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| Equilibrium Abundances in the |
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| Early
Universe |
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| • | To find total
energy density, add all |
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| these up
(includes photons, baryons): |
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| • | When
particles are no longer relativistic, |
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| and abundances
still maintained by |
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| particle
interactions, non-relativistic |
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| limit of eq.
10.1 gives equilibrium N: |
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| – | (No longer
adding to inertial mass density) |
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