Understanding Astrophysics: The Hubble Distance and Beyond

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SUMMARY

The discussion centers on the Hubble distance and its implications in astrophysics, particularly regarding the expansion of the universe. Participants clarify that objects beyond the Hubble sphere can emit light that may eventually reach us as the Hubble distance increases over time. The conversation also touches on the concepts of particle and event horizons, with references to the Friedmann-Robertson-Walker metric and the role of the cosmological constant in current cosmological models. Key insights include the distinction between superluminal expansion during inflation and the ongoing expansion of the universe, as well as the implications for observing distant galaxies.

PREREQUISITES
  • Understanding of Hubble's Law and the Hubble Sphere
  • Familiarity with General Relativity and cosmological models
  • Knowledge of the Friedmann-Robertson-Walker metric
  • Concept of particle and event horizons in cosmology
NEXT STEPS
  • Research the Friedmann equations and their implications for cosmic expansion
  • Study the role of the cosmological constant in modern cosmology
  • Explore the Horizon Problem and its significance in General Relativity
  • Learn about the differences between particle and event horizons in expanding universes
USEFUL FOR

Astronomers, astrophysicists, and students of cosmology seeking to deepen their understanding of cosmic expansion and the implications of the Hubble distance on observational astronomy.

  • #31
pervect said:
Very interesting, I must admit - thanks for the explanation. I don't suppose SCC can explain the galactic rotation curves / dark matter problem any better than GR can (or can it?).
No, not yet - its a problem that has been discussed on the GA&C forum.

In SCC there is no need for DE and the total matter density is 22% closure. However SCC BBN requires ~20% baryonic closure density to obtain the correct amount of helium. In other words there is no need for exotic non-baryonic DM either.
However the question that leaves is where is all this baryonic matter?
There is no clear answer to this and as such there is just as much a problem with SCC as there is in GR, which leaves the non-baryonic DM unidentified.
One leading contender though is that the majority of the DM in SCC could be in the form of IMBHs of about 102 - 103 solar masses. These would have formed as the end product of PopIII stars of about the same mass range. A few SMBHs would also form that could become proto-galactic nuclei, some of the IMBHs would be gravitationally bound to them and attract uncondensed gas that formed ordinary stars, planets and ISM. The presence of many PopIII stars going SN at an early stage would ionise the IGM and provide early metallicity. The primordial hydrogen and helium is also seeded with relatively high metallicity in freely coasting BBN and that allows PopIII stars of that mass range to form - metallicity is necessary to radiate the heat away.
Well that's my 'hand waving' scenario! Shoot it down if you want!

Garth
 

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