BLACK HOLES IN GENERAL RELATIVITY
BLACK HOLES IN GENERAL RELATIVITY
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DOI：
10.1007/bf01877517
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发表时间：
1972-01-01
影响因子：
2.4
通讯作者：
HAWKING, SW
中科院分区：
文献类型：
--
作者：
HAWKING, SW
假设引力坍缩中的奇点从外部是不可见的，而是隐藏在事件视界后面。这意味着人们仍然可以预测事件视界之外的未来。类空表面上的黑洞被定义为以事件视界为界的表面区域的连通分量。随着时间的增加，黑洞可能会合并在一起，但永远不会分叉。黑洞会稳定在一个静止的状态。证明了一个静止黑洞必须具有拓扑球边界，如果它是旋转的，则它必须是轴对称的。这些结果与伊斯雷尔和卡特的结果一起，大部分都是为了建立一个猜想，即任何静止黑洞都是克尔解。利用这个猜想和黑洞的表面积永远不会减少的结果，人们可以对从黑洞中提取的能量设置一定的限制。
It is assumed that the singularities which occur in gravitational collapse are not visible from outside but are hidden behind an event horizon. This means that one can still predict the future outside the event horizon. A black hole on a spacelike surface is defined to be a connected component of the region of the surface bounded by the event horizon. As time increase, black holes may merge together but can never bifurcate. A black hole would be expected to settle down to a stationary state. It is shown that a stationary black hole must have topologically spherical boundary and must be axisymmetric if it is rotating. These results together with those of Israel and Carter go most of the way towards establishing the conjecture that any stationary black hole is a Kerr solution. Using this conjecture and the result that the surface area of black holes can never decrease, one can place certain limits on the amount of energy that can be extracted from black holes.