44 research outputs found
Cauchy horizon singularity without mass inflation
A perturbed Reissner-Nordstr\"om-de Sitter solution is used to emphasize the
nature of the singularity along the Cauchy horizon of a charged spherically
symmetric black hole. For these solutions, conditions may prevail under which
the mass function is bounded and yet the curvature scalar
diverges.Comment: typeset in RevTex, 13 page
Surface-Gravity Inequalities and Generic Conditions for Strong Cosmic Censorship
Transforming Penrose's intuitive picture of a strong cosmic censorship
principle, that generically forbids the appearance of locally naked space-time
singularities, into a formal mathematical proof, remains at present, one of the
most outstanding unsolved mathematical problems from the theory of
gravitational collapse. Part of the difficulty lies in the fact that we do not
possess yet a clear-cut understanding of the hypothesis needed for the
establishment of some sort of strong cosmic censorship theorem. What we have is
a selected list of solutions, which at first sight seem to go against cosmic
censorship, but at the end they fail in some way. However, the space of
solutions of Einstein's field equations is vast. In this article, we plan to
increase one's intuition by establishing a link between certain inequalities
for Cauchy-horizon stability and a set of generic conditions, such as a
reasonable equation of state--which determines whether the space-time is
asymptotically flat or not, an energy condition, and an hypothesis over the
class of metrics on which Einstein's field equations ought to be solved to
ensure strong cosmic censorship inside black-holes. With these tools in hand we
examine the Cauchy-horizon stability of the theory created by Born and
Infeld--whose action principle has been used as a prototype in superstring
theory, and the singularity-free Bardeen's black-hole model.Comment: 6 pages, 2 figures(type eps), REVTeX
Kink Stability of Self-Similar Solutions of Scalar Field in 2+1 Gravity
The kink stability of self-similar solutions of a massless scalar field with
circular symmetry in 2+1 gravity is studied, and found that such solutions are
unstable against the kink perturbations along the sonic line (self-similar
horizon). However, when perturbations outside the sonic line are considered,
and taking the ones along the sonic line as their boundary conditions, we find
that non-trivial perturbations do not exist. In other words, the consideration
of perturbations outside the sonic line limits the unstable mode of the
perturbations found along the sonic line. As a result, the critical solution
for the scalar collapse remains critical even after the kink perturbations are
taken into account.Comment: latex, one figur
Absorption and quasinormal modes of classical fields propagating on 3D and 4D de Sitter spacetime
We extensively study the exact solutions of the massless Dirac equation in 3D
de Sitter spacetime that we published recently. Using the Newman-Penrose
formalism, we find exact solutions of the equations of motion for the massless
classical fields of spin s=1/2,1,2 and to the massive Dirac equation in 4D de
Sitter metric. Employing these solutions, we analyze the absorption by the
cosmological horizon and de Sitter quasinormal modes. We also comment on the
results given by other authors.Comment: 31 page
Interior Structure of a Charged Spinning Black Hole in -Dimensions
The phenomenon of mass inflation is shown to occur for a rotating black hole.
We demonstrate this feature in dimensions by extending the charged
spinning BTZ black hole to Vaidya form. We find that the mass function diverges
in a manner quantitatively similar to its static counterparts in ,
and dimensions.Comment: 5 pages, 2 figures (appended as postscript files), WATPHYS-TH94/0
Domain Wall Spacetimes: Instability of Cosmological Event and Cauchy Horizons
The stability of cosmological event and Cauchy horizons of spacetimes
associated with plane symmetric domain walls are studied. It is found that both
horizons are not stable against perturbations of null fluids and massless
scalar fields; they are turned into curvature singularities. These
singularities are light-like and strong in the sense that both the tidal forces
and distortions acting on test particles become unbounded when theses
singularities are approached.Comment: Latex, 3 figures not included in the text but available upon reques
Gravitational Radiation Theory and Light Propagation
The paper gives an introduction to the gravitational radiation theory of isolated sources and to the propagation properties of light rays in radiative gravitational fields. It presents a theoretical study of the generation, propagation, back-reaction, and detection of gravitational waves from astrophysical sources. After reviewing the various quadrupole-moment laws for gravitational radiation in the Newtonian approximation, we show how to incorporate post-Newtonian corrections into the source multipole moments, the radiative multipole moments at infinity, and the back-reaction potentials. We further treat the light propagation in the linearized gravitational field outside a gravitational wave emitting source. The effects of time delay, bending of light, and moving source frequency shift are presented in terms of the gravitational lens potential. Time delay results are applied in the description of the procedure of the detection of gravitational waves
Large-Eddy Simulations of Magnetohydrodynamic Turbulence in Heliophysics and Astrophysics
We live in an age in which high-performance computing is transforming the way we do science. Previously intractable problems are now becoming accessible by means of increasingly realistic numerical simulations. One of the most enduring and most challenging of these problems is turbulence. Yet, despite these advances, the extreme parameter regimes encountered in space physics and astrophysics (as in atmospheric and oceanic physics) still preclude direct numerical simulation. Numerical models must take a Large Eddy Simulation (LES) approach, explicitly computing only a fraction of the active dynamical scales. The success of such an approach hinges on how well the model can represent the subgrid-scales (SGS) that are not explicitly resolved. In addition to the parameter regime, heliophysical and astrophysical applications must also face an equally daunting challenge: magnetism. The presence of magnetic fields in a turbulent, electrically conducting fluid flow can dramatically alter the coupling between large and small scales, with potentially profound implications for LES/SGS modeling. In this review article, we summarize the state of the art in LES modeling of turbulent magnetohydrodynamic (MHD) ows. After discussing the nature of MHD turbulence and the small-scale processes that give rise to energy dissipation, plasma heating, and magnetic reconnection, we consider how these processes may best be captured within an LES/SGS framework. We then consider several special applications in heliophysics and astrophysics, assessing triumphs, challenges,and future directions