English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

The analysis of WMAP and Planck CMB data has shown the presence oftemperature asymmetries towards the halos of several galaxies, which isprobably due to the rotation of clouds present in these halos about therotational axis of the galaxies. It had been proposed that these are hydrogenclouds that {\it should} be in equilibrium with the CMB. However, standardtheory did not allow equilibrium of such clouds at the very low CMBtemperature, but it was recently shown that the equilibrium {\it could} bestable. This still does not prove that the cloud concentration and that theobserved temperature asymmetry is due to clouds in equilibrium with the CMB. Toinvestigate the matter further, it would be necessary to trace the evolution ofsuch clouds, which we call "virial clouds", from their formation epoch to thepresent, so as to confront the model with the observational data. The task isto be done in two steps: (1) from the cloud formation before the formation offirst generation of stars; (2) from that time to the present. In this paper wedeal with the first step leaving the second one to a subsequent analysis.

Evolution of virial clouds-I: from surface of last scattering up to the formation of population-III stars