ON THE PROPERTIES OF THERMAL DISK WINDS IN X-RAY TRANSIENT SOURCES: A CASE STUDY OF GRO J1655−40
ON THE PROPERTIES OF THERMAL DISK WINDS IN X-RAY TRANSIENT SOURCES: A CASE STUDY OF GRO J1655−40
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DOI：
10.1088/0004-637x/719/1/515
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发表时间：
2010-03
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通讯作者：
S. Luketic;D. Proga;T. Kallman;J. Raymond;J. M. M. U. O. Nevada-J.-M.-M.-U.-O.-Nevada-119298541;L. Vegas;NasaGsfc;Harvard-Smithsonian Cfa;U. Michigan
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作者：
S. Luketic;D. Proga;T. Kallman;J. Raymond;J. M. M. U. O. Nevada-J.-M.-M.-U.-O.-Nevada-119298541;L. Vegas;NasaGsfc;Harvard-Smithsonian Cfa;U. Michigan
我们提出的流体动力学模拟的结果，在吸积黑洞的磁盘的最里面的部分产生的强X射线照射的磁盘光球。正如预期的那样，辐射加热了光球层并驱动了热风。为了将我们的结果应用于研究得很好的X射线瞬态源GRO J1655−40，我们采用了观测到的黑洞质量和观测到的X射线辐射特性。为了与观测结果进行比较，我们还计算了基于风解的透射X射线谱。我们的主要发现是，风的快速移动部分的密度比从观测中推断的密度低1个数量级以上。因此，该模型无法预测光谱与线吸收一样强，蓝移的观察。然而，尽管热成风很弱，康普顿很薄，但质量损失率和质量吸积率之间的比值约为7。在较低的光度极限下，这个高的比值对吸积光度不敏感。大部分的质量在康普顿半径的0.07到0.2之间从盘中丢失。我们发现，超过这个范围，风的解决方案是自相似的。特别是，在它离开圆盘后不久，风以相对于圆盘的恒定角度流动。总的来说，在我们的综合模拟中产生的热成风与GRO J1655−40中观察到的风谱不匹配。这支持了米勒等人和卡尔曼等人的结论，即GRO J1655−40中的风，以及其他可能的X射线瞬变，可能是由磁过程驱动的。这反过来又意味着盘风携带的物质比我们的模拟预测的更多，因此对吸积盘结构和动力学有非常重要的影响。
We present the results of hydrodynamical simulations of the disk photosphere irradiated by strong X-rays produced in the innermost part of the disk of an accreting black hole. As expected, the irradiation heats the photosphere and drives a thermal wind. To apply our results to the well-studied X-ray transient source GRO J1655−40, we adopted the observed mass of its black hole and the observed properties of its X-ray radiation. To compare the results with the observations, we also computed transmitted X-ray spectra based on the wind solution. Our main finding is that the density of the fast-moving part of the wind is more than 1 order of magnitude lower than that inferred from the observations. Consequently, the model fails to predict spectra with line absorption as strong and as blueshifted as those observed. However, despite the thermal wind being weak and Compton thin, the ratio between the mass-loss rate and the mass-accretion rate is about seven. This high ratio is insensitive to the accretion luminosity, in the limit of lower luminosities. Most of the mass is lost from the disk between 0.07 and 0.2 of the Compton radius. We discovered that beyond this range the wind solution is self-similar. In particular, soon after it leaves the disk, the wind flows at a constant angle with respect to the disk. Overall, the thermal winds generated in our comprehensive simulations do not match the wind spectra observed in GRO J1655−40. This supports the conclusion of Miller et al. and Kallman et al. that the wind in GRO J1655−40, and possibly in other X-ray transients, may be driven by magnetic processes. This in turn implies that the disk wind carries even more material than our simulations predict and as such has a very significant impact on the accretion disk structure and dynamics.