scholarly journals Directly comparing GW150914 with numerical solutions of Einstein’s equations for binary black hole coalescence

2016 ◽  
Vol 94 (6) ◽  
Author(s):  
B. P. Abbott ◽  
R. Abbott ◽  
T. D. Abbott ◽  
M. R. Abernathy ◽  
F. Acernese ◽  
...  
2020 ◽  
Vol 37 (15) ◽  
pp. 154001 ◽  
Author(s):  
Julian Adamek ◽  
Cristian Barrera-Hinojosa ◽  
Marco Bruni ◽  
Baojiu Li ◽  
Hayley J Macpherson ◽  
...  

Author(s):  
Diego Fernández-Silvestre ◽  
Joshua Foo ◽  
Michael R.R Good

Abstract The Schwarzschild-de Sitter (SdS) metric is the simplest spacetime solution in general relativity with both a black hole event horizon and a cosmological event horizon. Since the Schwarzschild metric is the most simple solution of Einstein's equations with spherical symmetry and the de Sitter metric is the most simple solution of Einstein's equations with a positive cosmological constant, the combination in the SdS metric defines an appropriate background geometry for semi-classical investigation of Hawking radiation with respect to past and future horizons. Generally, the black hole temperature is larger than that of the cosmological horizon, so there is heat flow from the smaller black hole horizon to the larger cosmological horizon, despite questions concerning the definition of the relative temperature of the black hole without a measurement by an observer sitting in an asymptotically flat spacetime. Here we investigate the accelerating boundary correspondence (ABC) of the radiation in SdS spacetime without such a problem. We have solved for the boundary dynamics, energy flux and asymptotic particle spectrum. The distribution of particles is globally non-thermal while asymptotically the radiation reaches equilibrium.


2011 ◽  
Vol 23 (08) ◽  
pp. 865-882 ◽  
Author(s):  
İBRAHİM SEMİZ

We look for "static" spherically symmetric solutions of Einstein's Equations for perfect fluid source with equation of state p = wρ, for constant w. We consider all four cases compatible with the standard ansatz for the line element, discussed in previous work. For each case, we derive the equation obeyed by the mass function or its analogs. For these equations, we find all finite-polynomial solutions, including possible negative powers. For the standard case, we find no significantly new solutions, but show that one solution is a static phantom solution, another a black hole-like solution. For the dynamic and/or tachyonic cases we find, among others, dynamic and static tachyonic solutions, a Kantowski–Sachs (KS) class phantom solution, another KS-class solution for dark energy, and a second black hole-like solution. The black hole-like solutions feature segregated normal and tachyonic matter, consistent with the assertion of previous work. In the first black hole-like solution, tachyonic matter is inside the horizon, in the second, outside. The static phantom solution, a limit of an old one, is surprising at first, since phantom energy is usually associated with super-exponential expansion. The KS-phantom solution stands out since its "mass function" is a ninth order polynomial.


2021 ◽  
Vol 104 (2) ◽  
Author(s):  
T. Mishra ◽  
B. O’Brien ◽  
V. Gayathri ◽  
M. Szczepańczyk ◽  
S. Bhaumik ◽  
...  

2020 ◽  
Vol 102 (12) ◽  
Author(s):  
Collin D. Capano ◽  
Alexander H. Nitz
Keyword(s):  

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