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The Standard Model can incorporate baryogenesis, though the amount of net baryons (and leptons) thus created may not be sufficient to account for the present baryon asymmetry. There is a required one excess quark per billion quark-antiquark pairs in the early universe in order to provide all the observed matter in the universe. [3]
English: JWST early Universe observations and ΛCDM cosmology. Deep space observations of the JWST have revealed that the structure and masses of very early Universe galaxies at high redshifts (z ∼ 15), existing at ∼0.3 Gyr after the Big Bang, may be as evolved as the galaxies in existence for ∼ 10 Gyr.
The Affleck–Dine mechanism (AD mechanism) is a postulated mechanism for explaining baryogenesis during the primordial Universe immediately following the Big Bang. Thus, the AD mechanism may explain the asymmetry between matter and antimatter in the current Universe. It was proposed in 1985 by Ian Affleck and Michael Dine of Princeton ...
However, the Standard Model is known to violate the conservation of baryon number only non-perturbatively: a global U(1) anomaly. To account for baryon violation in baryogenesis, such events (including proton decay) can occur in Grand Unification Theories (GUTs) and supersymmetric (SUSY) models via hypothetical massive bosons such as the X boson.
A cosmological phase transition is an overall change in the state of matter across the whole universe. The success of the Big Bang model led researchers to conjecture possible cosmological phase transitions taking place in the very early universe, at a time when it was much hotter and denser than today. [1] [2]
Baryogenesis: 10 −5 s ~ 1 s: 10 12 K ~ 10 10 K (150 MeV ~ 1 MeV) Quarks are bound into hadrons. A slight matter-antimatter asymmetry from the earlier phases (baryon asymmetry) results in an elimination of anti-baryons. Until 0.1 s, muons and pions are in thermal equilibrium, and outnumber baryons by about 10:1. Close to the end of this epoch ...
Such non-conservation of baryon number is indeed assumed to have happened in the early universe, and is known as baryogenesis. However, in some theoretical models, it is suggested that leptogenesis also occurred prior to baryogenesis; thus the term leptogenesis is often used to imply the non-conservation of leptons without corresponding non ...
WMAP indicates (Figure 1) a smooth, homogeneous universe with density anisotropies of 10 parts per million. [4] However, there are large structures and density fluctuations in the present universe. Galaxies, for instance, are a million times more dense than the universe's mean density. [2]