Summary
With the rules for the development of density perturbations under gravity in the expanding Universe established, we need more tools to enable the models to be confronted with observation. We first need the concept of the horizon scales which are present in expanding world models and their physical significance. These are developed for the critical world model, Ω0 = 1, ΩΛ = 0 and then for the preferred reference model Ω0 = 0.3, ΩΛ = 0.7. This leads to the issues of dealing with perturbations on super-horizon scales. With these tools in place, two early models of the formation of structure are reviewed, the baryonic adiabatic and isothermal models of structure formation, based upon the assumption that the Universe is composed of only baryonic matter and radiation. Dissipative processes are included in the physical realisation of models of structure formation. It is shown that neither of these models can account for the observations, particularly the limits imposed in the early 1980s on the amplitude of temperature fluctuations in the CMB. Something was seriously missing—more than simply baryons are needed to account for the observations.
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Notes
- 1.
Many of the most important papers by Zeldovich and his colleagues are contained in Volume 2 of Zeldovich’s selected works (Zeldovich, 1993).
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Longair, M.S. (2023). More Tools and Problems. In: Galaxy Formation. Astronomy and Astrophysics Library. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-662-65891-8_12
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