Red spectroscopy of IP Pegasi |
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| Authors: | J. S. Martin D. H. P. Jones R. C. Smith |
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| Affiliation: | (1) Astronomy Centre and Royal Greenwich Observatory, Herstmonceux Castle, East Sussex, U.K.;(2) Royal Greenwich Observatory, Herstmonceux Castle, East Sussex, U.K.;(3) Astronomy Centre, University of Sussex, Brighton, U.K. |
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| Abstract: | Time resolved spectroscopy of the dwarf nova IP Pegasi in the range  7670–8320Å shows absorption lines originating from the cool secondary. A radial velocity curve for this component has been derived by cross-correlation with a normal M star. The curve has semi-amplitude K2=288.3±4 km s–1, and is slightly distorted. This distortion is equivalent to an orbit with an apparent eccentricity of 0.075±0.024. The mass function of the primary is 0.394±0.016M . From this we derive constraints on the component masses of 0.621<1.14M and 0.172<0.71M. The red star has a radius in the range 0.322<0.51R and is probably on the main sequence.Paper presented at the IAU Colloquium No. 93 on  Cataclysmic Variables. Recent Multi-Frequency Observations and Theoretical Developments , held at Dr. Remeis-Sternwarte Bamberg, F.R.G., 16–19 June, 1986 |
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