Period changes in W UMa-type eclipsing binaries: DK Cygni, V401 Cygni, AD Phoenicis and Y Sextantis

Details Period changes in W UMa-type eclipsing binaries: DK Cygni, V401 Cygni, AD Phoenicis and Y Sextantis Period changes in W UMa-type eclipsing binaries: DK Cygni, V401 Cygni, AD Phoenicis and Y Sextantis

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26as..147..243w&link_type=abstract

Astronomy and Astrophysics Supplement, v.147, p.243-249

Astronomy and Astrophysics

Astrophysics

14

Stars: Binaries: Eclipsing, Stars: Individual: Dk Cyg, Stars: Individual: V401 Cyg, Stars: Individual: Ad Phe, Stars: Individual: Y Sex, Stars: Fundamental Parameters

Scientific paper

We present a period analysis of the four well-known W UMa-type eclipsing binaries DK Cyg (P = 0fd47 ), V401 Cyg (0fd58 ), AD Phe (0fd38 ) and Y Sex (0fd42 ). Several new times of minimum light, recorded photoelectrically, have been gathered. Analysis of all available eclipse timings of the DK Cygni and V401 Cygni has confirmed a significant increase in period of 1.15 10-10 and 1.48 10-10 day cycle-1, respectively. A simultaneous solution of the B, V and R light curves was computed for V401 Cyg using the Binary Maker 2.0 synthetic lightcurve software. This solution indicates that V401 Cyg is in contact with a filing factor of 46%. The period of AD Phe seems to be constant. Period changes of Y Sex could be explain by a light-time effect caused by a third body in an eccentric orbit with a period of 58 years. Some of the observations reported in this paper were obtained at the South Africa Astronomical Observatory, Sutherland, South Africa.

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