A photometric study of the very short period eclipsing binary EH Hydrae

Details A photometric study of the very short period eclipsing binary EH Hydrae A photometric study of the very short period eclipsing binary EH Hydrae

Aug 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991aj....102..688s&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 102, Aug. 1991, p. 688-698. Research supported by American Astronomical Society and

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7

Eclipsing Binary Stars, Late Stars, Light Curve, Stellar Magnitude, Stellar Spectrophotometry, Stellar Mass, Stellar Temperature

Scientific paper

Recent Johnson-Cousins' B,V,Rc,Ic photoelectric observations of the very short period W UMa variable, EH Hya, are presented. These observations were made, using the Yale 1M telescope and the dry-ice-cooled Hamamatsu Ga-As PMT at Cerro Tololo Inter-Americal Observatory. The light curves reveal that the eclipses are total, and that the primary eclipse is an occultation. Thus, the system is of W-type, with the larger component being the cooler. Standard magnitudes were determined, and a reddening estimate was made. A simultaneous solution of the B,V,R light curves was computed using the Wilson-Devinney (1971) synthetic light curve code. The solution indicates that the system consists of two late G-type stars in shallow contact with a fill-out factor of 12 percent. The difference in component temperatures is 336(8) K and the mass ratio is rather extreme, being 0.314(2). EH Hya is compared to other very short period binaries of late G-type, and they are found to comprise a fairly homogenous group with regards to mass ratios, degree of thermal contact, and magnetic activity.

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