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User:Maschen/Thermodynamics in curved spacetime

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In general relativistic physics, and it's numerous applications to astrophysics, thermodynamics in curved spacetime is the mathematical description of classical thermodynamics in curved spacetime.

Equilibrium thermodynamics

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Thermodynamic laws

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Each of the classical thermodynamic laws can be stated in a number of equivalent ways. The fundamental thermodynamic relation combines the first and second laws into one:

The second law can be also be stated as:

From a more fundamental and modern perspective, a more fundamental law of thermodynamics is baryon number conservation. To formulate this; denote the number density of baryons (number of baryons N per unit 3d volume V) by n in the rest frame, then the proper time derivative of total number is zero:

and the changes in volume are given as the four-divergence of the four velocity u of the fluid:

Explicitly rewriting the divergence term leads to a simpler continuity equation:

where the baryon number flux vector is:

The relativistic generalization of eqn (X) is:

where the equality holds for thermal equilibrium only, the inequality is strict for non-equilibrium.

Non-equilibrium thermodynamics

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Relativistic heat conduction

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See also

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References

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Notes

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  • C.W. Misner, K.S. Thorne, J.A. Wheeler. Gravitation. p. 1146. ISBN 0-7167-0344-0.{{cite book}}: CS1 maint: multiple names: authors list (link)
  • H.E. Camblong (2005). [repository.usfca.edu/cgi/viewcontent.cgi?article=1020&context=phys "Semiclassical Methods in Curved Spacetime andBlack Hole Thermodynamics"]. {{cite news}}: Check |url= value (help) [1]

For AM in GR:

Further reading

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References

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