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

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

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...196.4501h&link_type=abstract

American Astronomical Society, 196th AAS Meeting, #45.01; Bulletin of the American Astronomical Society, Vol. 32, p.744

Astronomy and Astrophysics

Astronomy

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 of P=1.75992 d 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/M_1≈ 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 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 Pre-Cataclysmic Binary stars is also reviewed.

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