1. The stress-energy tensor of the quantized massive fields in the spacetime of the regular black hole in the asymtotically (Anti-)de Sitter universe

This code is an accompaniament to the paper Inside the degenerate horizons of the regular black holes. The stress-energy tensor can be constructed for the scalar (with arbitrary curvature coupling), spinor and vector fields. We provide Mathematica version of the code. The components of the tensor are stored here. A simple Mathematica notebook with basic informations. The coeffcients of the scalar, spinor and vector field.

${ds}^{2} = - {f(r) dt}^{2} + {h(r) dr}^{2} + r^{2} d Ω^{2}$

where

f(r) = \frac{1}{h(r)} = 1 - \frac{2M}{r} (1 - \tanh \frac{Q^{2}}{2Mr}) - ε \frac{Λ r^{2}}{3}

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2. The components of the stress-energy tensor in the Reissner-Nordstrom-(anti-)de Sitter geometry.

The components of the tensor are stored here
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3. Vacuum polarization, $< φ^{2} >$ , in spatially flat N-dimensional Friedman-Robertson-Walker spacetimes.

\begin{equation} ds^{2} = a^{2}(\eta)( d\eta^{2} + \delta_{ij} dx^{i} dx^{j}) \end{equation} \begin{equation} ds^{2} = -dt^{2} + a^{2}(t) \delta_{ij} dx^{i} dx^{j} \end{equation} For explanations see the paper Vacuum polarization ... and ReadMe,
tarred and gzipped Mathematica (*.m) files for

4 \leq N \leq 12

are stored here (conformal time) and here (proper time).
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4. (23 07 2022) The stress-energy tensor of the quantized massive fields in the geometries described by a general line element of the form

\begin{equation} ds^{2} = -fu,v) du dv + h(x,y) dx dy. \end{equation}
The results of the calculations will be presented here soon. Note, that the Minkowski, Nariai, anti-Nariai, Bertotti-Robinson and Plebanski-Hacyan solutions are the special cases of this line element with \begin{equation} f(u,v) = \frac{1}{(1-\frac{1}{2} \varepsilon_{1} a^{-2} uv)^{2}} \end{equation} and with \begin{equation} f(x,y) = \frac{1}{(1+\frac{1}{2} \varepsilon_{2} b^{-2} xy)^{2}} \end{equation}
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1. The stress-energy tensor of the quantized massive fields in the spacetime of the regular black hole in the asymtotically (Anti-)de Sitter universe

ds⁡ 2 = - f(r) dt⁡ 2 + h(r) dr⁡ 2 + r⁡ 2 d⁡ Ω 2

2. The components of the stress-energy tensor in the Reissner-Nordstrom-(anti-)de Sitter geometry.

3. Vacuum polarization, < φ 2 > , in spatially flat N-dimensional Friedman-Robertson-Walker spacetimes.

4. (23 07 2022) The stress-energy tensor of the quantized massive fields in the geometries described by a general line element of the form

${ds}^{2} = - {f(r) dt}^{2} + {h(r) dr}^{2} + r^{2} d Ω^{2}$

3. Vacuum polarization, $< φ^{2} >$ , in spatially flat N-dimensional Friedman-Robertson-Walker spacetimes.