Other
Scientific paper
Dec 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998phdt........23h&link_type=abstract
Thesis (PHD). INDIANA UNIVERSITY , Source DAI-B 59/09, p. 4873, Mar 1999, 129 pages.
Other
1
Accretion Disks
Scientific paper
Algols are close, usually eclipsing, semi-detached binary star systems. They typically consist of a spectral type A, or late B or F, primary star with normal main sequence characteristics, and an evolved secondary of lower mass, overflowing its 'Roche Surface' and losing mass to the primary. This overflowing mass can be accreted by the primary star by forming an accretion disk or ring around the star. Evidence of this process is the existence of red-shifted and blue-shifted emission lines, where the Doppler shifts are due to motion of the disk's rotation towards or away from the observer. These emission lines are most easily seen during eclipse, but in the systems discussed here (and others) they can also be studied out of eclipse. This thesis investigates the nature of the accretion disks of three short period Algol systems, SW Cyg, TZ Eri and SS Cet, by examining their Hα and Hβ spectral emission. The observations cover the complete orbit of each system in Hα, as well as Hα and Hβ observations of SW Cyg during 4 eclipses. For all the observational data, the circumstellar emission was isolated by subtracting the contribution of the stellar (photospheric) hydrogen lines. For the eclipse data, the emission was modeled with a simple code to determine various parameters of the disk structure. All three systems showed significant variability in absorption and emission features, often over periods as short as a few days. The absorption seems to be related to the interaction of the gas-stream from the secondary star and the accretion disk. This interaction may also lead to the supersonic turbulence seen during eclipse in SW Cyg.
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