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Nov 24
2009
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As the Universe cools a weak asymmetry in the direction towards
matter becomes evident. Matter that is massive is unstable,
particularly at the high temperature in the early Universe. Low mass
matter is stable, but susceptible to destruction by high 
energy
radiation ( photons).
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As the volume of the Universe increases, the lifetime of stable matter (its time between collisions with photons) increases. This also means that the time available for matter to interact with matter also increases. |
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The Universe evolves from a pure, energy dominated domain to a more disordered, matter dominated domain, i.e. entropy marches on. |
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The last two stages of matter construction is the combining of three
quark groups into baryons (protons and neutrons), then the collection of
electrons by proton/neutron atomic nuclei to form atoms. The
construction of baryons is called baryongenesis.
Baryongenesis begins around 1 second after the Big Bang. The equilibrium
process at work is the balance between the strong |
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As all the anti-particles annihilate by colliding with their matter counterparts leaving the remaining particles in the Universe to be photons, electrons, protons and neutrons. All quark pairs have reformed into baryons (protons and neutrons). Today, only around exotic objects like black holes, do we find any anti-matter, anti-mesons (quark pairs) or any of the other strange matter that was once found throughout the early Universe. |
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