc.contributor.authorCornide Castro-Piñeiro, Manuel
dc.contributor.authorCastro Rubio, Elisa de
dc.date.accessioned2023-06-20T20:07:36Z
dc.date.available2023-06-20T20:07:36Z
dc.date.issued1996-08
dc.description© 1996 EDP Sciencies. We thank F. Martín for the C iv ux measurements in IUE spectra retrieved from ULDA. We would also like to thank Dr. B. Montesinos for the very careful reading of the manuscript and the referee S. Catalano for suggesting several improvements and clarifications. This work has been supported by the Universidad Complutense de Madrid and the Spanish Dirección General de Investigación Científica y Técnica (DGICYT) under grant PB94-0263.
dc.description.abstractIn this work we analyze the behaviour of the excess Ca II H and K and H_ ε emissions in a sample of 73 chromospherically active binary systems (RS CVn and BY Dra classes), of different activity levels and luminosity classes. This sample includes the 53 stars analyzed by Fernandez-Figueroa et al. (1994) and the observations of 28 systems described by Montes et al. (1995c). By using the spectral subtraction technique (subtraction of a synthesized stellar spectrum constructed from reference stars of spectral type and luminosity class similar to those of the binary star components) we obtain the active-chromosphere contribution to the Ca II H and K lines in these 73 systems. We have determined the excess Ca II H and K emission equivalent widths and converted them into surface fluxes. The emissions arising from each component were obtained when it was possible to deblend both contributions. We have found that the components of active binaries are generally stronger emitters than single active stars for a given effective temperature and rotation rate. A slight decline of the excess Ca II H and K emissions towards longer rotation periods, P-rot, and larger Rossby numbers, R_0, is found. When we use R_0 instead of P_rot, the scatter is reduced and a saturation at R_0≈0.3 is observed. A good correlation between the excess Ca II K and H_ ε chromospheric emission fluxes has been found. The correlations obtained between the excess Ca II K emission and other activity indicators, (C IV in the transition region, and X-rays in the corona) indicate that the exponents of the power-law relations increase with the formation temperature of the spectral features.
dc.description.departmentDepto. de Física de la Tierra y Astrofísica
dc.description.facultyFac. de Ciencias Físicas
dc.description.refereedTRUE
dc.description.sponsorshipUniversidad Complutense de Madrid (UCM)
dc.description.sponsorshipDirección General de Investigación Científica y Técnica (DGICYT), España
dc.description.sponsorshipMinisterio de Economía y Competitividad (MINECO), España
dc.description.statuspub
dc.eprint.idhttps://eprints.ucm.es/id/eprint/31052
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dc.identifier.issn0004-6361
dc.identifier.officialurlhttp://arxiv.org/pdf/astro-ph/9511125v1.pdf
dc.identifier.relatedurlhttp://www.aanda.org/
dc.identifier.urihttps://hdl.handle.net/20.500.14352/59620
dc.issue.number1
dc.journal.titleAstronomy and astrophysics
dc.language.isoeng
dc.page.final233
dc.page.initial221
dc.publisherEDP Sciencies
dc.relation.projectIDPB94-0263
dc.rights.accessRightsopen access
dc.subject.cdu52
dc.subject.keywordRS-canum-venaticorum
dc.subject.keywordMain-sequence stars
dc.subject.keywordSolar-type stars
dc.subject.keywordCool stars
dc.subject.keywordMagnetic-structure
dc.subject.keywordAlpha emission
dc.subject.keywordStellar activity
dc.subject.keywordSynchronized binaries
dc.subject.keywordRadiative losses
dc.subject.keywordBy-draconis
dc.subject.ucmAstrofísica
dc.subject.ucmAstronomía (Física)
dc.titleThe behaviour of the excess Ca II H and K and H_ε emissions in chromospherically active binaries
dc.typejournal article
dc.volume.number312
dspace.entity.typePublication
relation.isAuthorOfPublication2dfe4286-12c7-4d3a-bfda-d298a90cc8fe
relation.isAuthorOfPublication69d74cdf-f618-484d-b812-aabbd99a993c
relation.isAuthorOfPublication7fb65e4f-6cd8-40f1-88c3-23f46fc271af
relation.isAuthorOfPublication.latestForDiscovery2dfe4286-12c7-4d3a-bfda-d298a90cc8fe
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