Optical observations of the black hole candidate GX 339-4 (V821 Arae)

被引:47
作者
Cowley, AP [1 ]
Schmidtke, PC
Hutchings, JB
Crampton, D
机构
[1] Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA
[2] Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Astrophys Observ, Victoria, BC V9E 2E7, Canada
关键词
binaries : close; stars : individual (GX 339-4); X-rays;
D O I
10.1086/339028
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
GX 339-4 has long been known as a black hole candidate because of its rapid variability and high/low X-ray states, which are similar to those of Cyg X-1. Although GX 339-4 is assumed to be a binary, the orbital period has not yet been convincingly determined, and hence little is known about the nature of the component stars. In this study simultaneous photometric and spectroscopic observations have been made in an effort to address these problems. Although a definitive period has not been found, we present evidence that it lies near similar to0.7 days. The I-band light curve has an amplitude of only similar to0.2 mag, with flickering of >0.1 mag superposed, making it difficult to determine the orbital period from light variations alone. The emission-line velocity amplitudes are small, suggesting that GX 339-4 is seen at a low orbital inclination angle. Even though the period is still not determined, the relative phasing of the velocities and light minima are known, since the photometric and spectroscopic observing runs overlapped. Assuming the orbital period is near similar to0.7 days, we can set limits on the mass ratio and stellar masses. For reasonable assumptions about the inclination angle, the mass ratio appears to lie between q similar to 3 and 15, where q = M-X/M-donor. If the donor star mass is greater than similar to0.3 M-circle dot, the X-ray source is likely to be a black hole.
引用
收藏
页码:1741 / 1749
页数:9
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