Gravitational Collapse : The Role of General Relativity 1
Gravitational Collapse : The Role of General Relativity 1
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DOI：
10.1017/s007418090023605x
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发表时间：
2002
期刊：
影响因子：
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通讯作者：
R. Penrose
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文献类型：
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作者：
R. Penrose
质量与太阳（M）相同的恒星可以找到一个最终的平衡状态，要么成为一个白色矮星，要么（在坍缩和物质抛射之后）成为一个中子星星。休伊什和萨尔彼得的讲座中已经很好地讨论了这些问题。但是，正如他们所指出的，对于更大的质量，似乎不可能有这样的平衡状态。事实上，许多恒星的质量都比M大得多，以至于它们似乎不太可能脱落足够的物质，从而低于形成稳定白矮星（1.3M：M-M [1]）或中子星（1.7M：Oppenheimer-M-M [2]）所需的极限。因此，我们不得不考虑这样一种情况的后果：一颗星星坍缩到一种状态，在这种状态下，广义相对论的效应变得如此重要，以至于它们最终压倒了所有其他力。我将开始从广义相对论所呈现的我们现在可以称之为"经典"坍缩图景开始。之后将考虑对这一设想的异议和修改。主要的讨论是基于史瓦西的解决方案的爱因斯坦真空方程。这个解表示球对称物体外部的引力场。在最初的史瓦西坐标中，度规采用熟悉的形式
Stars whose masses are of the same order as that of the sun (M ) can find a final equilibrium state either as a white dwarf or, apparently, (after collapse and ejection of material) as a neutron star. These matters have been nicely discussed in the lectures of Hewish and Salpeter. But, as they have pointed out, for larger masses no such equilibrium state appears to be possible. Indeed, many stars are observed to have masses which are much larger than M —so large that it seems exceedingly unlikely that they can ever shed sufficient material so as to be able to fall below the limit required for a stable white dwarf ( ∼1.3M : Chandrasekhar [1]) or neutron star ( ∼0.7M : Oppenheimer-Volkoff [2]) to develop. We are thus driven to consider the consequences of a situation in which a star collapses right down to a state in which the effects of general relativity become so important that they eventually dominate over all other forces. I shall begin with what I think we may now call the “classical” collapse picture as presented by general relativity. Objections and modifications to this picture will be considered afterwards. The main discussion is based on Schwarzschild’s solution of the Einstein vacuum equations. This solution represents the gravitational field exterior to a spherically symmetrical body. In the original Schwarzschild co-ordinates, the metric takes the familiar form