Volume 409, Number 2, October II 2003
|Page(s)||647 - 657|
|Section||Stellar structure and evolution|
|Published online||17 November 2003|
Spectroscopy of the double-lined dwarf nova AT Ara*
Laboratório Nacional de Astrofísica, CP 21, 37500–000 Itajubá – MG, Brazil
Corresponding author: email@example.com
Accepted: 3 July 2003
The first time-resolved spectroscopic observations of the dwarf nova AT Ara are presented. The system is a double lined spectroscopic binary. Thus, radial velocity curves of both, emission lines from the accretion disk (in this particular case of Hα) and of the secondary star can be measured. An orbital period of 0.37551 days is derived, placing AT Ara among the cataclysmic variables with the longest revolution periods. The RV-amplitudes yield a mass ratio of . The spectral type of the secondary star is K2. AT Ara has an intermediate orbital inclination of . The secondary star has a mass and a radius of and , respectively. It is thus significantly larger than a main sequence star of the same mass. Evolutionary calculations of cataclysmic variables suggest that the secondary is nuclearly evolved to a certain degree. The distance to AT Ara is estimated to be of the order of 600 pc.
Key words: stars: binaries: close / stars: novae, cataclysmic variables / stars: individual: AT Ara
© ESO, 2003
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