Red spectroscopy of IP Pegasi

Details Red spectroscopy of IP Pegasi Red spectroscopy of IP Pegasi

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987ap%26ss.130..145m&link_type=abstract

(IAU, DFG, and Bayerisches Staatsministerium für Unterricht und Kultus, Colloquium on Cataclysmic Variables, Recent Multi-Freque

Astronomy and Astrophysics

Astrophysics

1

Cataclysmic Variables, Dwarf Novae, Eclipsing Binary Stars, Radial Velocity, Stellar Orbits, Stellar Spectra, Cool Stars, Stellar Mass

Scientific paper

Time resolved spectroscopy of the dwarf nova IP Pegasi in the range λλ7670 - 8320 Å 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±0.016 M_sun;. From this the authors derive constraints on the component masses of 0.62 < M1 < 1.14 M_sun; and 0.17 < M2 < 0.71 M_sun;. The red star has a radius in the range 0.32 < R2 < 0.51 R_sun; and is probably on the main sequence.

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