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T. Hillwig, R. K. Honeycutt (Indiana U.), J. Robertson (Arkansas Tech U.)
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/M1\approx 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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