Spectroscopic observations of the dwarf nova IP Pegasi

Details Spectroscopic observations of the dwarf nova IP Pegasi Spectroscopic observations of the dwarf nova IP Pegasi

Aug 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989aj.....98..675h&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 98, Aug. 1989, p. 675-685, 751.

Astronomy and Astrophysics

Astronomy

29

Accretion Disks, Astronomical Spectroscopy, Cataclysmic Variables, Dwarf Novae, Balmer Series, Carbon, Chromosphere, Emission Spectra, Helium, Line Spectra, Nitrogen, Radial Velocity

Scientific paper

Time-resolved spectroscopic measurements of IP Peg were obtained immediately after a dwarf nova eruption. The radio-velocity amplitude of the white dwarf (118 + or - 10 km/s) implied by measurements from the wings of the Balmer emission lines is different from that found previously. The results suggest a mass ratio M1/M2 of 0.435 + or - 0.052 and that the narrow component is due to unusually strong chromospheric emission from the late-type star. The low value for the radial-velocity amplitude of this narrow emission (about 200 km/s) is consistent with the observed absorption-line amplitude of 331 km/s if the irradiated surface of the M dwarf produces little line absorption.

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