Spectroscopy and photometry of IP Peg in the near-infrared

Details Spectroscopy and photometry of IP Peg in the near-infrared Spectroscopy and photometry of IP Peg in the near-infrared

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.224.1031m&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 224, Feb. 15, 1987, p. 1031-1042.

Astronomy and Astrophysics

Astronomy

33

Dwarf Novae, Eclipsing Binary Stars, Near Infrared Radiation, Stellar Spectrophotometry, Variable Stars, Eccentric Orbits, Radial Velocity, Radiant Flux Density, Spectral Resolution, Stellar Mass, Temporal Resolution

Scientific paper

Time-resolved spectroscopy in the range λλ7600 - 8300 Å of the dwarf nova IP Peg has been used to derive a radial velocity curve for the secondary star, with semi-amplitude K = 288.3±4 km s-1. The curve is slightly distorted, giving an orbit with an apparent eccentricity of 0.075±0.024. The radial velocity curve gives a mass function for the primary of 0.394±0.016 M_sun;. From this the authors derive constraints on the possible masses of the components and on the inclination of the system of i > 80°, 0.62 < M1 < 1.14 M_sun;, 0.17 < M2 < 0.71 M_sun;. Photometry in a wavelength band around 9300 Å shows the existence of a large ellipsoidal variation in the light from the secondary star.

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