论文标题
一般相对论中的紧凑物体：从buchdahl星星到绝对孔
Compact objects in general relativity: From Buchdahl stars to quasiblack holes
论文作者
论文摘要
Buchdahl Star是一颗高度紧凑的恒星，边界半径$ r $ obeys $ r = \ frac98 r _+$，其中$ r _+$是恒星本身的引力半径。 Quasiblack孔是最大紧凑型星，或更一般的最大紧凑对象，边界半径$ r $ obeys $ r = r _+$。准布孔是成为黑洞的边缘的物体。持续的引力崩溃以黑洞结束，必须与Oppenheimer-Snyder形式主义一起处理。准危机收缩以准布孔结束，应使用适当的技术处理。米切尔（Mitchell）和拉普拉斯（Laplace）黑星的真正后代，是准布孔，而不是黑洞。准布孔具有许多有趣的属性。我们开发了一个准布孔的概念，给出了这样一个对象的几个示例，定义了它的含义，绘制其卡特 - 柔骨图，研究其压力特性，获得其质量配方，得出一个非Xtremal Quasiblack孔的熵，并通过极端的Quasiblack孔通过一个极端的黑孔的令人困惑的熵提供了解决方案。
A Buchdahl star is a highly compact star for which the boundary radius $R$ obeys $R=\frac98 r_+$, where $r_+$ is the gravitational radius of the star itself. A quasiblack hole is a maximum compact star, or more generically a maximum compact object, for which the boundary radius $R$ obeys $R=r_+$. Quasiblack holes are objects on the verge of becoming black holes. Continued gravitational collapse ends in black holes and has to be handled with the Oppenheimer-Snyder formalism. Quasistatic contraction ends in a quasiblack hole and should be treated with appropriate techniques. Quasiblack holes, not black holes, are the real descendants of Mitchell and Laplace dark stars. Quasiblack holes have many interesting properties. We develop the concept of a quasiblack hole, give several examples of such an object, define what it is, draw its Carter-Penrose diagram, study its pressure properties, obtain its mass formula, derive the entropy of a nonextremal quasiblack hole, and through an extremal quasiblack hole give a solution to the puzzling entropy of extremal black holes.
