On the massless scalar field in two space-time dimensions and the Thirring model

1979 ◽  
Vol 12 (1) ◽  
pp. 119-130 ◽  
Author(s):  
L K Hadjiivanov ◽  
S G Mikhov ◽  
D T Stoyanov
Keyword(s):  
Scalar Field ◽  
Space Time ◽  
Thirring Model ◽  
Massless Scalar ◽  
Massless Scalar Field

scholarly journals Self-force of a scalar charge in the space-time of extreme charged anti-dilatonic wormhole

2018 ◽  
Vol 15 (03) ◽  
pp. 1850050 ◽  
Author(s):  
A. A. Popov ◽  
O. Aslan
Keyword(s):  
Scalar Field ◽  
Space Time ◽  
The Self ◽  
Massless Scalar ◽  
Massless Scalar Field ◽  
Minimal Coupling ◽  
Scalar Charge ◽  
Self Force

The self-interaction for a static scalar charge in the space-time of extreme charged anti-dilatonic wormhole is calculated. We assume that the scalar charge is the source of massless scalar field with minimal coupling of the scalar field to the curvature of spacetime.

scholarly journals QUANTUM FLUCTUATIONS FOR A SCALAR FIELD IN THE SPACE–TIME OF GRAVITATIONAL IMPLUSIVE WAVE

1998 ◽  
Vol 13 (08) ◽  
pp. 1201-1211 ◽  
Author(s):  
Y. ENGINER ◽  
M. HORTAÇSU ◽  
N. ÖZDEMIR
Keyword(s):  
Scalar Field ◽  
Gravitational Waves ◽  
Quantum Fluctuations ◽  
De Sitter Space ◽  
Space Time ◽  
Massless Scalar ◽  
Massless Scalar Field ◽  
De Sitter

Quantum fluctuations for a massless scalar field in the background metric of spherical implusive gravitational waves propagating through Minkowski and de Sitter spaces are investigated. It is shown that there exist finite fluctuations for de Sitter space.

Rotational effects on the Casimir energy in the space–time with one extra compactified dimension

2018 ◽  
Vol 33 (20) ◽  
pp. 1850122 ◽  
Author(s):  
L. C. N. Santos ◽  
C. C. Barros
Keyword(s):  
Scalar Field ◽  
Angular Velocity ◽  
Physical Region ◽  
Casimir Energy ◽  
Space Time ◽  
Massless Scalar ◽  
Massless Scalar Field ◽  
Rotating Frame ◽  
Rotating System ◽  
Noninertial Effects

In this paper we study the quantization of a massless scalar field in a rotating frame. In particular, we obtain the Casimir energy in a space–time with one extra compactified dimension for a rotating observer. We consider a uniformly rotating system on the circle S1 and present an equation for spin-0 bosons where noninertial effects can be taken into account. It is shown that the spectrum of the scalar field depends on the angular velocity of the rotating system and in this way, positive and negative modes can be defined through an appropriate choice of the angular velocity. We show that noninertial effects restrict the physical region of the space–time where particles can be placed, and furthermore that the Casimir energy in the space–time with one extra compactified dimension is shifted by these effects. In addition, we pointed out that rotating effects modify the length of the extra dimension for a co-rotating observer in this kind of space–time.

scholarly journals ON THE EVOLUTION OF A MASSLESS SCALAR FIELD IN A SCHWARZSCHILD BACKGROUND: A NEW LOOK AT HAWKING RADIATION AND THE INFORMATION PARADOX

2004 ◽  
Vol 13 (08) ◽  
pp. 1595-1635 ◽  
Author(s):  
KIRILL MELNIKOV ◽  
MARVIN WEINSTEIN
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Hawking Radiation ◽  
Canonical Quantization ◽  
Space Time ◽  
Massless Scalar ◽  
Massless Scalar Field ◽  
Null Infinity ◽  
Information Paradox ◽  
Spacelike Hypersurfaces

We exhibit an explicit foliation of Schwarzschild space–time by spacelike hypersurfaces which extend from Schwarzschild r=0 to r=∞. This allows us to compute the values of a massless scalar field for all space–time points which lie in the future of the surface on which we initially quantize the theory. This is to be contrasted with approaches which start at past null infinity and propagate to future null infinity. One of its virtues is that this method allows us to discuss both asymptotic Hawking radiation and what is happening at finite distances from the black hole. In order to explain the techniques we use, we begin by discussing variants of the flat-space moving mirror9 problem. Then we discuss the canonical quantization of the massless scalar field theory and the geometric optics approximation which we use to solve the Heisenberg equations of motion in the black hole background. Using the example of an infalling mirror, an analogue of the moving mirror problem, we show that, although our spacelike slices extend to r=0, we can avoid discussing an initial state which extends through the horizon. Furthermore, we show that in the same way we avoid having to deal with the singularity at r=0 when we first quantize the system. This discussion naturally leads to a suggestion of how to handle the question of what is happening when the mirror hits the singularity. In the last section of the paper we discuss a discretization of the computation which behaves in the manner we suggest and yet exhibits Hawking radiation.5 This formulation of the problem allows us to discuss all the issues in an explicitly unitary setting. The resulting picture raises some interesting questions about the information paradox.

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