scholarly journals The charged black-hole bomb: A lower bound on the charge-to-mass ratio of the explosive scalar field

2016 ◽  
Vol 755 ◽  
pp. 177-182 ◽  
Author(s):  
Shahar Hod
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Lower Bound ◽  
Charged Black Hole ◽  
Mass Ratio

Entropy in a d-dimensional charged black hole

2018 ◽  
Vol 33 (27) ◽  
pp. 1850159 ◽  
Author(s):  
Shad Ali ◽  
Xin-Yang Wang ◽  
Wen-Biao Liu
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Hawking Radiation ◽  
Space Time ◽  
Charged Black Hole ◽  
Schwarzschild Black Hole ◽  
Proportionality Coefficient ◽  
Proportional Relation ◽  
Hamiltonian Analysis ◽  
Interior Volume

Christodoulou and Rovelli have shown that the interior volume of a Schwarzschild black hole grows linearly with time. The entropy of a scalar field in this interior volume of a Schwarzschild black hole has been calculated and shown to increase linearly with the advanced time too. In this paper, considering Hawking radiation from a d-dimensional charged black hole, we investigate the proportional relation between the entropy of the scalar field in the interior volume and the Bekenstein–Hawking entropy using the method of our previous work. We also derive this proportionality relation using Hamiltonian analysis and find a consistent result. We then investigate the proportionality coefficient with respect to d and find that it gradually decreases as the dimension of space–time increases.

scholarly journals Physics of the interior of a spherical, charged black hole with a scalar field

2005 ◽  
Vol 71 (6) ◽  
Author(s):  
Jakob Hansen ◽  
Alexei Khokhlov ◽  
Igor Novikov
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Charged Black Hole

scholarly journals The heavier the better: how to constrain mass ratios and spins of high-mass neutron star mergers

2020 ◽  
Vol 496 (1) ◽  
pp. L16-L21 ◽  
Author(s):  
Elias R Most ◽  
Lukas R Weih ◽  
Luciano Rezzolla
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Lower Bound ◽  
Equations Of State ◽  
High Mass ◽  
Maximum Mass ◽  
Mass Ratio ◽  
Effective Spin ◽  
Binary Neutron Star ◽  
Merger Event

ABSTRACT The first binary neutron star merger event, GW170817, and its bright electromagnetic counterpart have provided a remarkable amount of information. By contrast, the second event, GW190425, with $M_{\rm tot}=3.4^{+0.3}_{-0.1}\, \mathrm{ M}_{\odot }$ and the lack of an electromagnetic counterpart, has hardly improved our understanding of neutron star physics. While GW190425 is compatible with a scenario in which the merger has led to a prompt collapse to a black hole and little ejected matter to power a counterpart, determining the mass ratio and the effective spin $\tilde{\chi }$ of the binary remains difficult. This is because gravitational waveforms cannot yet well constrain the component spins of the binary. However, since the mass of GW190425 is significantly larger than the maximum mass for non-rotating neutron stars, $M_{_{\rm TOV}}$, the mass ratio q cannot be too small, as the heavier star would not be gravitationally stable. Making use of universal relations and a large number of equations of state, we provide limits in the $(\tilde{\chi },q)$ plane for GW190425, namely qmin ≥ 0.38 and $\tilde{\chi }_{\rm max}\le 0.20$, assuming $M_\mathrm{tot} \simeq 3.4\, \mathrm{ M}_\odot$. Finally, we show how future observations of high-mass binaries can provide a lower bound on $M_{_{\rm TOV}}$.

scholarly journals Addendum to “Absorption of a massive scalar field by a charged black hole”

2017 ◽  
Vol 95 (4) ◽  
Author(s):  
Carolina L. Benone ◽  
Ednilton S. de Oliveira ◽  
Sam R. Dolan ◽  
Luís C. B. Crispino
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Charged Black Hole ◽  
Massive Scalar ◽  
Massive Scalar Field

CAN A BLACK HOLE BE USED AS A PORTAL TO OTHER UNIVERSES?

2002 ◽  
Vol 11 (10) ◽  
pp. 1561-1566 ◽  
Author(s):  
LIOR M. BURKO
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Compact Support ◽  
Space Time ◽  
Charged Black Hole ◽  
Cauchy Horizon

We study numerically the evolution of space-time inside a black hole under perturbations of non-compact support. Using a very simplified toy model of a spherical charged black hole which is perturbed nonlinearly by a self-gravitating, spherical scalar field, we find that a portion of the Cauchy horizon survives as a non-central, null singularity.

BEYOND THE HORIZON TO UNKNOWN TERRITORIES: THE SINGULARITY INSIDE BLACK HOLES

1999 ◽  
Vol 14 (15) ◽  
pp. 1015-1019 ◽  
Author(s):  
LIOR M. BURKO
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Scalar Field ◽  
Nonlinear Effects ◽  
Charged Black Hole ◽  
Cauchy Horizon ◽  
Weak Singularity

We study the Cauchy horizon singularity inside a spherical charged black hole, coupled to a self-gravitating scalar field. We show that all the radial causal geodesics terminate at a weak singularity according to the Tipler classification. Our result is valid anywhere along the singularity, in particular in the regime where nonlinear effects are crucial.

scholarly journals CONDENSATION OF THE SCALAR FIELD WITH STUCKELBERG AND WEYL CORRECTIONS IN THE BACKGROUND OF A PLANAR AdS–SCHWARZSCHILD BLACK HOLE

2012 ◽  
Vol 27 (22) ◽  
pp. 1250128 ◽  
Author(s):  
D. MOMENI ◽  
M. R. SETARE ◽  
RATBAY MYRZAKULOV
Keyword(s):  
Black Hole ◽  
Stability Analysis ◽  
Critical Temperature ◽  
Scalar Field ◽  
Lower Bound ◽  
Chemical Potential ◽  
Numerical Estimate ◽  
Schwarzschild Black Hole ◽  
Holographic Superconductors ◽  
Analytical Properties

We study analytical properties of the Stuckelberg holographic superconductors with Weyl corrections. We obtain the minimum critical temperature as a function of the mass of the scalar field m2. We show that in limit of the [Formula: see text] which is close to the numerical estimate [Formula: see text]. Further we show that the mass of the scalar field is bounded from below by the [Formula: see text] where [Formula: see text]. This lower bound is weaker and different from the previous lower bound m2 = -3 predicted by stability analysis. We show that in the Breitenlohner–Freedman bound, the critical temperature remains finite. Explicitly, we prove that here there exists a linear relation between 〈OΔ〉 and the chemical potential.

Sign in / Sign up

Export Citation Format

Share Document