An emission-line model for AM Herculis systems

Journal Article · Thu Jun 01 04:00:00 EDT 1989 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/167497· OSTI ID:5598207

Ferrario, L; Tuohy, I R; Wickramasinghe, D T ^[1]

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1. Mount Stromlo and Siding Spring Observatories, Canberra (Australia)

The optical spectra of the AM Herculis binaries are characterized by extremely complex emission lines whose profiles can be resolved into at least three components which are formed in different regions of the accretion stream leading from the companion star toward the magnetic white dwarf. A theoretical model is presented for the radial velocity and velocity dispersion of the broad emission line component assuming that it originates mainly in the gas which is diverted out of the orbital plane and funneled onto the white dwarf surface along magnetic field lines. The model is used to locate the line-forming region in three AM Her variables: E1405-451, CW 1103+254, and EXO 033319-2554.2, using as constraints the radial velocity and velocity dispersion data. The analyses of these systems show that the material is threaded by the magnetic field in a very azimuthally extended coupling region located 0.5-0.75 of the way between the white dwarf and the inner Lagrange point. 36 refs.

• OSTI ID: 5598207
• Journal Information: Astrophysical Journal; (USA), Journal Name: Astrophysical Journal; (USA) Vol. 341; 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
ATMOSPHERES
BINARY STARS
CONSTRAINTS
DWARF STARS
EMISSION SPECTRA
ERUPTIVE VARIABLE STARS
LINE WIDTHS
MAGNETIC STARS
MATHEMATICAL MODELS
NOVAE
RADIAL VELOCITY
SPECTRA
STAR ACCRETION
STAR EVOLUTION
STAR MODELS
STARS
STELLAR ATMOSPHERES
STELLAR MAGNETOSPHERES
VARIABLE STARS
VELOCITY
VISIBLE SPECTRA
WHITE DWARF STARS