Computer Science
Scientific paper
Dec 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004phdt........29s&link_type=abstract
Ph.D dissertation, 2004. 384 pages; United States -- Arkansas: University of Arkansas; 2004. Publication Number: AAT 3149268. D
Computer Science
Binary Stars, Eclipsing, Rt Coronae Borealis
Scientific paper
This thesis examines the significance of binary stars and their evolutionary status, with particular emphasis on RT Coronae Borealis, a member of the RS Canis Venticorum type. The dissertation is primarily broken down into two parts: a general description of binary stars and a detailed examination of the RS CVn phenomenon.
We present an analysis of existing photometric observations in U, B, and V, and a new light curve in V, as well as spectroscopic observations of the 5.1 day- period, double-lined main-sequence eclipsing binary RT CrB. From the analysis of the light curves and radial velocity curves, we have determined the masses and radii of the components: 1.343 +/- 0.010 [Special characters omitted.] and 2.615 +/- 0.04 [Special characters omitted.] for the primary (hotter) component, 1.359 +/- 0.009 [Special characters omitted.] and 2.946 +/- 0.05 [Special characters omitted.] for the secondary (cooler) component. The formal uncertainties in the masses are both less than 1%, and the formal uncertainties in the radii are both less than 2%. Based on the analyzed light curves as well as the combined absolute photometry of the system, we estimate effective temperatures of 5781 +/- 100 K for the primary component and 5134 +/- 100 K for the secondary component, corresponding to the spectral types of G5 and K0, respectively. Projected rotational velocities ( v sin i ) from the spectrograms are measured as 25 +/- 2 km s -1 for the primary component and 33 +/- 3 km s -1 for the secondary component, and are consistent with rotation that is synchronous with the orbital motion. Evolutionary tracks from the current models are in good agreement with the observations for a system of about age 3.5 x 10 9 yr with a slightly non-solar chemical composition. We also report an approximate D P/P = 3.0 x 10 -6 decrease in the orbital period over 37-years.
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