论文标题
Black Hole GRO J1655-40中的积聚磁盘风的快速光谱
Swift Spectroscopy of the Accretion Disk Wind in the Black Hole GRO J1655-40
论文作者
论文摘要
Chandra在2005年爆发期间获得了恒星质量黑洞GRO J1655-40的两个高能传输光栅（HETG）光谱，显示出丰富而复杂的磁盘风。发射后不久，尼尔·盖尔斯·斯威夫特天文台开始监视同一爆发。以某种模式获得了一些X射线望远镜（XRT）观测值，该模式无法删除强大的MN校准线，因此先前忽略了光谱中的Fe K-Alpha线区域。但是，这些线可以对能量量表进行精确的校准，从而促进对吸收为主的磁盘风及其速度变化的研究。在这里，我们将拟合到15个Swift/XRT光谱，从而揭示了流出中的可变性和演变。 The data strongly point to a magnetically driven disk wind: both the higher velocity (e.g., v ~ 10^4 km/s) and lower velocity (e.g., v ~ 10^3 km/s) wind components are typically much faster than is possible for thermally driven outflows (v < 200 km/s), and photoionization modeling yields absorption radii that are two orders of magnitude below the Compton radius这定义了热风的典型内部范围。此外，关键风参数之间的相关性产生的平均吸收度量分布（AMD）与磁流失动力风模型一致。我们讨论了我们的结果，该结果是关于黑洞积聚磁盘和流出以及未来前景的最新观察和理论研究。
Chandra obtained two High Energy Transmission Grating (HETG) spectra of the stellar-mass black hole GRO J1655-40 during its 2005 outburst, revealing a rich and complex disk wind. Soon after its launch, the Neil Gehrels Swift Observatory began monitoring the same outburst. Some X-ray Telescope (XRT) observations were obtained in a mode that makes it impossible to remove strong Mn calibration lines, so the Fe K-alpha line region in the spectra was previously neglected. However, these lines enable a precise calibration of the energy scale, facilitating studies of the absorption-dominated disk wind and its velocity shifts. Here, we present fits to 15 Swift/XRT spectra, revealing variability and evolution in the outflow. The data strongly point to a magnetically driven disk wind: both the higher velocity (e.g., v ~ 10^4 km/s) and lower velocity (e.g., v ~ 10^3 km/s) wind components are typically much faster than is possible for thermally driven outflows (v < 200 km/s), and photoionization modeling yields absorption radii that are two orders of magnitude below the Compton radius that defines the typical inner extent of thermal winds. Moreover, correlations between key wind parameters yield an average absorption measure distribution (AMD) that is consistent with magnetohydrodynamic wind models. We discuss our results in terms of recent observational and theoretical studies of black hole accretion disks and outflows, and future prospects.
