天鹅座X-1在X射线软/高态期间X射线光电离风的紫外观测
Ultraviolet observations of the X-ray photoionized wind of Cygnus X-1 during X-ray soft/high state
摘要：
利用HSTubble上的STIS对黑洞X射线双星天鹅座X-1进行了紫外观测。我们检测到天鹅座P线的功能表现出强大的，广泛的吸收成分时，X射线源是后面的伴星和明显较弱的吸收时，X射线源是我们和伴星之间。我们拟合的P天鹅座配置文件使用SEI方法适用于球对称恒星风受到X射线光电离的黑洞。Si IV偶极子提供了风和X射线照明参数的最可靠估计。根据$v=v_\infty(1-r_\star/r)^β$，速度$v$随半径$r$增加，$β\approx0.75$和$v_\infty\approx1420$ km s $^{-1}$。微湍流速度为$\approx160$ km s $^{-1}$。我们的拟合意味着X射线光度与风质量损失率的比值为L $_{X,38}/\dot M_{-6} \approx 0.33$，在$\dot M_{-6}$ = 4.8处测量。我们的模型确定的参数，可用于估计吸积率到黑洞和独立预测的X射线光度。我们预测的L $_x$与同期RXTE ASM确定的结果非常匹配，但比Bondi-Hoyle-Littleton球形风吸积的速率低3倍。我们认为，吸积的一部分能量可能用于驱动喷流。
英文摘要：
(Shortened) Ultraviolet observations of the black hole X-ray binary Cygnus X-1 were obtained using the STIS on HSTubble. We detect P Cygni line features show strong, broad absorption components when the X-ray source is behind the companion star and noticeably weaker absorption when the X-ray source is between us and the companion star. We fit the P Cygni profiles using the SEI method applied to a spherically symmetric stellar wind subject to X-ray photoionization from the black hole. The Si IV doublet provides the most reliable estimates of the parameters of the wind and X-ray illumination. The velocity $v$ increases with radius $r$ according to $v=v_\infty(1-r_\star/r)^β$, with$β\approx0.75$ and $v_\infty\approx1420$ km s$^{-1}$.The microturbulent velocity was $\approx160$ km s$^{-1}$. Our fit implies a ratio of X-ray luminosity to wind mass-loss rate of L$_{X,38}/\dot M_{-6} \approx 0.33$, measured at $\dot M_{-6}$ = 4.8. Our models determine parameters that may be used to estimate the accretion rate onto the black hole and independently predict the X-ray luminosity. Our predicted L$_x$ matches that determined by contemporaneous RXTE ASM remarkably well, but is a factor of 3 lower than the rate according to Bondi-Hoyle-Littleton spherical wind accretion. We suggest that some of the energy of accretion may go into powering a jet.
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