Analysis of light variations of the eclipsing binary system XY Ceti with AM spectra

Details Analysis of light variations of the eclipsing binary system XY Ceti with AM spectra Analysis of light variations of the eclipsing binary system XY Ceti with AM spectra

Jul 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978ap%26ss..56..293o&link_type=abstract

Astrophysics and Space Science, vol. 56, no. 2, July 1978, p. 293-302.

Astronomy and Astrophysics

Astrophysics

5

A Stars, Eclipsing Binary Stars, Light Curve, Stellar Spectra, Ubv Spectra, Light Emission, Periodic Variations, Stellar Motions, Stellar Spectrophotometry

Scientific paper

The photoelectric light curves of XY Cet of Srivastava and Padalia (1975) and of Morrison and Morrison (1968), from which considerably different sets of photometric elements have pre- viously been deduced, were re-analyzed in detail. The elements derived in the present study from Srivastava and Padalia's (1975) UBV observations are rg = 0.157 ± 0.006 (p.e.), r~ = 0.142 ± 0.007, 1 = 88~4 ± 0?5, Lg = 0.600 ± 0.017, 0.602 ± 0.015 and 0.584 ± 0.018 for U, B and V. respectively. It is also found from their light curves that the system has an eccentric orbit with e cos w = 0.0026 ± 0.0005. The elements deduced from the V observations of Morrison and Morrison (1968) are found to be in satisfactory agreement with those presented above. The existence of the Am characteristics of both components, which was recognized by earlier spectroscopic observations, are supported by the B-V and U-B color indices and L1[mi] value of the system. Both components are also found to have appreciably evolved, as expected for metallic- line stars

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