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How can Universe be at equilibrium when the FRW metric has no time-like Killing Vector?Request: Please, move this into Cosmology thread... :( Mistakenly I posted it in HEP
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The discussion centers on the concept of equilibrium in the universe, specifically addressing the implications of the Friedmann-Robertson-Walker (FRW) metric lacking a time-like Killing vector. Participants clarify that the term "equilibrium" refers to a thermal energy distribution rather than a static state. The slow expansion argument is highlighted, indicating that during the early universe, local heat exchange occurred rapidly enough to maintain local thermal equilibrium despite the ongoing expansion. This understanding is crucial for interpreting the universe's thermal properties over time.
PREREQUISITESCosmologists, theoretical physicists, and students of astrophysics seeking to deepen their understanding of the universe's thermal dynamics and expansion behavior.
It's not an equilibrium in the strict sense of a final state of a system that no longer changes. What it essentially means is that the system is well-described by a thermal energy distribution.ChrisVer said:http://www.damtp.cam.ac.uk/user/db275/Cosmology/Chapter3.pdf
page:5 as you scroll down, the subnote with number 7...
I am trying to pursue a little further and understanding better what they meant in it... In fact I am looking for a better explanation on the slow expansion-argument as well..
ChrisVer said:I am looking for a better explanation on the slow expansion-argument as well..