Abstract
This chapter introduces the basic solutions of Einstein field equations that describe black holes. Motion of particles in the vicinity of black holes, space-time structure, and other elemental properties of each solution are discussed. Brief discussions are also presented on mini-black holes, Born-Infeld black holes, f(R) black holes, and regular black holes.
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Notes
- 1.
Asymptotic flatness is a property of the geometry of space-time which means that in appropriate coordinates, the limit of the metric at infinity approaches the metric of the flat (Minkowskian) space-time.
- 2.
Notice that dv loc/dτ=(dv loc/dr)(dr/dτ)=(dv loc/dr)v loc=r g c 2/r 2.
- 3.
We remind that two geometries are conformally equivalent if there exists a conformal transformation (an angle-preserving transformation) that maps one geometry to the other. More generally, two (pseudo) Riemannian metrics on a manifold M are conformally equivalent if one is obtained from the other through multiplication by a function on M.
- 4.
The relation with Boyer-Lindquist coordinates is z=rcosθ, \(x=\sqrt{r^{2}+a^{2}c^{-2}} \sin\theta\cos\phi\), \(y=\sqrt{r^{2}+a^{2}c^{-2}} \sin\theta\sin\phi\).
- 5.
\(F(\gamma, k)=\int_{0}^{\gamma}(1-k^{2}\sin^{2}\phi )^{-1/2}d\phi=\int_{0}^{\sin\gamma }[(1-z^{2})(1-k^{2}z^{2})]^{-1/2}dz \).
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Romero, G.E., Vila, G.S. (2014). Black Holes. 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_2
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