scholarly journals Complete gauge-invariant formalism for arbitrary second-order perturbations of a Schwarzschild black hole

2009 ◽  
Vol 80 (2) ◽  
Author(s):  
David Brizuela ◽  
José M. Martín-García ◽  
Manuel Tiglio
Keyword(s):  
Black Hole ◽  
Second Order ◽  
Schwarzschild Black Hole ◽  
Gauge Invariant

scholarly journals THE EVENT HORIZON OF THE SCHWARZSCHILD BLACK HOLE IN NONCOMMUTATIVE SPACES

2006 ◽  
Vol 15 (07) ◽  
pp. 1113-1117 ◽  
Author(s):  
FOROUGH NASSERI
Keyword(s):  
Black Hole ◽  
Event Horizon ◽  
Lower Limit ◽  
Second Order ◽  
Schwarzschild Black Hole ◽  
Perturbative Calculations ◽  
First Order ◽  
Noncommutative Spaces

The event horizon of the Schwarzschild black hole is obtained in noncommutative spaces up to the second order of perturbative calculations. Because this type of black hole is non-rotating, to the first order there is no effect on the event horizon due to the noncommutativity of space. A lower limit for the noncommutativity parameter is also obtained. As a result, the event horizon in noncommutative spaces is less than the event horizon in commutative spaces.

scholarly journals Second Order Perturbations of a Schwarzschild Black Hole: Inclusion of Odd Parity Perturbations

2000 ◽  
Vol 32 (10) ◽  
pp. 2021-2042 ◽  
Author(s):  
Carlos O. Nicasio ◽  
Reinaldo Gleiser ◽  
Jorge Pullin
Keyword(s):  
Black Hole ◽  
Second Order ◽  
Schwarzschild Black Hole

scholarly journals Second-order perturbations of a Schwarzschild black hole

1996 ◽  
Vol 13 (10) ◽  
pp. L117-L124 ◽  
Author(s):  
Reinaldo J Gleiser ◽  
Carlos O Nicasio ◽  
Richard H Price ◽  
Jorge Pullin
Keyword(s):  
Black Hole ◽  
Second Order ◽  
Schwarzschild Black Hole

The Schwarzschild black hole

2018 ◽  
Author(s):  
Nathalie Deruelle ◽  
Jean-Philippe Uzan
Keyword(s):  
Black Hole ◽  
Gravitational Field ◽  
Equilibrium Configuration ◽  
Original Form ◽  
Schwarzschild Black Hole ◽  
Schwarzschild Metric ◽  
Schwarzschild Geometry

This chapter discusses the Schwarzschild black hole. It demonstrates how, by a judicious change of coordinates, it is possible to eliminate the singularity of the Schwarzschild metric and reveal a spacetime that is much larger, like that of a black hole. At the end of its thermonuclear evolution, a star collapses and, if it is sufficiently massive, does not become stabilized in a new equilibrium configuration. The Schwarzschild geometry must therefore represent the gravitational field of such an object up to r = 0. This being said, the Schwarzschild metric in its original form is singular, not only at r = 0 where the curvature diverges, but also at r = 2m, a surface which is crossed by geodesics.

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