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Colección SciELO Chile

Fundamental Parameters of the Eclipsing Binary TU Canis Majoris

Indexado

WoS	WOS:000398666300001
Scopus	SCOPUS_ID:85015885910

DOI

10.1088/1538-3873/AA5B7F

Año

2017

Tipo

artículo de investigación

Citas Totales

Autores Afiliación Chile

Instituciones Chile

% Participación
Internacional

Autores
Afiliación Extranjera

Instituciones
Extranjeras

Abstract

We present a spectroscopic and photometric study of the eclipsing binary TU Canis Majoris aimed to obtain their fundamental stellar parameters and evolutionary stage. Our results indicate that the masses, radii, temperatures, and luminosities for the primary and secondary stars are: M-1 = 1.761 +/- 0.012 M-circle dot, M-2 = 1.144 +/- 0.010 M-circle dot, R-1 = 1.553 +/- 0.002 M-circle dot, R-2 = 1.075 +/- 0.002 R-circle dot, T-1 = 8014 +/- 151. K, T-2 = 6060 +/- 100 K, L-1 = 8.913 +/- 0.695 L-circle dot, and L-2 = 1.396 +/- 0.097 L-circle dot. We estimate an age for the system of tau = 2.11 +/- 0.24 x 10(8) years, and a distance of d = 324.81 +/- 12.86 pc. In addition, we note that none of the components has filled their respective Roche lobe and both are on the main sequence.

Revista

Revista	ISSN
Publications Of The Astronomical Society Of The Pacific	0004-6280

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Disciplinas de Investigación

WOS
Astronomy & Astrophysics

Scopus
Sin Disciplinas

SciELO
Sin Disciplinas

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Publicaciones WoS (Ediciones: ISSHP, ISTP, AHCI, SSCI, SCI), Scopus, SciELO Chile.

Colaboración Institucional

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Autores - Afiliación

Ord.	Autor	Género	Institución - País
1	GARCES-LETELIER, JUAN ISAIAS	Hombre	Universidad de Concepción - Chile
2	MENNICKENT-CID, RONALD ENRIQUE	Hombre	Universidad de Concepción - Chile Centro de Excelencia en Astrofísica y Tecnologías Afines - Chile
3	Zharikov, Sergey	Hombre	Univ Nacl Autonoma Mexico - México Universidad Nacional Autónoma de México - México

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Financiamiento

Fuente
BASAL Centro de Astrofisica y Tecnologias Afines (CATA)
VRID-Enlace
CONACyT Grant
Polish KBN grant
DGAPA/PAPIIT project

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Agradecimientos

Agradecimiento
We thank the anonymous referee who reviewed the first version of this manuscript. J.G.L. acknowledges the comments of members of stellar variability group (S.V.G. UdeC) that helped to improve the first version of this study. R.E.M. and J.G.L. acknowledge support by VRID-Enlace 216.016.002-1.0 and the BASAL Centro de Astrofisica y Tecnologias Afines (CATA) PFB-06/2007. S.Z. acknowledges support from DGAPA/PAPIIT project IN100614 and CONACyT grant CAR 208512. We acknowledge the use of data from ASAS database, supported by the Polish KBN 2P03D02024 grant. This work has made use of data from the European Space Agency (ESA) mission Gaia (http://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, http://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.

Agradecimiento

We thank the anonymous referee who reviewed the first version of this manuscript. J.G.L. acknowledges the comments of members of stellar variability group (S.V.G. UdeC) that helped to improve the first version of this study. R.E.M. and J.G.L. acknowledge support by VRID-Enlace 216.016.002-1.0 and the BASAL Centro de Astrofisica y Tecnologias Afines (CATA) PFB-06/2007. S.Z. acknowledges support from DGAPA/PAPIIT project IN100614 and CONACyT grant CAR 208512. We acknowledge the use of data from ASAS database, supported by the Polish KBN 2P03D02024 grant. This work has made use of data from the European Space Agency (ESA) mission Gaia (http://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, http://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.