On the Mass Ratio of IP Peg

Details On the Mass Ratio of IP Peg On the Mass Ratio of IP Peg

Jun 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aca....52..189s&link_type=abstract

Acta Astronomica, v.52, pp.189-193, (2002).

Astronomy and Astrophysics

Astronomy

6

Binaries: Eclipsing, Novae, Cataclysmic Variables, Stars: Individual: Ip Peg

Scientific paper

Radial velocities measured from peaks of the emission lines of IP Peg (Hessman 1989) are analyzed within the three-body approximation, giving mu =M_2/(M_1+M_2)=0.31+/-0.02, or q=M_2/M_1=0.45+/p0.04. Combined with K_2=298+/-8 km/s (Martin etal 1989), this implies the true value of K_1^*=134+/-15 km/s. The large value of K_1=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 K_1=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 K_1^*. System parameters are: i=81.8 arcd+/-0.9 arcd, M_1=0.94+/-0.10 MS, M_2=0.42+/-0.08 MS, and A=1.36+/-0.08 RS. The radius of the secondary component R_2=0.43+/-0.03 RS, when compared with its mass, shows that the secondary is a normal main sequence star.

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