Hawking radiation of massive fields in 2D

Abstract

We extend the classic results of the paper P. C. W. Davies, S. A. Fulling, and W. G. Unruh "Energy-momentum tensor near an evaporating black hole" by considering a massive scalar field in a two dimensions in the presence of a thin shell collapse. We show that outside the shell the WKB approximation is valid for any value of $r$ if $m{r}_g\gg 1$, where $m$ is the mass of the field, and $r_g$ is the Schwarzschild radius. Thus, we use semiclassical modes to calculate the flux in the vicinity of the shell, and at spatial infinity, $r\to +\infty$ at the final stage of the collapse, $t\to +\infty$ with the use of the covariant point-splitting regularization. We get that near the shell and at the spatial infinity the radiation is thermal with Hawking temperature. We obtain the negative flux $T_{vv}$ in the vicinity of the shell, which is similar to the classic result in the massless case.

23 pages, shorter version of the paper to appear in PRD, minor corrections, the title has been changed to meet requirements of the journal

References in corpus (1)

• Heating up an environment around black holes and inside de Sitter space

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