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

Journal Article · Tue Aug 01 04:00:00 EDT 1989 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/167758· OSTI ID:5348653

Horne, K; Schneider, D P ^[1]

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1. Space Telescope Science Institute, Baltimore, MD (USA)

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. 32 refs.

• OSTI ID: 5348653
• Journal Information: Astrophysical Journal; (USA), Journal Name: Astrophysical Journal; (USA) Vol. 343; ISSN ASJOA; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
BALMER LINES
BINARY STARS
CONSTRAINTS
DWARF STARS
EMISSION SPECTRA
ERUPTIVE VARIABLE STARS
IDENTIFICATION SYSTEMS
MAGNETIC STARS
MASS
NOVAE
RADIAL VELOCITY
SPECTRA
SPECTROSCOPY
STAR ACCRETION
STAR EVOLUTION
STARS
VARIABLE STARS
VARIATIONS
VELOCITY
WHITE DWARF STARS