Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...341..327f&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 341, June 1, 1989, p. 327-339.
Astronomy and Astrophysics
Astrophysics
45
Binary Stars, Cataclysmic Variables, Emission Spectra, Stellar Mass Accretion, White Dwarf Stars, Dwarf Novae, Polarized Radiation, Spectral Line Width, Stellar Magnetospheres, Visible Spectrum
Scientific paper
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.
Ferrario Lilia
Tuohy Ian R.
Wickramasinghe Dayal T.
No associations
LandOfFree
An emission-line model for AM Herculis systems does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with An emission-line model for AM Herculis systems, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and An emission-line model for AM Herculis systems will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1850060