Center of mass energy of charged particles about Reissner–Nordström black hole

We study the acceleration of charged particles by Reissner Nordström black hole by taking into account the term appearing in the formula of the center of mass energy due to charge of the particle. We consider that the particle is radially falling towards the black hole, i.e., [Formula: see text]. It is found that the center of mass energy is infinitely large at the outer horizon without any constraint.

Particle spectrum of the Reissner–Nordström black hole

The Reissner–Nordström black hole – moving mirror correspondence is solved. The beta coefficients reveal that charge makes a black hole radiate fewer particles (neutral massless scalars) per frequency. An old Reissner–Nordström black hole emits particles in an explicit Planck distribution with temperature corresponding to the surface gravity of its outer horizon.

A simple quantum test for smooth horizons

We develop a new test that provides a necessary condition for a quantum state to be smooth in the vicinity of a null surface: “near-horizon modes” that can be defined locally near any patch of the null surface must be correctly entangled with each other and with their counterparts across the surface. This test is considerably simpler to implement than a full computation of the renormalized stress-energy tensor. We apply this test to Reissner-Nordström black holes in asymptotically anti-de Sitter space and provide numerical evidence that the inner horizon of such black holes is singular in the Hartle-Hawking state. We then consider BTZ black holes, where we show that our criterion for smoothness is satisfied as one approaches the inner horizon from outside. This results from a remarkable conspiracy between the properties of mode-functions outside the outer horizon and between the inner and outer horizon. Moreover, we consider the extension of spacetime across the inner horizon of BTZ black holes and show that it is possible to define modes behind the inner horizon that are correctly entangled with modes in front of the inner horizon. Although this provides additional suggestions for the failure of strong cosmic censorship, we lay out several puzzles that must be resolved before concluding that the inner horizon will be traversable.

Quasinormal modes of massive scalar field with nonminimal coupling in higher-dimensional de Sitter black hole with single rotation

We analytically investigate the quasinormal modes of the massive scalar field with a nonminimal coupling in the higher-dimensional de Sitter black hole with a single rotation. According to the separated scalar field equation, the boundary conditions of quasinormal modes are well constructed at the outer and cosmological horizons. Then, under near-extremal conditions, where the outer horizon closes to the cosmological horizon, the quasinormal frequencies are obtained and generalized to universal form in the higher-dimensional spacetime. Here, the real part of the frequency includes the scalar field contents, and its imaginary part only depends on the surface gravity at the outer horizon of the black hole.

Behavior of null-geodesics in the interior of Reissner–Nordstrom black hole

We show that an incoming null-geodesic belonging to a plane passing through the origin and starting outside the outer horizon crosses the outer and the inner horizons. Then it turns at some point inside the inner horizon and approaches the inner horizon when the time tends to infinity. We also construct a geometric optics solution of the Reissner–Nordstrom equation that has support in a neighborhood of the null-geodesic.

THERMODYNAMICAL PROPERTIES AND QUASI-LOCALIZED ENERGY OF THE STRINGY DYONIC BLACK HOLE SOLUTION

In this paper, we calculate the heat flux passing through the horizon TS|rh and the difference of energy between the Einstein and Møller prescription within the region [Formula: see text], in which is the region between outer horizon [Formula: see text] and inner horizon [Formula: see text], for the modified GHS solution, KLOPP solution and CLH solution. The formula [Formula: see text]TS is obeyed for the mGHS solution and the KLOPP solution, but not for the CLH solution. Also, we suggest a RN-like stringy dyonic black hole solution, which comes from the KLOPP solution under a dual transformation, and its thermodynamical properties are the same as the KLOPP solution.

MAPPING HAWKING TEMPERATURE IN THE SPINNING CONSTANT CURVATURE BLACK HOLE SPACES INTO UNRUH TEMPERATURE

We established the equivalence between the local Hawking temperature measured by the time-like Killing observer located at some positions r with finite distances from the outer horizon r+ in the five-dimensional spinning black hole space with both negative and positive constant curvature, and the Unruh temperature measured by the Rindler observer with constant acceleration in the six-dimensional flat space by employing the globally embedding approach.

Imaginary-frequency interior modes of black holes

Perturbations of black holes (Schwarzschild, Reissner-Nordstrøm and Kerr) can be treated by simple radial wave equations. It is shown that the massless scalar radial equation is a form of the spin-weighted spheroidal wave equation. The region in r corresponding to the usual angular argument (cos 0, 0 real) for such functions is the black hole interior, r E (r - r + ) where r - , r + are the inner and outer horizon radii respectively. We restrict ourselves to axisymmetric scalar waves. (Because of the spherical symmetry this is no restriction in the Schwarzschild and Reissner-Nordstrøm backgrounds, but it is a physical restriction in the Kerr background.) In these cases the spin-weighted spheroidal harmonics correspond to imaginary-frequency waves, i.e. to exponentially growing or decaying waves that fall inward across the outer horizon r+ and are converted to waves moving in the opposite direction as they cross the r _-horizon (r is a timelike coordinate when r e( r _ , r + )). These modes are exactly analogous to the external quasi-normal modes of the black hole. There is always one zero-frequency mode, and l non-zero imaginaryfrequency modes. Here l is the angular momentum eigen-number associated with the angular decomposition.