The Mass Ratio and the Disk Image of the X-Ray Nova GS 2000+25

Details The Mass Ratio and the Disk Image of the X-Ray Nova GS 2000+25 The Mass Ratio and the Disk Image of the X-Ray Nova GS 2000+25

Sep 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996pasp..108..762h&link_type=abstract

Publications of the Astronomical Society of the Pacific, v.108, p.762

Astronomy and Astrophysics

Astronomy

64

X-Rays: Bursts, Ism: Individual: Gs 2000+25

Scientific paper

Keck observations of the black hole candidate GS 2000+25 in quiescence have recently been used by Filippenko, Matheson, and Barth to determine a mass function f(M_x) = 4.97 +/- 0.10 solar mass for the compact object. Our reanalysis of the data confirms this result (5.01 +/- 0.12 solar mass). We estimate a mass ratio of q = M_c/M_x = 0.042 +/- 0.012 from the rotational broadening of the companion star, v sin i = 86 +/- 8 km s^-1. From q and the companion star's radial velocity K_c, we derive the mass of the compact object M_x = (5.44 +/- 0.15) sin^-3 i solar mass and the mass of the companion star M_c = (0.23 +/- 0.02) sin^-3 i solar mass. Constraints on the inclination (75 degrees > i > 47 degrees) lead to 6.04 < M_x < 13.9 and 0.26 < M_c < 0.59 (1-sigma) in solar mass units. We determine a spectral type of K3-K6 for the companion star, which contributes more than 72% of the light at red wavelengths (94% +/- 5% for K5 V). Our analysis shows that the companion is an undermassive star, slightly evolved but not a subgiant. Consistent with the work of Filippenko et al. we detect Li I lambda-6708 absorption (equivalent width 150 +/- 85 mA) in the spectrum of the companion. A Doppler image of the system shows evidence for a bright spot which contributes 10% of the emission-line flux density, and arises in the range 0.3-0.6 R_L1 of the accretion disk, where L1 is the inner Lagrangian point. Along the trajectory of the gas stream, the velocities are initially ballistic and gradually become Keplerian. (SECTION: Stars)

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