Todd C. Hillwig et al. 2000 The Astronomical Journal 120 1113 doi:10.1086/301479
Todd C. Hillwig1, R. Kent Honeycutt1 and Jeff W. Robertson2
Show affiliationsWe 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.
Issue 2 (2000 August)
Received 2000 March 27, accepted for publication 2000 April 25
Todd C. Hillwig et al. 2000 The Astronomical Journal 120 1113
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