The photometric solution of CC COM by use of the Wilson and Devinney card

Details The photometric solution of CC COM by use of the Wilson and Devinney card The photometric solution of CC COM by use of the Wilson and Devinney card

Feb 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988ap%26ss.141..199z&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 141, no. 2, Feb. 1988, p. 199-206. Research supported by the National Natu

Astronomy and Astrophysics

Astrophysics

3

Eclipsing Binary Stars, Late Stars, Light Curve, Stellar Spectrophotometry, Limb Darkening, Mass Ratios

Scientific paper

The data of Rucinski et al. (1977) on the photometric observations of CC Comae system (conducted in February 1975 with a 91-cm telescope at the Kitt Peak National Observatory) and the synthetic light curve technique of Wilson and Devinney (1971, 1973) were used to calculate the photometric orbit of the system. The results indicate that the CC Com belongs to the late-type eclipsing binary system with the spectral type of components K5V and K6V. The component masses M1 and M2 equal to 0.62 and 0.36 solar mass, respectively; and the radii R1 and R2 equal to 0.70 and 0.52 solar radii. The mass ratio of the CC Com is 0.58732 + or - 0.0021, and the orbital inclination equals to 87.714 + or - 1.44 deg. The temperatures of the two components are T1 = 4300 K and T2 = 4265 K. These parameters indicate that the system cannot be explained by Lucy's (1968) theoretical model for late W-type systems, since the two CC Com components have low mass, temperature, and size, and hence are more similar to each other than the model specifies.

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