Black hole kinematics: The “in”-vacuum energy density and flux for different observers
Apr 2, 20149 pages
Published in:
- Phys.Rev.D 90 (2014) 2, 024011
- Published: Jul 3, 2014
e-Print:
- 1404.0684 [gr-qc]
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Abstract: (APS)
We have investigated the local invariant scalar observables—energy density and flux—which explicitly depend on the kinematics of the concerned observers in the thin null shell gravitational collapse geometry. The use of globally defined null coordinates allows for the definition of a unique in-vacuum for the scalar field propagating in this background. Computing the stress-energy tensor for this scalar field, we work out the energy density and flux for the static observers outside the horizon and then consider the radially in-falling observers who fall in from some specified initial radius all the way through the horizon and inside to the eventual singularity. Our results confirm the thermal Tolman-shifted energy density and fluxes for the static observers which diverge at the horizon. For the in-falling observer starting from far off, both the quantities—energy density and flux—at the horizon crossing are regular and finite. For example, the flux at the horizon for the in-falling observer from infinity is approximately 24 times the flux for the observer at infinity. Compared with the static observers in the near-horizon region, this is quite small. Both the quantities grow as the in-fall progresses inside the horizon and diverge at the singularity.Note:
- Matches published version. 8 pages, 6 figures
- 04.62.+v
- 04.70.Dy
- energy: density
- field theory: scalar
- horizon: crossing
- gravitation: collapse
- tensor: energy-momentum
- kinematics
- black hole
- Vaidya
References(12)
Figures(17)
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