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The Photometric Observations and the Light Curve Analysis of U Pegasi
The system of U Pegasi was observed photometrically in B and V filtersin 1998 at Birouni Observatory, University of Shiraz, Iran. Two Lightcurves were obtained and have been analyzed separately ofWilson-Devinney code. New geometrical and physical elements for thesystem are given. The absolute dimensions of the binary have beenderived by combining the photometric solution with spectroscopic data ofthe system. The light curves analysis indicate that U peg is anovercontact W UMa system with W type components which fill theircorresponding Roche lobe. The results obtained in this study indicatethat U Peg may be lied on main sequence with estimated masses of 0.565M_solar and 0.362 M_solar.
| A new photoelectric investigation of the W UMa system U Pegasi
Data from 217 pairs of BV photometric observations of U Peg, obtainedwith a single-channel photomultiplier photometer on the 60-cm reflectorat Beijing Observatory during 1978, are presented in tables and graphsand discussed in comparison with previous observations. Four minimatimes are determined; a secular period decrease of 4.16 msec/yr iscalculated from for the period 1896-1978; and a 17-yr oscillation withsemiamplitude 0.00323 d is identified and attributed to the light-timeeffect of a main-sequence type-M6 third body of 0.16 solar mass.Interpretation of the 1978 light curves and those obtained by Binnendijk(1960) in 1958 indicates an overcontact of about 9 percent, aphotometric mass ratio m2/m1 between 2.5 and 3, a gamma velocity of -40km/sec, and dimensions 0.6 solar mass and 0.8 solar radius for the firstcomponent and 1.3 solar mass and 1.4 solar radius for the secondcomponent.
| A new analysis of the eclipsing binary, U Pegasi.
Abstract image available at:http://adsabs.harvard.edu/abs/1972AJ.....77..319R
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