Evidence for a high-mass white dwarf in nova V1500 Cygni 1975

Details Evidence for a high-mass white dwarf in nova V1500 Cygni 1975 Evidence for a high-mass white dwarf in nova V1500 Cygni 1975

Aug 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...343..888h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 343, Aug. 15, 1989, p. 888-901.

Astronomy and Astrophysics

Astrophysics

25

Binary Stars, Novae, Stellar Spectra, White Dwarf Stars, Balmer Series, Emission Spectra, Light Curve, Line Spectra, Radial Velocity, Stellar Mass Accretion

Scientific paper

Time-resolved spectroscopy of V1500 Cyg are presented from 1981, when the nebular lines from the nova ejecta had faded sufficiently to permit reliably radial velocity measurements on emission lines from the binary remnant. The spectra possess a typical AM Herculis signature. The wavelength region 3800-5100 A contains a number of strong lines, in particular the Balmer series and He II 4686 A. All lines show periodic velocity changes with the same period as the photometric variations. On the first night the lines are relatively weak and narrow, are in phase with the photometric cycle, and suffer extreme modulation; two months later they are strong and broad, are roughly 90 deg out of phase with the photometric cycle, and have relatively less variation in their line fluxes. These features support the suggestion that the remnant is an AM Her system. The observed radial velocity of the secondary is 193 + or - 9 km/s. Various constraints suggest that the magnetic white dwarf in this system has a mass over 0.9 solar.

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