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On the Mass Ratio of IP Peg

Smak J.

Acta Astronomica

2002

Vol. 52, No. 2

189--193

Radial velocities measured from peaks of the emission lines of IP Peg (Hessman 1989) are analyzed within the three-body approximation, giving μ=M2/(M1+M2)=0.31±0.02, or q=M2/M1=0.45±0.04. Combined with K2=298±8 km/s (Martin et al. 1989), this implies the true value of K1*=134±15 km/s. The large value of K1=175±15 km/s, determined by Marsh (1988) from wings of emission lines, is qualitatively interpreted as being due to contaminations by contributions from parts of the stream which are overflowing the disk close to the white dwarf. The value of K1=118±10 km/s, obtained by Hessman (1989) from observations made immediately after outburst, when stream overflow effects were limited or absent, agrees - within errors - with K1*. System parameters are: i=81°.8±0°.9, M1=0.94±0.10 Msolar, M2=0.42±0.08 Msolar, and A=1.36±0.08 Rsolar. The radius of the secondary component R2=0.43±0.03 Rsolar, when compared with its mass, shows that the secondary is a normal main sequence star.