Volume 507, Number 2, November IV 2009
|Page(s)||929 - 937|
|Section||Stellar structure and evolution|
|Published online||15 September 2009|
Orbital periods of cataclysmic variables identified by the SDSS*
VI. The 4.5-h period eclipsing system SDSS J100658.40+233724.4
Department of Physics, University of Warwick, Coventry, CV4 7AL, UK e-mail: email@example.com
2 Departamento de Física y Astronomía, Universidad de Valparaíso, Avenida Gran Bretana 1111, Valparaíso, Chile
3 Isaac Newton Group of Telescopes, Apdo. de Correos 321, 38700 Santa Cruz de La Palma, Spain
4 Instituto de Astrofísica de Canarias, vía Líctea, s/n, La Laguna, 38205 Tenerife, Spain
Accepted: 13 September 2009
We present time-resolved spectroscopy and photometry of SDSS J100658.40+233724.4, which we have discovered to be an eclipsing cataclysmic variable with an orbital period of 0.18591324 days (267.71507 min). The observed velocity amplitude of the secondary star is km s-1, which an irradiation correction reduces to km s-1. Doppler tomography of emission lines from the infrared calcium triplet supports this measurement. We have modelled the light curve using the lcurve code and Markov Chain Monte Carlo simulations, finding a mass ratio of . From the velocity amplitude and the light curve analysis we find the mass of the white dwarf to be and the masses and radii of the secondary star to be and , respectively. The secondary component is less dense than a normal main sequence star but its properties are in good agreement with the expected values for a CV of this orbital period. By modelling the spectral energy distribution of the system we find a distance of pc and estimate a white dwarf effective temperature of K.
Key words: stars: novae, cataclysmic variables / stars: dwarf novae / stars: binaries: eclipsing / stars: binaries: spectroscopic / stars: white dwarfs / stars: individual: SDSS J100658.40+233724
© ESO, 2009
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