Whatever the "frozen star" interpretation of black holes is supposed to be.Cosmic inflation appears to solve several problems, lpetrich. But as you know singlularities are mentioned in the context of black holes and the Big Bang. Once you understand the "frozen star" black hole interpretation then flip it around, the flatness problem and the horizon problem go away.
There is indeed an analogy between gravitational collapse and the Big Bang, but for gravitational collapse, the singularity is in the future, while in the Big Bang, the singularity is in the past. However, the mechanics are somewhat different. The Universe does not seem to have a surface, as a gravitationally-collapsing star does.
As to the flatness problem, let's see how the various constituents of the Universe behave. Let's consider their densities as functions of the Universe size parameter a.
Wavelength ~ a
Temperature ~ 1/a
I'll set c = 1 as is usual in the professional literature.
For an equation of state with (pressure) = w * (density),
(density) ~ a[sup]-3(1+w)[/sup]
Radiation (gas of particles moving at v = c): w = 1/3, (density) ~ a[sup]-4[/sup]
Dust (gas of particles moving at v = 0): w = 0, (density) ~ a[sup]-3[/sup]
Curvature: w = -1/3, (density) ~ a[sup]-2[/sup]
Cosmological constant: w = -1, (density) ~ constant
Let's see how the curvature behaves. I'll ignore dark energy and assume that the Universe is dust all the way back to the matter/radiation crossover at a ~ 1/3000 * present.
Present day:
Size factor = 1
Temperature = 3 K or 3*10[sup]-4[/sup] eV
Curvature/density = Less than few percent, but I'll use 1 for convenience, for matter/curvature crossover
Matter dominated; I'll ignore dark energy
Matter/radiation crossover
Size factor = 3*10[sup]-4[/sup]
Temperature = 10[sup]4[/sup] K or 1 eV
Curvature/density = 3*10[sup]-4[/sup]
Radiation dominated
Planck: quantum gravity
Temperature = 10[sup]19[/sup] GeV or 10[sup]28[/sup] eV
Size factor = 3*10[sup]-32[/sup]
Curvature/density = 3*10[sup]-60[/sup]
So one gets extreme fine tuning.
However, inflation solves that problem nicely, because curvature/density behaves as a[sup]-2[/sup] during it, instead of as a (dust) or a[sup]2[/sup] (radiation). It flattened out the Universe.
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Now the horizon problem. For that, let us consider the light cone from a point.
Comoving coordinate x = integral dt/a
The event horizon is thus at x = (typical time)/a
The Hubble parameter H is essentially 1/(typical time)
Since time ~ 1/sqrt(G*density),
we get a ~ t[sup]2/(3(1+w))[/sup],
and x ~ t[sup](1+3w)/(3(1+w))[/sup]
Thus, x ~ t[sup]1/3[/sup] for dust and t[sup]1/2[/sup] for radiation. In both cases, the event horizon expands with time, thus producing the horizon problem.
But for inflation, x ~ 1/(H*a) where H is constant. Since a increases, x decreases, thus solving the horizon problem. In fact, a = a0*e[sup]H*t[/sup].
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I hope that this math has not been too difficult to follow.