A new photometric study of the binary U Pegasi

Details A new photometric study of the binary U Pegasi A new photometric study of the binary U Pegasi

Jun 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984acasn..25..336z&link_type=abstract

(Acta Astronomica Sinica, vol. 25, 1984, p. 336-347) Chinese Astronomy and Astrophysics (ISSN 0275-1062), vol. 9, June 1985, p.

Astronomy and Astrophysics

Astrophysics

Astronomical Photometry, Binary Stars, Electrophotometry, Light Curve, Main Sequence Stars, Mass Ratios, Radial Velocity, Tables (Data)

Scientific paper

Over four hundred photoelectric observations of the binary star U Pegasi (U Peg) have been obtained using the 0.6-meter reflector telescope at Beijing Observatory. The observations were used to calculate the periods of minimum light of U Peg from 1896 to 1980. A secular period decrease of -1.32 x 10 to the -10th (-4.16 x 10 to the -3rd sec/yr) was found, as well as a short term (17 yr) sinusoidal oscillation with a semiamplitude of 0.00323 days. It is suggested that the oscillating term was due to the light-time effects of an unseen third body, possibly a M 6 main sequence star with a mass of 0.16 solar mass. Analysis of light curves for the year 1978, together with the light curves of Binnendijk (1958) showed that U Peg has an overcontact configuration of about 9 percent. The absolute dimensions of the components of U Peg were calculated based on the photometric results. The estimated masses were 0.6 and 1.8 solar mass for components one and two, respectively. The physical dimensions of the components indicate that they are main sequence stars.

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