Equilibrium at Universe (possible?)

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    Equilibrium Universe
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SUMMARY

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.

PREREQUISITES
  • Friedmann-Robertson-Walker (FRW) metric
  • Thermal energy distribution concepts
  • Understanding of local thermal equilibrium
  • Cosmological expansion dynamics
NEXT STEPS
  • Study the implications of the Friedmann-Robertson-Walker (FRW) metric in cosmology
  • Research local thermal equilibrium in expanding systems
  • Explore the slow expansion argument in cosmological contexts
  • Examine the relationship between thermal properties and cosmic expansion
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Cosmologists, theoretical physicists, and students of astrophysics seeking to deepen their understanding of the universe's thermal dynamics and expansion behavior.

ChrisVer
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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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How can you write an ordered post if the universe is at equilibrium?

Do you mean the large-scale homogeneity instead of equilibrium?
 
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:
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..
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:
I am looking for a better explanation on the slow expansion-argument as well..

Sorry to necropost but I'm just running across this thread. The slow expansion argument is that, in the early universe, the time scale for local heat exchange, which is what drives the system to local thermal equilibrium, was much shorter than the time scale of expansion; in other words, on the time scale for achieving local thermal equilibrium, the universe could be approximated as not expanding. Of course over longer time scales, the expansion does affect the thermal properties, because it causes the universe to cool; but as long as the thermalization time scale is much shorter than the expansion time scale, the cooling can be thought of as just a succession of local thermal equilibrium states at gradually decreasing temperature, because local heat exchange happens fast enough to keep adjusting to the expansion.
 

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