Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999apj...525..915w&link_type=abstract
The Astrophysical Journal, Volume 525, Issue 2, pp. 915-920.
Astronomy and Astrophysics
Astronomy
3
Accretion, Accretion Disks, Stars: Binaries: Close, Stars: Novae, Cataclysmic Variables, Stars: Atmospheres, Ultraviolet: Stars
Scientific paper
We have modified a spectrum synthesis code for accretion disks in binary star systems, to deal with the case of a disk that is partially eclipsed by the mass-losing star. The known Roche geometry of the binary system permits the correspondence to be made between the spectrum observed over some phase interval and the regions of the disk that contribute to the spectrum. The code can generate simulated observations corresponding to arbitrary phase intervals, with arbitrary spectral sampling and resolution. This capability clearly includes generating broadband light curves as a limiting case. The use of angle-dependent specific intensities means that limb-darkening effects are automatically taken into account. We present trailed-spectrogram and other representations of the partially eclipsed disk spectra of representative models of cataclysmic variables. The spectra are shown versus orbital phase, for portions of the ultraviolet spectral region accessible to the Hubble Space Telescope. We illustrate the behavior of blended features through eclipse and comment on the sensitivity of the synthesized spectra to the parameters of the input model, such as the stellar masses, mass transfer rate, and orbital inclination. Compared with out-of-eclipse spectra of the entire disk, observations during eclipse should have the advantage for diagnostic purposes of showing (1) deeper individual lines, (2) reduced blending of lines, and (3) an effectively smaller range of effective temperatures contributing to the observed spectrum. These advantages are especially important in analysis of the ultraviolet spectra of disks.
Orosz Jerome A.
Wade Richard A.
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