Details

Autor(en) / Beteiligte

• van den Besselaar, E. J. M.
• Greimel, R.
• Morales-Rueda, L.
• Nelemans, G.
• Thorstensen, J. R.
• Marsh, T. R.
• Dhillon, V. S.
• Robb, R. M.
• Balam, D. D.
• Guenther, E. W.
• Kemp, J.
• Augusteijn, T.
• Groot, P. J.

Titel

DE Canum Venaticorum: a bright, eclipsing red dwarf–white dwarf binary

Ist Teil von

• Astronomy and astrophysics (Berlin), 2007-05, Vol.466 (3), p.1031-1041

Erscheinungsjahr

2007

Quelle

EZB Electronic Journals Library

Beschreibungen/Notizen

• Context. Close white dwarf-red dwarf binaries must have gone through a common-envelope phase during their evolution. de CVn is a detached white dwarf-red dwarf binary with a relatively short ( similar to 8.7 h) orbital period. Its brightness and the presence of eclipses makes this system ideal for a more detailed study. Aims. From a study of photometric and spectroscopic observations of de CVn we derive the system parameters that we discuss in the framework of common-envelope evolution. Methods. Photometric observations of the eclipses are used to determine an accurate ephemeris. From a model fit to an average low-resolution spectrum of de CVn, we constrain the temperature of the white dwarf and the spectral type of the red dwarf. The eclipse light curve is analysed and combined with the radial velocity curve of the red dwarf determined from time-resolved spectroscopy to derive constraints on the inclination and the masses of the components in the system. Results. The derived ephemeris is HJD _{\rm min} = 2 452 784.5533(1) + 0.3641394(2) \times E. The red dwarf in de CVn has a spectral type of M3V and the white dwarf has an effective temperature of 8\,000 K. The inclination of the system is 86+3 \circ}_ and the mass and radius of the red dwarf are 0.41\pm 0.06 M_{\odot} and 0.37 super(+0.06) sub(-0.007) R_{\odot}, respectively, and the mass and radius of the white dwarf are 0.51 super(+0.06) sub(-0.02) M_{\odot} and 0.0136 super(+0.0008) sub(-0.0002) R_{\odot}, respectively. Conclusions. We found that the white dwarf has a hydrogen-rich atmosphere (DA-type). Given that de CVn has experienced a common-envelope phase, we can reconstruct its evolution and we find that the progenitor of the white dwarf was a relatively low-mass star ( M\leq 1.6 similar to M_{\odot}). The current age of this system is 3.3{- }7.3\times 10 { years, while it will take longer than the Hubble time for de CVn to evolve into a semi-detached system.