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karlzr
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Kolb&Turner in "the early universe" mentioned that for a scalar field ##\phi## at finite temperature, ##p=-V_T(\phi)## and ##\rho=-p+T\frac{d p(T)}{d T}## where ##V_T## is potential energy including temperature correction. My question is: when we consider the evolution of the universe using Friedman's equation, should we use this kind of definition of ##\rho## and ##p## or we stick to those obtained from stress energy tensor? I would say the latter since that's what we can get from Einstein's equation. But then I don't understand what are Kolb&Turner's ##\rho## and ##p##. Why doesn't kinetic term contribute to them?
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