The analytic part of the stress-energy tensor at thermodynamic equilibrium has a universal covariant form independent of specific curved spacetime geometry for the massless scalar field, argued to hold for any quantum field theory.
Kubo formulas for thermodynamic transport coefficients
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abstract
Uncharged relativistic fluids in 3+1 dimensions have three independent thermodynamic transport coefficients at second order in the derivative expansion. Fluids with a single global $U(1)$ current have nine, out of which seven are parity preserving. We derive the Kubo formulas for all nine thermodynamic transport coefficients in terms of equilibrium correlation functions of the energy-momentum tensor and the current. All parity-preserving coefficients can be expressed in terms of two-point functions in flat space without external sources, while the parity-violating coefficients require three-point functions. We use the Kubo formulas to compute the thermodynamic coefficients in several examples of free field theories.
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Carroll hydrodynamics with spin is obtained as the c→0 limit of relativistic hydrodynamics with spin, extending the description of boost-invariant flows.
Ricci cosmology adds curvature-matter coupling terms to the stress-energy tensor, enabling analytic inflationary solutions in standard flat FLRW cosmology without Lambda or new scalar fields.
citing papers explorer
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Universal analytic dependence of the stress-energy tensor at thermodynamic equilibrium in curved space-time
The analytic part of the stress-energy tensor at thermodynamic equilibrium has a universal covariant form independent of specific curved spacetime geometry for the massless scalar field, argued to hold for any quantum field theory.
-
Carroll hydrodynamics with spin
Carroll hydrodynamics with spin is obtained as the c→0 limit of relativistic hydrodynamics with spin, extending the description of boost-invariant flows.
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Ricci cosmology
Ricci cosmology adds curvature-matter coupling terms to the stress-energy tensor, enabling analytic inflationary solutions in standard flat FLRW cosmology without Lambda or new scalar fields.