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首页> 外文期刊>The Astrophysical journal >SIMULTANEOUS CHANDRA AND RXTE SPECTROSCOPY OF THE MICROQUASAR H1743-322: CLUES TO DISK WIND AND JET FORMATION FROM A VARIABLE IONIZED OUTFLOW
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SIMULTANEOUS CHANDRA AND RXTE SPECTROSCOPY OF THE MICROQUASAR H1743-322: CLUES TO DISK WIND AND JET FORMATION FROM A VARIABLE IONIZED OUTFLOW

机译：微型潮汐H1743-322的同时Chandra和RXTE光谱：可变电离流对盘风和射流形成的影响

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摘要

We observed the bright phase of the 2003 outburst of the Galactic black hole candidate H1743-322 in X-rays simultaneously with Chandra and RXTE on four occasions. The Chandra HETGS spectra reveal narrow, variable (He-like) Fe xxv and (H-like) Fe XXVI resonance absorption lines. In the first observation, the Fe XXVI line has a FWHM of 1800 ± 400 km s~(-1) and a blueshift of 700 ± 200 km s~(-1), suggesting that the highly ionized medium is an outflow. Moreover, the Fe xxv line is observed to vary significantly on a timescale of a few hundred seconds in the first observation, which corresponds to the Keplerian orbital period at approximately 10~4r_g (where r_g = GM/c~2). Our models for the absorption geometry suggest that a combination of changing ionizing flux and geometric effects are required to account for the large changes in line flux observed between observations and that the absorption likely occurs at a radius between 10~2r_g and 10~4r_g for a 10 solar mass black hole. We suggest that the absorption occurs in an inhomogeneous accretion disk wind. If the wind in H1743-322 has unity filling factor, the highest implied mass outflow rate is 5% of the Eddington mass accretion rate. The observed wind may be a hotter, more ionized version of the Seyfert-like, outflowing warm absorber geometries recently found in the Galactic black holes GX 339-4 and XTE J1650-500. We discuss these findings in the context of ionized Fe absorption lines found in the spectra of other Galactic sources, and connections to warm absorbers, winds and jets in other accreting systems.
机译：我们在4次观测中与钱德拉和RXTE同时在X射线观察了2003年银河黑洞候选H1743-322爆发的亮相。 Chandra HETGS光谱显示出狭窄的，可变的（He类）Fe xxv和（H类）Fe XXVI共振吸收线。在第一个观察中，Fe XXVI线的FWHM为1800±400 km s〜（-1），蓝移为700±200 km s〜（-1），表明高电离介质是流出。此外，在第一次观测中观察到Fe xxv线在几百秒的时间尺度上有显着变化，这对应于约10〜4r_g（其中r_g = GM / c〜2）的开普勒轨道周期。我们的吸收几何模型表明，需要结合变化的电离通量和几何效应来解决两次观测之间观测到的线通量的大变化，并且吸收可能发生在半径介于10〜2r_g和10〜4r_g之间的区域。 10太阳质量黑洞。我们建议吸收发生在不均匀的吸积盘风中。如果H1743-322中的风具有统一的填充因子，则最高的隐含质量流出率是Eddington质量增加率的5％。观测到的风可能是最近在银河系黑洞GX 339-4和XTE J1650-500中发现的塞弗特样流出的热吸收体几何形状的更热，更电离的形式。我们将在其他银河源光谱中发现的离子化铁吸收线以及与其他吸积系统中的热吸收剂，风和射流的连接中讨论这些发现。

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