arXiv subjects

Samir D. Mathur

Publications and source records attributed to Samir D. Mathur.

At least 145 records · Page 8Linked to original sources

arXiv1997

Emission rates, the Correspondence Principle and the Information Paradox

When we vary the moduli of a compactification it may become entropically favourable at some point for a state of branes and strings to rearrange itself into a new configuration. We observe that for the elementary string with two large charges such a rearrangement happens at the `correspondence point' where the string becomes a black hole. For smaller couplings it is entropically favourable for the excitations to be vibrations of the string, while for larger couplings the favoured excitations are pairs of solitonic 5-branes attached to the string; this helps resolve some recently noted difficulties with matching emission properties of the string to emission properties of the black hole. We also examine the change of state when a black hole is placed in a spacetime with an additional compact direction, and the size of this direction is varied. These studies suggest a mechanism that might help resolve the information paradox.

hep-th↗

arXiv1997

Absorption of angular momentum by black holes and D-branes

We consider the absorption of higher angular momentum modes of scalars into black holes, at low energies, and ask if the resulting cross sections are reproduced by a D-brane model. To get the correct dependence on the volume of the compactified dimensions, we must let the absorbing element in the brane model have a tension that is the geometric mean of the tensions of the D-string and an effective stringlike tension obtained from the D-5-brane; this choice is also motivated by T-duality. In a dual model we note that the correct dependence on the volume of the compact dimensions and the coupling arise if the absorbing string is allowed to split into many strings in the process of absorbing a higher angular momentum wave. We obtain the required energy dependence of the cross section by carrying out the integrals resulting from partitioning the energy of the incoming quantum into vibrations of the string.

hep-th↗

arXiv1997

Black Hole Greybody Factors and Absorption of Scalars by Effective Strings

We compute the greybody factors for classical black holes in a domain where two kinds of charges and their anticharges are excited by the extra energy over extremality. We compare the result to the greybody factors expected from an effective string model which was earlier shown to give the correct entropy. In the regime where the left and right moving temperatures are much smaller than the square root of the effective string tension, we find a non-trivial greybody factor which agrees with the effective string model. However, if the temperatures are comparable with the square root of the effective string tension, the greybody factors agree only at the leading order in energy. Nevertheless, there are several interesting relations between the two results, suggesting that a modification of the effective string model might lead to better agreement.

hep-th↗

arXiv1996

Comparing decay rates for black holes and D-branes

We compute the leading order (in coupling) rate of emission of low energy quanta from a slightly nonextremal system of 1 and 5 D-branes. We also compute the classical cross-section, and hence the Hawking emission rate, for low energy scalar quanta for the black hole geometry that corresponds to these branes (at sufficiently strong coupling). These rates are found to agree with each other.

hep-th↗

arXiv1996

Non-BPS excitations of D-branes and Black holes

This note discusses some results on the non-BPS excitations of D-branes. We show that the excitation spectrum of a bound state of D-strings changes character when the length of the wrapping circle becomes less than $\sim g^{-1}\LS$. We review the observed relation between the low energy absorption cross-section of D-branes and the low energy absorption cross-section for black holes. We discuss various issues related to the information question for black holes.

hep-th↗

arXiv1996

Universailty of Low Energy Absorption Cross-sections for Black Holes

In this paper we compute the low energy absorption cross-section for minimally coupled massles scalars and spin-$1/2$ particles, into a general spherically symmetric black hole in arbitrary dimensions. The scalars have a cross section equal to the area of the black hole, while the spin-$1/2$ particles give the area measured in a flat spatial metric conformally related to the true metric.

hep-th↗

arXiv1996

Interactions involving D-branes

We investigate some aspects of the spectrum of D-branes and their interactions with closed strings. As argued earlier, a collection of many D-strings behaves, at large dilaton values, as a single multiply wound string. We use this result and T-duality transformations to show that a similar phenomenon occurs for effective strings produced by wrapping p-branes on a small (p-1)-dimensional torus, for suitable coupling. To understand the decay of an excited D-string at large dilaton values, we study the decay of an elementary string at small dilaton values. A long string, multiply wound on a circle, with a small excitation energy is found to predominantly decay into another string with the same winding number and an unwound closed string (rather than two wound strings). This decay amplitude agrees, under duality, with the decay amplitude computed using the Born-Infeld action for the D-string. We compute the absorption cross section for the D-brane model studied by Callan and Maldacena. The absorption cross section for the dilaton equals that for the scalars obtained by reduction of the graviton, and both agree with the cross section expected from a classical hole with the same charges.

hep-th↗

arXiv1996

Quantum Gravity and Turning Points in the Semiclassical Approximation

The wavefunctional in quantum gravity gives an amplitude for 3-geometries and matter fields. The four-space is usually recovered in a semiclassical approximation where the gravity variables are taken to oscillate rapidly compared to matter variables; this recovers the Schrodinger evolution for the matter. We examine turning points in the gravity variables where this approximation appears to be troublesome. We investigate the effect of such a turning point on the matter wavefunction, in simple quantum mechanical models and in a closed minisuperspace cosmology. We find that after evolving sufficiently far from the turning point the matter wavefunction recovers to a form close to that predicted by the semiclassical approximation, and we compute the leading correction (from `backreaction') in a simple model. We also show how turning points can appear in the gravitational sector in dilaton gravity. We give some remarks on the behavior of the wavefunctional in the vicinity of turning points in the context of dilaton gravity black holes.

gr-qc↗

arXiv1996

Excitations of D-strings, Entropy and Duality

We examine the BPS and low energy non-BPS excitations of the D-string, in terms of open strings that travel on the D-string. We use this to study the energy thresholds for exciting a long D-string, for arbitrary winding number. We also compute the leading correction to the entropy from non-BPS states for a long D-string, and observe the relation of all these quantities with the corresponding quantities for the elementary string.

hep-th↗

arXiv1995

A Note on the Semi-Classical Approximation in Quantum Gravity

We re-examine the semiclassical approximation to quantum gravity in the canonical formulation, focusing on the definition of a quasiclassical state for the gravitational field. It is shown that a state with classical correlations must be a superposition of states of the form $e^{iS}$. In terms of a reduced phase space formalism, this type of state can be expressed as a coherent superposition of eigenstates of operators that commute with the constraints and so correspond to constants of the motion. Contact is made with the usual semiclassical approximation by showing that a superposition of this kind can be approximated by a WKB state with an appropriately localised prefactor. A qualitative analysis is given of the effects of geometry fluctuations, and the possibility of a breakdown of the semiclassical approximation due to interference between neighbouring classical trajectories is discussed. It is shown that a breakdown in the semiclassical approximation can be a coordinate dependent phenomenon, as has been argued to be the case close to a black hole horizon.

gr-qc↗

arXiv1995

Folds, Bosonization and non-triviality of the classical limit of 2D string theory

In the 1-dimensional matrix model one identifies the tachyon field in the asymptotic region with a nonlocal transform of the density of fermions. But there is a problem in relating the classical tachyon field with the surface profile of the fermi fluid if a fold forms in the fermi surface. Besides the collective field additional variables $w_j(x)$ are required to describe folds. In the quantum theory we show that the $w_j$ are the quantum dispersions of the collective field. These dispersions become $O(1)$ rather than $O(\hbar)$ precisely after fold formation, thus giving additional `classical' quantities and leading to a rather nontrivial classical limit. A coherent pulse reflecting from the potential wall turns into high energy incoherent quanta (if a fold forms), the frequency amplification being of the order of the square root of the number of quanta in the incident wave.

hep-th↗

arXiv1994

Black hole entropy and the semiclassical approximation

We compute the entropy of the Hawking radiation for an evaporating black hole, in 1+1 dimensions and in 3+1 dimensions. We investigate the validity of the semiclassical approximation for the evaporation process. It appears that there might be a large entropy of entanglement between the classical degrees of freedom describing the black hole and the radiation fields when the theory of quantum gravity plus matter is considered.

hep-th↗

arXiv1994

Evaporating Black Holes and Entropy

We study the Hawking radiation for the geometry of an evaporating 1+1 dimensional black hole. We compute Bogoliubov coefficients and the stress tensor. We use a recent result of Srednicki to estimate the entropy of entanglement produced in the evaporation process, for the 1+1 dimensional hole and for the 3+1 dimensional hole. It is found that the one space dimensional result of Srednicki is the pertinent one to use, in both cases.

hep-th↗

arXiv1993

Real Time Propagator in the First Quantised Formalism

We argue that a basic modification must be made to the first quantised formalism of string theory if the physics of `particle creation' is to be correctly described. The analogous quantisation of the relativistic particle is performed, and it is shown that the proper time along the world line must go both forwards and backwards (in the usual quantisation it only goes forwards). The matrix propagator of the real time formalism is obtained from the two directions of proper time. (Talk given at the Thermal Fields Workshop held at Banff, Canada (August 1993).)

hep-th↗

arXiv1993

Information Retrieval from a Charge `Trap'

We study the model of massless $1+1$ electrodynamics with nonconstant coupling, introduced by Peet, Susskind and Thorlacius as the `charge hole'. But we take the boundary of the strong coupling region to be first timelike, then spacelike for a distance $X$, and then timelike again (to mimic the structure of a black hole). For an incident charge pulse entering this `charge trap' the charge and information get separated. The charge comes out near the endpoint of the singularity. The `information' travels a well localised path through the strong coupling region and comes out later.

hep-th↗

arXiv1993

Is the Polyakov path integral prescription too restrictive?

In the first quantised description of strings, we integrate over target space co-ordinates $X^μ$ and world sheet metrics $g_{αβ}$. Such path integrals give scattering amplitudes between the `in' and `out' vacuua for a time-dependent target space geometry. For a complete description of `particle creation' and the corresponding backreaction, we need instead the causal amplitudes obtained from an `initial value formulation'. We argue, using the analogy of a scalar particle in curved space, that in the first quantised path integral one should integrate over $X^μ$ and world sheet {\it zweibiens}. This extended formalism can be made to yield causal amplitudes; it also naturally allows incorporation of density matrices in a covariant manner. (This paper is an expanded version of hep-th 9301044)

hep-th↗

arXiv1993

Kinetic theory in curved space: a first quantised approach

We study the real time formalism of non-equilibrium many-body theory, in a first quantised language. We argue that on quantising the relativistic scalar particle in spacetime with Minkowski signature, we should study both propagations $e^{i(p^2-m^2)\tilde λ}$ and $e^{-i(p^2-m^2)\tilde λ}$ on the particle world line. The path integral needs regulation at the mass shell $p^2=m^2$. If we regulate the two propagations independently we get the Feynman propagator in the vacuum, and its complex conjugate. But if the regulation mixes the two propagations then we get the matrix propagator appropriate to perturbation theory in a particle flux. This formalism unifies the special cases of thermal fluxes in flat space and the fluxes `created' by Cosmological expansion, and also gives covariance under change of particle definition in curved space. We comment briefly on the proposed application to closed strings, where we argue that coherent fields and `exponential of quadratic' particle fluxes must {\it both} be used to define the background for perturbation theory.

hep-th↗

arXiv1992

Eluding the no-hair conjecture: Black holes in spontaneously broken gauge theories

We study regular and black hole solutions to the coupled classical Einstein--Yang-Mills--Higgs system. It has long been thought that black hole solutions in the spontaneously broken phase of such a theory could have no nontrivial field structure outside of the horizon. We first show that the standard black hole no-hair theorem underlying this belief, although true in the abelian setting, does not necessarily extend to the non-abelian case. This indicates the possibility of solutions with non-trivial gauge and Higgs configurations decaying exponentially {\it outside} the horizon. We then find such solutions by numerical integration of the classical equations for the case of $SU(2)$ coupled to a Higgs doublet (the standard model less hypercharge). As a prelude to this work we also study regular and black hole solutions to Einstein--Non-Abelian--Proca theory and as a postscript we briefly discuss the important issue of stability.

hep-th↗