Method to compute the stress-energy tensor for the massless spin<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mfrac><mml:mrow><mml:mn>1</mml:mn></mml:mrow><mml:mrow><mml:mn>2</mml:mn></mml:mrow></mml:mfrac></mml:math>field in a general static spherically symmetric spacetime

Recently, a novel kind of scalar wigs around Schwarzschild black holes-scalar dynamical resonance states were introduced in [Phys. Rev. D 84, 083008 (2011)] and [Phys. Rev. Lett. 109, 081102 (2012)]. In this paper, we investigate the existence and evolution of Dirac dynamical resonance states. First we look for stationary resonance states of a Dirac field around a Schwarzchild black hole by using the Schrödinger-like equations reduced from the Dirac equation in Schwarzschild spacetime. Then Dirac pseudo-stationary configurations are constructed from the stationary resonance states. We use these configurations as initial data and investigate their numerical evolutions and energy decay. These dynamical solutions are the so-called "Dirac dynamical resonance states".It is found that the energy of the Dirac dynamical resonance states shows an exponential decay.The decay rate of energy is affected by the resonant frequency, the mass of Dirac field, the total angular momentum, and the spin-orbit interaction. In particular, for ultra-light Dirac field, the corresponding particles can stay around a Schwarzschild black hole for a very long time, even for cosmological time-scales.

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“…This coordinate system is suitable in the exterior region r ∈ (2M, ∞). In addition, we choose the following vierbein for convenience [30,49]:…”

Section: Dirac Equation In Schwarzschild Spacetimementioning

confidence: 99%

Dirac dynamical resonance states around Schwarzschild black holes

2014

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“…In the Schwarzschild geometry we have good understanding of the stress-energy tensor of the quantized massive and massless fields in the Boulware, Unruh and Hartle-Hawking states. Specifically, due to excellent numerical work we have results that may be considered as exact [1,2,3,4,5,6,7,8]. On the other hand, analytical [9,10,11,12] and semi-analytical [13,14,15,16,17,18] approximations have been constructed and successfully applied in numerous physically interesting cases.…”

Section: Introductionmentioning

confidence: 99%

Entropy of quantum-corrected black holes

Matyjasek¹

2006

Phys. Rev. D

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The approximate renormalized one-loop effective action of the quantized massive scalar, spinor and vector field in a large mass limit, i.e., the lowest order of the DeWitt-Schwinger expansion involves the coincidence limit of the Hadamard-DeWitt coefficient a3. Building on this and using Wald's approach we shall construct the general expression describing entropy of the sphericallysymmetric static black hole being the solution of the semi-classical field equations. For the concrete case of the quantum-corrected Reissner-Nordström black hole this result coincides, as expected, with the entropy obtained by integration of the first law of black hole thermodynamics with a suitable choice of the integration constant. The case of the extremal quantum corrected black hole is briefly considered.

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“…The bi-vector and bi-spinor of parallel transport are introduced into the above expression so that the Feynman propagator and its derivatives are correctly evaluated at x [13]. The definition (20) differs from the canonical expression by a term proportional to g λ ν L , where L is the Dirac Lagrangian.…”

Section: Hadamard Renormalizationmentioning

confidence: 99%

Dirac fermions on an anti-de Sitter background

Ambruş¹,

Winstanley²

2014

AIP Conference Proceedings

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Abstract. Using an exact expression for the bi-spinor of parallel transport, we construct the Feynman propagator for Dirac fermions in the vacuum state on anti-de Sitter space-time. We compute the vacuum expectation value of the stress-energy tensor by removing coincidence-limit divergences using the Hadamard method. We then use the vacuum Feynman propagator to compute thermal expectation values at finite temperature. We end with a discussion of rigidly rotating thermal states.

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

Cited by 40 publications

References 64 publications

Dirac dynamical resonance states around Schwarzschild black holes

Dirac dynamical resonance states around Schwarzschild black holes

Entropy of quantum-corrected black holes

Dirac fermions on an anti-de Sitter background

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