Spherically symmetric systems of fields and black holes. II. Apparent horizon in canonical formalism

1984 ◽  
Vol 30 (6) ◽  
pp. 1178-1184 ◽  
Author(s):  
P. Hajicek
Keyword(s):  
Black Holes ◽  
Apparent Horizon ◽  
Canonical Formalism ◽  
Spherically Symmetric ◽  
Symmetric Systems

scholarly journals Thermodynamic structure of field equations near apparent horizon for radiating black holes

2014 ◽  
Vol 29 (34) ◽  
pp. 1450188 ◽  
Author(s):  
Uma Papnoi ◽  
Megan Govender ◽  
Sushant G. Ghosh
Keyword(s):  
Black Holes ◽  
Apparent Horizon ◽  
Higher Dimensions ◽  
Spherically Symmetric ◽  
Einstein Field Equations ◽  
Field Equations ◽  
Four Dimensions ◽  
Thermodynamic Structure ◽  
Kinematical Parameters

We study the intriguing analogy between gravitational dynamics of the horizon and thermodynamics for the case of nonstationary radiating spherically symmetric black holes both in four dimensions and higher dimensions. By defining all kinematical parameters of nonstationary radiating black holes in terms of null vectors, we demonstrate that it is possible to interpret the Einstein field equations near the apparent horizon in the form of a thermodynamical identity T dS = dE+P dV.

scholarly journals HAWKING RADIATION AS TUNNELING AND THE UNIFIED FIRST LAW OF THERMODYNAMICS FOR A CLASS OF DYNAMICAL BLACK HOLES

2009 ◽  
Vol 18 (11) ◽  
pp. 1707-1717 ◽  
Author(s):  
JIANG KE-XIA ◽  
KE SAN-MIN ◽  
PENG DAN-TAO
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Physical Meaning ◽  
Apparent Horizon ◽  
Null Geodesic ◽  
Tunneling Rate ◽  
Spherically Symmetric ◽  
Frw Universe ◽  
First Law Of Thermodynamics ◽  
Trapping Horizons

An analysis is made for relations between the tunneling rate and the unified first law of thermodynamics at the trapping horizons of two kinds of spherically symmetric dynamical black holes. The first kind is the Vaidya–Bardeen black hole; the tunneling rate Γ ~ e△S can be obtained naturally from the unified first law at the apparent horizon, which holds the form dEH = TdS + WdV. The second kind is the McVittie solution; the action of the radial null geodesic of the outgoing particles does not always have a pole at the apparent horizon, while the ingoing mode always has one. The solution of the ingoing mode of the radiation can be mathematically reduced to the case in the FRW universe smoothly. However, as a black hole, the physical meaning is unclear and even puzzling.

Perturbations of spherically symmetric black holes

1980 ◽  
Vol 77 (1) ◽  
pp. 7-8
Author(s):  
Basilis C. Xanthopoulos
Keyword(s):  
Black Holes ◽  
Spherically Symmetric
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