Special thread for answers to Mathbrain's questions

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SUMMARY

This discussion centers on Mathbrain's inquiries regarding the movement of galaxy clusters and the nature of cosmic microwave background (CMB) radiation. Mathbrain questions whether the distance between two galaxy clusters can be predicted given their perpendicular movement and how CMB photons, originating from the Big Bang, can be detected from all directions. The responses clarify that the expansion of space is related to the Hubble constant and that the CMB is uniformly present due to the universe's expansion, with light traveling through curved space. The conversation emphasizes the importance of understanding the Einstein Field Equations and the Friedmann equations in cosmology.

PREREQUISITES
  • Understanding of Einstein Field Equations (EFE)
  • Familiarity with Friedmann equations in cosmology
  • Knowledge of cosmic microwave background (CMB) radiation
  • Basic principles of differential geometry
NEXT STEPS
  • Study the Einstein Field Equations and their implications in cosmology
  • Learn about the Friedmann equations and their role in understanding cosmic expansion
  • Research the nature and significance of cosmic microwave background radiation
  • Explore differential geometry and its applications in representing curvature in space
USEFUL FOR

Astronomers, cosmologists, physics students, and anyone interested in understanding the dynamics of the universe and the mathematical models that describe cosmic phenomena.

  • #31
marcus said:
That's a pretty nice implementation of the standard cosmology model! You could say that it is better than both of the ones I've been using because it combines good features of the Morgan one and the Wright one.

Thanks Marcus. My motivation has been to include a variable for Omega_radiation, which none of the then cosmo-calculators had. Hellfire offered me his source code and the freedom to modify it, so I've added Omega_r and a few outputs.

For the usual ranges of z < 100 or so, Omega_r makes virtually no difference, but it becomes noticeable around z > 1000, where Omega_r_then makes up around 25% of Omega. It is primarily of interest for looking at the sensitivity of the standard model to radiation density. It's also nice to verify or demonstrate radiation dominance at z > ~3300.
 
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  • #32
Hey thanks for your help guys! It's been really fascinating to find out that there are special metrics for cosmological objects. This has really given me a greater appreciation for abstact algebras and geometries. I really feel like I have a better understanding of cosmology now.

Thank you SO MUCH!
 

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