Post-common envelope pre-cataclysmic and cataclysmic variable binaries

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Cataclysmic, Binaries, Common Envelope

Scientific paper

Extensive photometric and spectroscopic observations have been obtained for the binary HS1136+6646, a newly formed post-common envelope binary system containing a hot ~DAO.5 primary and a highly irradiated secondary. H1136+6646 is the most extreme example yet of a class of short period systems containing a hot H-rich white dwarf with a K-M companion. An orbital period of 0.83607 +/- 0.00003 days has been determined through the phasing of radial velocities; emission line equivalent widths, and photometric measurements spanning a range of 24 months. Radial velocity measurements yield an amplitude of K WD = 69 +/- 2 km s -1 for the white dwarf and K K 7 V = 115 +/- 1 km s -1 for the secondary star. Photometric measurements revealed a low amplitude modulation with a period of 234 minutes, associated with the rotation of the white dwarf. The white dwarf is estimated to have an effective temperature and gravity of ~100,000 K and log g ~ 8.29 respectively; indicating the binary system is the second earliest post-CE objects known; having an age around 6.4x10 5 years. Indications are that the secondary star is overly luminous for its mass.
I also present FUSE observations of the magnetic cataclysmic variable V405 Aurigae. Together with four other DQ Her type binaries, V405 Aur forms a small subclass of intermediate polars which are likely to evolve into low magnetic field strength polars. The FUSE spectrum exhibits broad O VI and C III emission-lines as well as a narrow O VI emission-line component which likely forms near the white dwarf surface in an optically thin gas. Radial velocity measurements restrict any orbital modulation to a very low amplitude (K WD 2.5 +/- 0.5 km s -1 ) indicating that the binary system is at low inclination.
Recent photometric and spectroscopic observations have revealed J0644+3344 to be a bright, deeply eclipsing cataclysmic variable binary with a 6.46488+/-0.00024 hour period. Although the nature of the hot component is not presently clear, J0644+3344 is one of the brightest eclipsing nova-like cataclysmic variable system yet. As such, the possibility exists for an unambiguous determination of the masses and temperatures of both components in fixture studies.

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