Rotating winds from accretion disks in cataclysmic variables: Eclipse modeling of V347 Puppis

Journal Article · Mon Apr 01 04:00:00 EST 1996 · Astrophysical Journal

DOI:https://doi.org/10.1086/177066· OSTI ID:284643

Shlosman, I ^[1]; Vitello, P ^[2]; Mauche, C W ^[3]

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1. Department of Physics and Astronomy, University of Kentucky, Lexington, Kentucky 40506-0055 (United States)
2. Lawrence Livermore National Laboratory, L-14, P.O. Box 808, Livermore, California 94550 (United States)
3. Lawrence Livermore National Laboratory, L-41, P.O. Box 808, Livermore, California 94550 (United States)

We study the eclipsing nova-like variable V347 Pup by matching its UV emission-line profiles in and out of eclipse to synthetic lines using a three dimensional kinematic and radiation transfer model. Our results support the accretion disk origin of winds in nonmagnetic cataclysmic variables as opposed to the white dwarf origin. Our main point concerns the importance of rotation for the UV emission-line shapes in such systems. In particular, we show that the narrowing of the UV emission lines in V347 Pup during eclipse can be easily explained by the eclipse of the innermost part of the wind by the secondary and the resulting reduction in the contribution of rotational broadening to the width of the lines. During the eclipse, the residual line flux is very sensitive to the maximum temperature of disk radiation. Good fits for reasonable mass-loss rates have been obtained for maximum disk temperatures {approx_equal}50,000 K. This constraint was imposed either by leveling off the inner disk temperature profiles, in agreement with recent observations of some nova-like objects, or by assuming that the accretion disk does not extend to the surface of the white dwarf, in which case V347 Pup would be an intermediate polar. In anticipation of high-speed spectrophotometry of cataclysmic variables by the {ital Hubble} {ital Space} {ital Telescope}, we provide a numerical model of a time-resolved eclipse of V347 Pup or similar such system to be verified by future observations. {copyright} {ital 1996 The American Astronomical Society.}

• Research Organization: Lawrence Livermore National Laboratory
• DOE Contract Number: W-7405-ENG-48
• OSTI ID: 284643
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 461; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

66 PHYSICS
ACCRETION DISKS
BINARY STARS
ECLIPSE
ECLIPSING BINARY STARS
ERUPTIVE VARIABLE STARS
KINEMATICS
LINE BROADENING
LINE FORMATION
LINE WIDTHS
MASS LOSS
NOVAE
NUMERICAL SOLUTION
RADIANT HEAT TRANSFER
ROTATION
SPECTROPHOTOMETRY
STAR ACCRETION
STELLAR WINDS
THREE-DIMENSIONAL CALCULATIONS
ULTRAVIOLET SPECTRA
WHITE DWARF STARS