scholarly journals Bouncing cosmologies in massive gravity on de Sitter

2013 ◽  
Vol 30 (20) ◽  
pp. 205012 ◽  
Author(s):  
David Langlois ◽  
Atsushi Naruko
Keyword(s):  
Massive Gravity ◽  
De Sitter ◽  
Bouncing Cosmologies

scholarly journals The third way to 3D gravity

2015 ◽  
Vol 24 (12) ◽  
pp. 1544015 ◽  
Author(s):  
Eric Bergshoeff ◽  
Wout Merbis ◽  
Alasdair J. Routh ◽  
Paul K. Townsend
Keyword(s):  
Equations Of Motion ◽  
Massive Gravity ◽  
De Sitter ◽  
Gravitational Field Equation ◽  
Third Way ◽  
Metric Tensor ◽  
The Third ◽  
Higher Dimensional ◽  
Conservation Condition ◽  
3D Gravity

Consistency of Einstein’s gravitational field equation [Formula: see text] imposes a “conservation condition” on the [Formula: see text]-tensor that is satisfied by (i) matter stress tensors, as a consequence of the matter equations of motion and (ii) identically by certain other tensors, such as the metric tensor. However, there is a third way, overlooked until now because it implies a “nongeometrical” action: one not constructed from the metric and its derivatives alone. The new possibility is exemplified by the 3D “minimal massive gravity” model, which resolves the “bulk versus boundary” unitarity problem of topologically massive gravity with Anti-de Sitter asymptotics. Although all known examples of the third way are in three spacetime dimensions, the idea is general and could, in principle, apply to higher dimensional theories.

scholarly journals Quantum topologically massive gravity in de Sitter space

2011 ◽  
Vol 2011 (8) ◽  
Author(s):  
Alejandra Castro ◽  
Nima Lashkari ◽  
Alexander Maloney
Keyword(s):  
De Sitter Space ◽  
Massive Gravity ◽  
De Sitter ◽  
Topologically Massive Gravity

scholarly journals On the black holes in alternative theories of gravity: The case of nonlinear massive gravity

2015 ◽  
Vol 24 (03) ◽  
pp. 1550022 ◽  
Author(s):  
Ivan Arraut
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Degrees Of Freedom ◽  
Massive Gravity ◽  
Alternative Theories Of Gravity ◽  
De Sitter ◽  
Theories Of Gravity ◽  
Bound Orbits ◽  
Black Hole Temperature ◽  
Alternative Theories

I derive general conditions in order to explain the origin of the Vainshtein radius inside dRGT. The set of equations, which I have called "Vainshtein" conditions are extremal conditions of the dynamical metric (gμν) containing all the degrees of freedom of the theory. The Vainshtein conditions are able to explain the coincidence between the Vainshtein radius in dRGT and the scale [Formula: see text], obtained naturally from the Schwarzschild de-Sitter (S-dS) space inside general relativity (GR). In GR, this scale was interpreted as the maximum distance in order to get bound orbits. The same scale corresponds to the static observer position if we want to define the black hole temperature in an asymptotically de-Sitter space. In dRGT, the scale marks a limit after which the extra degrees of freedom of the theory become relevant.

Thermal corrections of Born–Infeld–anti-de Sitter black hole in massive gravity

2019 ◽  
Vol 34 (27) ◽  
pp. 1950222
Author(s):  
Abdul Jawad ◽  
Shahid Chaudhary
Keyword(s):  
Black Hole ◽  
Critical Points ◽  
Thermal Fluctuations ◽  
Massive Gravity ◽  
Vital Role ◽  
De Sitter ◽  
Logarithmic Corrections ◽  
The Impact

The impact of thermal fluctuations on the thermodynamics of Born–Infeld–anti-de Sitter black hole is being investigated. For this purpose, we analyze the consequences of logarithmic corrections on thermodynamics potentials like Helmholtz and Gibbs. We find out the relations for critical points and stability and observe that thermal corrections play a vital role in them.

scholarly journals Probing correlation between photon orbits and phase structure of charged AdS black hole in massive gravity background

2019 ◽  
Vol 34 (35) ◽  
pp. 1950231 ◽  
Author(s):  
M. Chabab ◽  
H. El Moumni ◽  
S. Iraoui ◽  
K. Masmar
Keyword(s):  
Phase Transition ◽  
Black Holes ◽  
Black Hole ◽  
Phase Structure ◽  
Black Hole Solution ◽  
Massive Gravity ◽  
Direct Link ◽  
De Sitter ◽  
Thermodynamic Phase ◽  
The Impact

The phase structure of charged anti-de Sitter black hole in massive gravity is investigated using the unstable circular photon orbits formalism, concretely we establish a direct link between the null geodesics and the critical behavior thermodynamic of such black hole solution. Our analysis reveals that the radius and the impact parameter corresponding to the unstable circular orbits can be used to probe the thermodynamic phase structure. We also show that the latter are key quantities to characterize the order of Van der Waals-like phase transition. Namely, we found a critical exponent around [Formula: see text]. All these results support further that the photon trajectories can be used as a useful and crucial tool to probe the thermodynamic black holes criticality.

scholarly journals Massive gravity on de Sitter and unique candidate for partially massless gravity

2013 ◽  
Vol 2013 (01) ◽  
pp. 035-035 ◽  
Author(s):  
Claudia de Rham ◽  
Sébastien Renaux-Petel
Keyword(s):  
Massive Gravity ◽  
De Sitter

scholarly journals De Sitter vacua in ghost-free massive gravity theory

2015 ◽  
Vol 751 ◽  
pp. 19-24 ◽  
Author(s):  
Charles Mazuet ◽  
Mikhail S. Volkov
Keyword(s):  
Massive Gravity ◽  
Gravity Theory ◽  
De Sitter ◽  
De Sitter Vacua

scholarly journals Hawking evaporation of black holes in massive gravity

2020 ◽  
Vol 80 (11) ◽  
Author(s):  
Meng-Shi Hou ◽  
Hao Xu ◽  
Yen Chin Ong
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Null Geodesic ◽  
Massive Gravity ◽  
Late Time ◽  
De Sitter ◽  
Emission Surface ◽  
Metric Function ◽  
The Impact ◽  
Hawking Evaporation

AbstractWe study the Hawking evaporation of a class of black hole solutions in dRGT massive gravity, in which the graviton mass gives rise to an effective negative cosmological constant. We found that the effective emission surface can be either proportional to the square of the effective AdS length scale, or corresponds to the square of the impact parameter of the null geodesic that falls onto the photon orbit of the black hole. Furthermore, depending on the black hole parameters, the emission surface could switch from one to another as the black hole loses mass during the evaporation process. Furthermore, the black holes can either evaporate completely or become a remnant at late time. Our result is more generally applicable to any asymptotically anti-de Sitter-like black hole solution in any theory whose metric function has a term linear in the coordinate radius, with massive gravity being only a concrete example.

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