MY Camelopardalis, a very massive merger progenitor

Por favor, use este identificador para citar o enlazar este ítem: http://hdl.handle.net/10045/43247
Registro completo de metadatos
Registro completo de metadatos
Campo DCValorIdioma
dc.contributorAstrofísica Estelar (AE)es
dc.contributor.authorLorenzo Espinosa, Javier-
dc.contributor.authorNegueruela, Ignacio-
dc.contributor.authorVal Baker, Amira-
dc.contributor.authorGarcía, Miriam-
dc.contributor.authorSimón Díaz, Sergio-
dc.contributor.authorPastor Seva, Pedro-
dc.contributor.authorMéndez Majuelos, Manuel-
dc.contributor.otherUniversidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señales
dc.contributor.otherUniversidad de Alicante. Departamento de Lenguajes y Sistemas Informáticoses
dc.date.accessioned2014-12-11T10:23:34Z-
dc.date.available2014-12-11T10:23:34Z-
dc.date.issued2014-12-04-
dc.identifier.citationAstronomy & Astrophysics. 2014, 572: A110. doi:10.1051/0004-6361/201424345es
dc.identifier.issn0004-6361 (Print)-
dc.identifier.issn1432-0746 (Online)-
dc.identifier.urihttp://hdl.handle.net/10045/43247-
dc.description.abstractContext. The early-type binary MY Cam belongs to the young open cluster Alicante 1, embedded in Cam OB3. Aims. MY Cam consists of two early-O type main-sequence stars and shows a photometric modulation suggesting an orbital period slightly above one day. We intend to confirm this orbital period and derive orbital and stellar parameters. Methods. Timing analysis of a very exhaustive (4607 points) light curve indicates a period of 1.1754514 ± 0.0000015 d. High-resolution spectra and the cross-correlation technique implemented in the todcor program were used to derive radial velocities and obtain the corresponding radial velocity curves for MY Cam. Modelling with the stellar atmosphere code fastwind was used to obtain stellar parameters and create templates for cross-correlation. Stellar and orbital parameters were derived using the Wilson-Devinney code, such that a complete solution to the binary system could be described. Results. The determined masses of the primary and secondary stars in MY Cam are 37.7 ± 1.6 and 31.6 ± 1.4M⊙, respectively. The corresponding temperatures, derived from the model atmosphere fit, are 42 000 and 39 000 K, with the more massive component being hotter. Both stars are overfilling their Roche lobes, sharing a common envelope. Conclusions. MY Cam contains the most massive dwarf O-type stars found so far in an eclipsing binary. Both components are still on the main sequence, and probably not far from the zero-age main sequence. The system is a likely merger progenitor, owing to its very short period.es
dc.description.sponsorshipThis research is partially supported by the Spanish Ministerio de Economía y Competitividad under grant AYA2012-39364-C02-01/02, and the European Union.es
dc.languageenges
dc.publisherEDP Scienceses
dc.rights© ESO, 2014es
dc.subjectBinaries: spectroscopices
dc.subjectBinaries: eclipsinges
dc.subjectStars: massivees
dc.subjectStars: early-typees
dc.subject.otherAstronomía y Astrofísicaes
dc.titleMY Camelopardalis, a very massive merger progenitores
dc.typeinfo:eu-repo/semantics/articlees
dc.peerreviewedsies
dc.identifier.doi10.1051/0004-6361/201424345-
dc.relation.publisherversionhttp://dx.doi.org/10.1051/0004-6361/201424345es
dc.rights.accessRightsinfo:eu-repo/semantics/openAccesses
dc.relation.projectIDinfo:eu-repo/grantAgreement/MINECO//AYA2012-39364-C02-01-
dc.relation.projectIDinfo:eu-repo/grantAgreement/MINECO//AYA2012-39364-C02-02-
Aparece en las colecciones:INV - Astrofísica Estelar - Artículos de Revistas

Archivos en este ítem:
Archivos en este ítem:
Archivo Descripción TamañoFormato 
Thumbnail2014_Lorenzo_etal_A&A.pdf1,49 MBAdobe PDFAbrir Vista previa


Todos los documentos en RUA están protegidos por derechos de autor. Algunos derechos reservados.