Stress-energy tensor of neutral massive fields in Reissner-Nordström spacetime

Matyjasek, Jerzy

doi:10.1103/physrevd.61.124019

Cited by 59 publications

(78 citation statements)

References 29 publications

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“…This approximation has been derived for massive scalar fields in Schwarzschild spacetime [27][28][29][30], in a general static spherically symmetric spacetime [21,17], and in a general spacetime [31]. It has also been derived for massive spin 1 2 and 1 fields in Reissner-Nordström spacetimes [32]. The DeWitt-Schwinger approximation is independent of the state of the field.…”

Section: Introductionmentioning

confidence: 99%

Method to compute the stress-energy tensor for the massless spin12field in a general static spherically symmetric spacetime

2002

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A method for computing the stress-energy tensor for the quantized, massless, spin 1 2 field in a general static spherically symmetric spacetime is presented. The field can be in a zero temperature state or a non-zero temperature thermal state. An expression for the full renormalized stress-energy tensor is derived. It consists of a sum of two tensors both of which are conserved. One tensor is written in terms of the modes of the quantized field and has zero trace. In most cases it must be computed numerically. The other tensor does not explicitly depend on the modes and has a trace equal to the trace anomaly. It can be used as an analytic approximation for the stress-energy tensor and is equivalent to other approximations that have been made for the stress-energy tensor of the massless spin 1 2 field in static spherically symmetric spacetimes.

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Section: Introductionmentioning

confidence: 99%

Method to compute the stress-energy tensor for the massless spin12field in a general static spherically symmetric spacetime

2002

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“…General expressions for the first nonvanishing order of SET of the massive scalar, spinor, and vector fields, which generalize earlier results of Frolov and Zel'nikov for vacuum type-D geometries [9] , are constructed in [4] and [5]. They may be, in principle, used in any spacetime provided the temporal changes of the background are slow and the ratio of the by expanding the near-horizon geometry into a whole manifold.…”

Section: Manifoldsmentioning

confidence: 89%

“…Apart from this, such a kind of a metric appears in the limiting transition from nonextreme black holes to extreme ones [12], [13], [14]. SET for the BR spacetime was studied in [15], [4]. Now, however, we start not from the BR itself, but from its quantum-corrected version.…”

Section: Quantum-corrected Br-like Spacetimesmentioning

confidence: 99%

“…[4] and [8], below we collect the formulas that have been used in the backreaction calculations. For the quantized massive scalar field with an arbitrary curvature coupling one has…”

Section: Of Massive Fields In the Spacetime Of Extremal Reissner-nordmentioning

confidence: 99%

“…For massless fields, this task is extremely difficult. Meanwhile, for massive fields recent progress in deriving general expressions for SET [4], [5] makes the task tractable. As the calculation of SET is the key to the problem of existence of quantum-corrected EBH, let us dwell upon this issue in a more detail.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Quantum back reaction of massive fields and self-consistent semiclassical extreme black holes and acceleration horizons

Matyjasek¹,

Заславский²

2001

Phys. Rev. D

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We consider the effect of backreaction of quantized massive fields on the metric of extreme black holes (EBH). We find the analytical approximate expression for the stress-energy tensor for a scalar (with an arbitrary coupling), spinor and vector fields near an event horizon. We show that, independent of a concrete type of EBH, the energy measured by a freely falling observer is finite on the horizon, so that quantum backreaction is consistent with the existence of EBH. For the Reissner-Nordström EBH with a total mass M tot and charge Q we show that for all cases of physical interest M tot < Q . We also discuss different types of quantum-corrected Bertotti-Robinson spacetimes, find for them exact self-consistent solutions and consider situations in which tiny quantum corrections lead to the qualitative change of the classical geometry and topology. In all cases one should start not from a classical background with further adding quantum corrections but from the quantum-corrected self-consistent geometries from the very beginning.

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Stability of the effective potential of the gauge-less top-Higgs model in curved spacetime

Czerwińska

Lalak

Nakonieczny

2015

J. High Energ. Phys.

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We investigate stability of the Higgs effective potential in curved spacetime. To this end, we consider the gauge-less top-Higgs sector with an additional scalar field. Explicit form of the terms proportional to the squares of the Ricci scalar, the Ricci tensor and the Riemann tensor that arise at the one-loop level in the effective action has been determined. We have investigated the influence of these terms on the stability of the scalar effective potential. The result depends on background geometry. In general, the potential becomes modified both in the region of the electroweak minimum and in the region of large field strength.

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Stress-energy tensor of neutral massive fields in Reissner-Nordström spacetime

Cited by 59 publications

References 29 publications

Method to compute the stress-energy tensor for the massless spin12field in a general static spherically symmetric spacetime

Method to compute the stress-energy tensor for the massless spin12field in a general static spherically symmetric spacetime

Quantum back reaction of massive fields and self-consistent semiclassical extreme black holes and acceleration horizons

Stability of the effective potential of the gauge-less top-Higgs model in curved spacetime

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