On the Mass Ratio of IP Peg

• Autorzy: Smak J.
• Języki publikacji: EN

Abstrakty

EN

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 M_solar, M₂=0.42±0.08 M_solar, and A=1.36±0.08 R_solar. The radius of the secondary component R₂=0.43±0.03 R_solar, when compared with its mass, shows that the secondary is a normal main sequence star.

Słowa kluczowe

EN

binaries: eclipsing; novae; cataclysmic variables; stars: individual: IP Peg

• Wydawca: Copernicus Foundation for Polish Astronomy
• Czasopismo: Acta Astronomica
• Rocznik: 2002
• Tom: Vol. 52, No. 2
• Strony: 189--193
• Opis fizyczny: Bibliogr. 13 poz., tab., wykr.

Twórcy

autor

Smak J.

• N. Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, 00-716 Warsaw, Poland

Bibliografia

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