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Red Spectroscopy of IP Pegasi

Published online by Cambridge University Press:  12 April 2016

J.S. Martin ,
D.H.P. Jones  and
R.C Smith
J.S. Martin
Affiliation:
Astronomy Centre and Royal Greenwich Observatory, Herstmonceux Castle, East Sussex, U.K.
D.H.P. Jones
Affiliation:
Royal Greenwich Observatory, Herstmonceux Castle, East Sussex, U.K.
R.C Smith
Affiliation:
Astronomy Centre, University of Sussex, Brighton, U.K.

Abstract

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Time resolved spectroscopy of the dwarf nova IP Pegasi in the range λλ 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 0.62 < M1 < 1.14M⊙ and 0.17 < M2 < 0.71M⊙. The red star has a radius in the range 0.32 < R2 < 0.51R⊙ and is probably on the main sequence.

Type
II. Radio, IR and Optical Observations
Information
International Astronomical Union Colloquium , Volume 93: Cataclysmic Variables: Recent Multi-Frequency Observations and Theoretical Developments , 1987 , pp. 145 - 149
Copyright
Copyright © Reidel 1987

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