Bibcode
Southworth, J.; Hickman, R. D. G.; Marsh, T. R.; Rebassa-Mansergas, A.; Gänsicke, B. T.; Copperwheat, C. M.; Rodríguez-Gil, P.
Bibliographical reference
Astronomy and Astrophysics, Volume 507, Issue 2, 2009, pp.929-937
Advertised on:
11
2009
Journal
Citations
29
Refereed citations
26
Description
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 276 ± 7 km s-1, which an irradiation correction
reduces to 258 ± 12 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 0.51
± 0.08. From the velocity amplitude and the light curve analysis
we find the mass of the white dwarf to be 0.78 ± 0.12 {{M}_&sun;}
and the masses and radii of the secondary star to be 0.40 ± 0.10
{{M}_&sun;} and 0.466 ± 0.036 {{R}_&sun;}, 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 676 ± 40 pc and estimate a white
dwarf effective temperature of 16 500 ± 2000 K.
Spectra are only available in electronic form at the CDS via anonymous
ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via
http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/507/929
Related projects
Binary Stars
The study of binary stars is essential to stellar astrophysics. A large number of stars form and evolve within binary systems. Therefore, their study is fundamental to understand stellar and galactic evolution. Particularly relevant is that binary systems are still the best source of precise stellar mass and radius measurements. Research lines
Pablo
Rodríguez Gil