Two very similar late-type contact systems - BX and BB Pegasi

Details Two very similar late-type contact systems - BX and BB Pegasi Two very similar late-type contact systems - BX and BB Pegasi

Mar 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985aj.....90..515l&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 90, March 1985, p. 515-521. Research supported by the Chinese Academy of Sciences.

Astronomy and Astrophysics

Astronomy

11

Astronomical Photometry, Eclipsing Binary Stars, Electrophotometry, Late Stars, Light Curve, Mass Ratios

Scientific paper

V and B observations of BX and BB Pegasi secured at Beijing Observatory were analyzed with the Wilson and Devinney method. An extensive search for reliable photometric mass ratios was performed. Both systems were found to be in contact with small degrees of overcontact, 10 percent and 12 percent, for BX and BB Peg, respectively. Their mass ratios were, respectively, 2.80 and 2.81. The eclipse at primary minimum was found to be total for both systems. They have the characteristics of W-type W UMa systems. The computed light curves fit the observations very well for BX Peg. The light curves of BB Peg are very complex: there is large asymmetry in the maxima, and significant discrepancy in the differential eclipse depths (Min I and Min II) between the V and B curves. As a result of these complications, the computed light curves do not fit the observations well. Adopted photometric parameters for BX Peg are similar to those obtained by Kaluzny, who used the Rucinski method. It is believed that adopted photometric parameters for BB Peg are more reliable than those obtained by Cerruti-Sola et al.

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