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For the time being, mainly what we have is just Liddle, Ch. 11: The Early Universe.

Plus some supplements/complements.

1. Liddle, Ch. 11: The Early Universe:
1. In fact, this chapter is almost all only about the temperature of the early universe from about the recombination era t = 377,770(3200) y = 1.192*10**13 s (formally the decoupling era which occurs during the recombination era: see Wikipedia: Λ CDM model: Parameters to t = 10**(-10) which is beginning of the quark era.
2. z_rec = 1089.90(23) (formally for the decoupling era. Recall
```           (a_0/a)=z+1 and so at z_rec ≅ 1100, a/a_0 ≅ 1/1100.
```
3. Before recombination radiation and matter had the same temperature. This temperature scales T = T_rec(a_rec/a) just like radiation alone. This is because radiation is the dominant thermal energy. Matter dominates the mass-energy, but most of this thermally inert rest mass.
4. Note
```
(Ω_r/Ω_m) ≅ (a_e/a) = (t_e/t)**(2/3)

(Ω_r/Ω_m)_rec ≅ (a_e/a_rec) = (t_e/t_rec)**(2/3) = (1/8)**(2/3) = 1/4

```
So at the recombination era radiation is ∼ 1/4 of matter in mass-energy. However,
```           E_rad = a*T**4 = a*4000**4 = [(7.56573345 ...)*10**(-23)]*256*10**12 = 2.5*10**(-8) J/m**3

E_matter_thermal ≅ (3/2)*nkT = (3/2)*(5*10**8)*(1.380649*10**(-23) J/K)*4000
= 10**(-14)*4000 J/m**3
= 4*10**(-11) J/m**3
```
(see Wikipedia: Chronology of the universe: Tabular summary; Wikipedia: Ideal gas law, Wikipedia: Ideal gas law: Energy associated with a gas, Boltzmann contant k = 1.380649*10**(-23) J/K = (8.617333262 ... )*10**(-5) eV/K (exact) ≅ 10**(-4) eV/K ≅ 10**(-10) MeV/K; Wikipedia: blackbody spectrum, radiation density constant a=(4σ/c) = (7.56573345 ... )*10**(-15) J/*m**3/K**4 (exact)).

So it seems that radiation energy must overwhelingly dominate the thermal energy at recombination. The matter thermal energy can only be a perturbation.

2. Radiation-Matter era of the universe figure: For exxact solution and approximate solutions: see Universe in problems:Solutions of Friedman equations in the Big Bang model: Problem 5, but note they do NOT explicitly evaluate the integral which can be done:
```        a_e=(omega_r_0_p/omega_m_0_p)*a_0_cosmic   ! Radiation era end a(t).
omega_e=omega_r_0_p*(a_0_cosmic/a_e)**power_r
Ω_e = omega_e
t_e = (4/3)(sqrt(2)-1)/[H_0*sqrt(2Ω_e)]

sqrt(Ω_r_0)*H_0*t
=c1*x*(1+c0*x)**(1/2)+c2*((1+c0*x)**(3/2)+c3
where c0=omega_m_0_p/omega_r_0_p
c1=2/c0
c2=-(4/3)/c0**2
c3=-c2
x=a/a_0

sqrt(Ω_r_0)*H_0*t for x << 1 which is needed for a < ∼ 10**(-8) for numerical accuracy
=(1/2)*x**2-(1/6)*c0*x**3

```
3. Early universe cosmic temperature figure. Note the Boltzmann contant k = 1.380649*10**(-23) J/K = (8.617333262 ... )*10**(-5) eV/K (exact) ≅ 10**(-4) eV/K ≅ 10**(-10) MeV/K implies that 1 mega-electron-volt (MeV) corresponds to about 10**(10) K.
4. Wikipedia: Chronology of the universe: Tabular summary:
5. Wikipedia: Graphical timeline from Big Bang to Heat Death but note that the left-hand vertical scale is tricky, for greater than about > 0, it is x=100*log(log(t_year)) and so t_year=10**(10**(x/100)))
6. Wikipedia: Graphical timeline of the Big Bang: Redundant to the timeline above.
7. ** | Evidence of Neutrino Enhanced Clustering in a Complete Sample of Sloan Survey Clusters, Implying ∑ m_ν = 0.11(3) eV.: KATRIN: neutrino mass experiment (sensitivity range ∼ 0.2--2 eV): out of luck.
8. * | The eras of radiation, matter, and dark energy: new information from the Planck Collaboration: Kevin Cahill, arXiv, 2016, June 22, 13 pages: Research: On cosmic scale factor and the cosmic energy eras based on the Planck 2015: Planck 2015 results. XIII. Cosmological parameters.
---Keywords: cold dark matter (CDM), concordance model, concordance model distance measures, cosmic energy eras (radiation era, matter era, dark-energy era) cosmic scale factor, cosmological redshift, cosmology, dark energy, dark matter, disk galaxies, expansion of the universe, IOP cosmological parameters summary: bit dated, Universe in Problems: lots of solutions, etc.
9. Keywords: Big Bang, Big Bang nucleosynthesis, big bang singularity, cosmic energy eras (radiation era, matter era, dark-energy era) early universe, IOP cosmological parameters summary: bit dated, Universe in Problems: lots of solutions.