Abstract
This chapter is devoted to some physical properties of black holes, including a discussion of their thermodynamics, black hole laws, quantum effects, black hole magnetospheres, interiors, and singularities. The chapter opens with a discussion on the formation of black holes in astrophysical environments.
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- 1.
The reader is referred for numerical calculations to the book by Baumgarte and Shapiro (2010) and references therein.
- 2.
The solar luminosity is L ⊙≈3.8×1033 erg s−1.
- 3.
In Cartesian coordinates the Kerr singularity occurs at x 2+y 2=a 2 c −2 and z=0.
- 4.
A space is said to be compact if whenever one takes an infinite number of “steps” in the space, eventually one must get arbitrarily close to some other point of the space. Thus, whereas disks and spheres are compact, infinite lines and planes are not, nor is a disk or a sphere with a missing point. In the case of an infinite line or plane, one can set off making equal steps in any direction without approaching any point, so that neither space is compact. In the case of a disk or sphere with a missing point, one can move toward the missing point without approaching any point within the space. More formally, a topological space is compact if, whenever a collection of open sets covers the space, some sub-collection consisting only of finitely many open sets also covers the space. A topological space is called compact if each of its open covers has a finite sub-cover. Otherwise it is called non-compact. Compactness, when defined in this manner, often allows one to take information that is known locally—in a neighborhood of each point of the space—and to extend it to information that holds globally throughout the space.
- 5.
A set of points in a space-time with no two points of the set having time-like separation.
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Romero, G.E., Vila, G.S. (2014). Black Hole Physics. In: Introduction to Black Hole Astrophysics. Lecture Notes in Physics, vol 876. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-39596-3_3
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