ESTIMATING THE PROMPT ELECTROMAGNETIC LUMINOSITY OF A BLACK HOLE MERGER
ESTIMATING THE PROMPT ELECTROMAGNETIC LUMINOSITY OF A BLACK HOLE MERGER
复制标题
估计黑洞合并的瞬发电磁光度
DOI：
10.1088/0004-637x/709/2/774
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发表时间：
2009
期刊：
影响因子：
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通讯作者：
J. Krolik
中科院分区：
文献类型：
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作者：
J. Krolik
虽然最近的数值相对论工作在量化黑洞合并的引力波光度方面取得了巨大的进步，但对可能与这些事件直接相关的电磁光度却知之甚少。我们表明，每当一对合并黑洞附近的气体中沉积的热量与其总质量成正比，并且紧邻的气体的表面密度大于使其光学厚度所需的（相当小的）量时，与合并直接相关的发光度的特征尺度是与气体质量无关的爱丁顿发光度。光子信号的持续时间与气体质量成正比，并且通常比合并事件更长。在更大的距离上，与气体轨道重新调整到黑洞新的自旋方向相关的耗散可以补充轨道调整所获得的能量耗散到引力辐射中损失的质量;这两个热源可以联合收割机在更长的时间尺度上增加电磁辐射。
Although recent work in numerical relativity has made tremendous strides in quantifying the gravitational wave luminosity of black hole mergers, very little is known about the electromagnetic luminosity that might occur in immediate conjunction with these events. We show that whenever the heat deposited in the gas near a pair of merging black holes is proportional to its total mass, and the surface density of the gas in the immediate vicinity is greater than the (quite small) amount necessary to make it optically thick, the characteristic scale of the luminosity emitted in direct association with the merger is the Eddington luminosity independent of the gas mass. The duration of the photon signal is proportional to the gas mass, and is generally rather longer than the merger event. At somewhat larger distances, dissipation associated with realigning the gas orbits to the new spin orientation of the black hole can supplement dissipation of the energy gained from orbital adjustment to the mass lost in gravitational radiation; these two heat sources can combine to augment the electromagnetic radiation over longer timescales.