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Chemical abundances on the secondary star in the low-mass x-ray binary Cygnus X-2

Published online by Cambridge University Press:  25 February 2014

L. Suárez-Andrés ,
J.I. González Hernández ,
G. Israelian ,
J. Casares  and
R. Rebolo
L. Suárez-Andrés
Affiliation:
Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain Depto. Astrofísica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, Spain
J.I. González Hernández
Affiliation:
Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain Depto. Astrofísica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, Spain
G. Israelian
Affiliation:
Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain Depto. Astrofísica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, Spain
J. Casares
Affiliation:
Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain Depto. Astrofísica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, Spain
R. Rebolo
Affiliation:
Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain Depto. Astrofísica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, Spain Consejo Superior de Investigaciones Científicas, Spain
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Abstract

We present our first results in the analysis of the secondary star in the Low-Mass X-Ray binary (LMXB) Cygnus X-2, using a high resolution spectrum obtained with UES@WHT in ORM (La Palma, Tenerife). We have used a χ2 minimization procedure to create a grid of 1 500 000 LTE synthetic spectra that allow us to obtain a plausible range of values of the stellar parameters, taking into account any possible veiling from the accretion disk produced by the presence of a neutron star as the primary. We will study the chemical abundances of several elements and study their anomalies regarding Galactic trends.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 64: Setting a New Standard in the Analysis of Binary Stars , 2013 , pp. 253 - 256
Copyright
© EAS, EDP Sciences, 2014

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References

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