Post-Common-Envelope Binary Stars and the Precataclysmic Binary PG 1114+187

Details Post-Common-Envelope Binary Stars and the Precataclysmic Binary PG 1114+187 Post-Common-Envelope Binary Stars and the Precataclysmic Binary PG 1114+187

Aug 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aj....120.1113h&link_type=abstract

The Astronomical Journal, Volume 120, Issue 2, pp. 1113-1119.

Astronomy and Astrophysics

Astronomy

23

Stars: Binaries: Close, Stars: Individual (Pg 1114+187)

Scientific paper

We present orbit-resolved spectroscopy and orbit-sampled photometry of the binary system PG 1114+187. Both photometry and radial velocity studies reveal a period P=1.75992 days, which is taken to be the orbital period of the binary. Strong modulation of emission-line strength with the same period is also present. A preliminary mass ratio, M2/M1~0.7, is found from primary- and secondary-star radial velocity amplitudes. No evidence is seen for either an accretion disk or mass transfer, leading to the conclusion that PG 1114+187 is not a cataclysmic variable (CV) but is in a pre-CV state, before the initiation of mass transfer. The short orbital period also leads to the conclusion that the system passed through a common-envelope phase at some time in the past. The current list of known post-common-envelope and precataclysmic binary stars is also reviewed and the general properties of this class of star are discussed.

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