arXiv subjects

S. Kalyana Rama

Publications and source records attributed to S. Kalyana Rama.

69 records · Page 4Linked to original sources

arXiv1996

Short Distance Repulsive Gravity as a Consequence of Non Trivial PPN Parameters $β$ and $γ$

We look for a graviton-dilaton theory which can predict non trivial values of the PPN parameters $β$ and/or $γ$ for a charge neutral point star, without any naked singularity. With the potential for dilaton $ϕ$ set to zero, it contains one arbitrary function $ψ(ϕ)$. Our requirements impose certain constraints on $ψ$, which lead to the following generic and model independent novel results: For a charge neutral point star, the gravitational force becomes repulsive at distances of the order of, but greater than, the Schwarzschild radius $r_0$. There is also no horizon for $r > r_0$. These results suggest that black holes are unlikely to form in a stellar collapse in this theory.

hep-th↗

arXiv1996

F-theory from Dirichlet 3-branes

Starting from the type IIB Dirichlet 3-brane action, we obtain a Nambu-Goto action. It is interpreted as the world volume action of a fundamental 3-brane, and its target space theory as F-theory. The target space is twelve dimensional, with signature $(11, 1)$. It is an elliptic fibration over a ten dimensional base space. The $SL(2, Z)$ symmetry of type IIB string has now an explicit geometric interpretation. Also, one gets a glimpse of the conjectured self-duality of M-theory.

hep-th↗

arXiv1995

Singularities in Graviton-Dilaton System: Their Implications on the PPN Parameters and the Cosmological Constant

Alternatives to Einstein's theory of general relativity can be distinguished by measuring the parametrised post Newtonian parameters. Two such parameters $β$ and $γ$, equal to one in Einstein theory, can be obtained from static spherically symmetric solutions. For the graviton-dilaton system, as in Brans-Dicke or low energy string theory, we find that if $γ\ne 1$ for a charge neutral point star, then there exist naked singularities. Thus, if $γ$ is measured to be different from one, then it cannot be explained by these theories, without implying naked singularities. We also couple a cosmological constant $Λ$ to the graviton-dilaton system, a la string theory. We find that static spherically symmetric solutions in low energy string theory, which describe the gravitational field of a point star in the real universe atleast upto a distance $r_* \simeq {\cal O} ({\rm pc})$, always lead to curvature singularities. These singularities are stable and much worse than the naked ones. Requiring their absence upto a distance $r_*$ implies a bound $| Λ| < 10^{- 102} (\frac{r_*}{\rm pc})^{- 2}$ in natural units. If $r_* \simeq 1 {\rm Mpc}$ then $| Λ| < 10^{- 114}$, and if $r_*$ extends all the way upto the edge of the universe ($10^{28} {\rm cm}$) then $| Λ| < 10^{- 122}$ in natural units.

hep-th↗

arXiv1995

Implications of Some Static Spherically Symmetric Graviton-Dilaton Solutions in Brans-Dicke and Low Energy String Theory

Analysing the static, spherically symmetric graviton-dilaton solutions in low energy string and Brans-Dicke theory, we find the following. For a charge neutral point star, these theories cannot predict non trivial PPN parameters, $β$ and $γ$, without introducing naked singularities. We then couple a cosmological constant $Λ$ as in low energy string theory. We find that only in low energy string theory, a non zero $Λ$ leads to a curvature singularity, which is much worse than a naked singularity. Requiring its absence upto a distance $r_*$ implies a bound $| Λ| < 10^{- 102} (\frac{r_*}{\rm pc})^{- 2}$ in natural units. If $r_* \simeq 1 {\rm Mpc}$ then $| Λ| < 10^{- 114}$ and, if $r_* \simeq 10^{28} {\rm cm}$ then $| Λ| < 10^{- 122}$ in natural units.

hep-th↗

arXiv1994

Inconsistent Physics in the Presence of Time Machines

We present a scenario in $1 + 1$ and $3 + 1$ dimensional space time which is paradoxical in the presence of a time machine. We show that the paradox cannot be resolved and the scenario has {\em no} consistent classical solution. Since the system is macroscopic, quantisation is unlikely to resolve the paradox. Moreover, in the absence of a consistent classical solution to a macroscopic system, it is not obvious how to carry out the path integral quantisation. Ruling out, by fiat, the troublesome initial conditions will resolve the paradox, by not giving rise to it in the first place. However this implies that time machines have an influence on events, extending indefinitely into the past, and also tachyonic communication between physical events in an era when no time machine existed. If no resolution to the paradox can be found, the logical conclusion is that time machines of a certain, probably large, class cannot exist in $3 + 1$ and $1 + 1$ dimensional space time, maintaining the consistency of known physical laws.

gr-qc↗

arXiv1994

Cosmological Constant in Low Energy $d = 4$ String Leads to Naked Singularity

In the sigma model approach, the $β$-function equations for non critical strings contain a term which acts like a tree level cosmological constant, $Λ$. We analyse the static, spherically symmetric solutions to these equations in $d = 4$ space time and show that the curvature scalar seen by the strings is singular if $Λ\ne 0$. This singularity is naked. Requiring its absence in our universe imposes the constraint $| Λ| < 10^{- 120}$ in natural units. {}From another point of view, our analysis implies that low energy $d = 4$ non critical strings lead to naked singularities.

hep-th↗

arXiv1993

Scenario for Seeding a Singularity in $d = 2$ String Black Hole with Tachyon

The $d = 2$ string admits a black hole solution and also a singular solution when tachyon back reaction is included. It is of importance to know if the former solution can evolve into a later one. An explicit solution describing this process is difficult to obtain. We present here a scenario in which such an evolution is very likely to occur. In essence, it takes place when a derivative discontinuity is seeded in the dilaton field by an incident tachyon pulse. An application of this scenario to $1 + 1$ dimensional toy models suggests that a black hole can evolve into a massive remnant, strengthening its candidacy for the end state of a black hole.

hep-th↗

arXiv1993

Symplectic Manifolds, Coherent States and Semiclassical Approximation

We describe the symplectic structure and Hamiltonian dynamics for a class of Grassmannian manifolds. Using the two dimensional sphere ($S^2$) and disc ($D^2$) as illustrative cases, we write their path integral representations using coherent state techniques. These path integrals can be evaluated exactly by semiclassical methods, thus providing examples of localisation formula. Along the way, we also give a local coordinate description for a class of Grassmannians.

hep-th↗

arXiv1993

Singularities in Low Energy $d = 4$ Heterotic String and Brans-Dicke Theories

We present the static, spherically symmetric solutions of the low energy $d = 4$ string. They form a simple generalisation of the Schwarzschild solution and describe the gravitational field of a spherical star in perturbative string theory. If the Robertson parameter $γ$ is different from one, these solutions describe singular objects with naked singularities at their horizons, and whose Hawking temperature is infinite. These objects might represent ``massive remnants'', the end states of black holes. Our analysis also implies that Brans-Dicke theory has a naked singularity. Invoking cosmic censorship conjecture will rule out Brans-Dicke theory.

hep-th↗

arXiv1993

Tachyon Back Reaction on $d = 2$ String Black Hole

We describe a static solution for $d = 2$ critical string theory including the tachyon $T$ but with its potential $V (T)$ set to zero. This solution thus incorporates tachyon back reaction and, when $T = 0$, reduces to the black hole solution. When $T \neq 0$ we find that (1) the Schwarzschild horizon of the above black hole splits into two, resembling Reissner-Nordstrom horizons and (2) the curvature scalar develops new singularities at the horizons. We show that these features will persist even when $V (T)$ is nonzero. We present a time dependent extension of our static solution and discuss some possible methods for removing the above singularities.

hep-th↗

arXiv1993

Comments on Witten Invariants of 3-Manifolds for SU(2) and $Z_m$

The values of the Witten invariants, $I_W$, of the lens space $L(p, 1)$ for SU(2) at level $k$ are obtained for arbitrary $p$. A duality relation for $I_W$ when $p$ and $k$ are interchanged, valid for asymptotic $k$, is observed. A method for calculating $I_W$ for any group $G$ is described. It is found that $I_W$ for $Z_m$, even for $m = 2$, distinguishes 3-manifolds quite effectively.

hep-th↗

arXiv1993

Tachyon Splits the (d = 2 String) Black Hole Horizon and Turns it Singular

We present a static solution for $d = 2$ critical string theory including the tachyon $T$ but not its potential $V(T)$. This solution thus incorporates tachyon back reaction and, when $T = 0$, reduces to the black hole solution. When $T \neq 0$ one finds that (1) the Schwarzschild horizon of the above black hole splits into two, resembling Reissner-Nordstrom horizons and (2) the curvature scalar develops new singularities at the horizons. These features, as we argue, will persist even with $V(T)$ present. Some possible methods for removing these singularities are discussed.

hep-th↗

arXiv1992

Renormalization of Couplings in Embedded Random Surfaces

We study the dressing of operators and flows of corresponding couplings in models of {\it embedded} random surfaces. We show that these dressings can be obtained by applying the methods of David and Distler and Kawai. We consider two extreme limits. In the first limit the string tension is large and the dynamics is dominated by the Nambu-Goto term. We analyze this theory around a classical solution in the situation where the length scale of the solution is large compared to the length scale set by the string tension. Couplings get dressed by the liouville mode (which is now a composite field) in a non-trivial fashion. However this does {\it not} imply that the excitations around a physical ``long string" have a phase space corresponding to an extra dimension. In the second limit the string tension is small and the dynamics is governed by the extrinsic curvature term. We show, perturbatively, that in this theory the relationship between the induced metric and the worldsheet metric is ``renormalized", while the extrinsic curvature term receives a non-trivial dressing as well. This has the consequence that in a generic situation the dependence of couplings on the physical scale is different from that predicted by their beta functions.

hep-th↗

arXiv1991

Three Manifolds and Graph Invariants

We show how the Turaev--Viro invariant can be understood within the framework of Chern--Simons theory with gauge group SU(2). We also describe a new invariant for certain class of graphs by interpreting the triangulation of a manifold as a graph consisiting of crossings and vertices with three lines. We further show, for $S^3$ and $RP^3$, that the Turaev-Viro invariant is the square of the absolute value of their respective partition functions in SU(2) Chern--Simons theory and give a method of evaluating the later in a closed form for lens spaces $L_{p,1}$.

hep-th↗

arXiv1991

New Special Operators in $W$-Gravity Theories

We find new special physical operators of $W_3 -$gravity having non trivial ghost sectors. Some of these operators may be viewed as the liouville dressings of the energy operator of the Ising model coupled to {\it 2d~gravity} and this fills in a gap in the connection between pure $W_3 -$gravity and Ising model coupled to 2d gravity found in our previous work. We formulate a selection rule required for the calculation of correlators in $W -$gravity theories. Using this rule, we construct the non ghost part of the new operators of $W_N -$gravity and find that they represent the $(N , N+1)$ minimal model operators from both inside and outside the minimal table. Along the way we obtain the canonical spectrum of $W_N -$gravity for all $N$ .

hep-th↗