18-10.
We need some assumptions:
- flat universe
- Wm  ~ 0.3
- mass of galaxy Mg  ~ 1012Msun
- present horizon radius d  ~ 2/H0
Let M(t) = 4/3pd3(t) rm(t) be the mass contained within the horizon radius d. Using (18.47), the constancy of rma3 and the present value rm(t0) = Wmrcrit = 3WmH02/8p we find
| |  | dM dt
 
 | = 4prm(t) d2(t)        so at present | dM dt
 
 | ~ 6Wm  ~ 1.8. | 
 | 
The required time Dt is therefore
| | Dt = | Mg dM/dt
 
 | ~ | 1012 Msun×(1.5 km/Msun) 1.8 ×(3×105 km/s)
 
 | ~ 106 s  ~ 1 month. | 
 | 
18-20
 The Friedmann equation (18.77) becomes (with â(t) = a(t)/a0)
| |  | æ è
 | dâ dt
 
 | ö ø
 | 2 
 
 
 | = Wv â2 + | Wm ä
 
 |  | 
 | 
This can be solved by separation of variables (the substitution y = â3/2 helps),
| | â(t) = | æ è
 | Wm Wv
 
 | ö ø
 | 1/3 
 
 
 | sinh2/3(3/2 Wv½
H0t). | 
 | 
The present moment occurs when â(t0) = 1, namely
| | t0 = | æ è
 | 2 3H0 Wv½
 
 | ö ø
 | sinh-1 | é ë
 | æ è
 | wv Wm
 
 | ö ø
 | 1/2 
 
 
 | ù û
 | . | 
 | 
18-24
a) Look for the maximum of Ueff of (18.78): this occurs when   -(Wm/â2) + 2Wvâ = 0   or   rm = 2 rv = L/4p.
b) From the Friedman equation (18.77) we have   Ueff(â) = 1/2 Wc   or 
-8p/3 (rm +rvac ) a2 = -1     hence     a = L-½
so the volume is   V = 2p2 a3 = 2p2 L-3/2.
c) The plot of Ueff in Fig 18.9 shows that a small change in rm will either cause the universe to expand to infinite volume, or to collapse to a singularity.
18-27
a) From (18.63) and (18.77) we have
The first law of thermo (18.20) gives
| | p(a) = - | d(ra3) d(a3)
 
 | = | 1 4pa2
 
 |  | d[aUeff(a)] da
 
 |  | 
 | 
That's your parametric representation.
b) The potential should be like (18.78) down to a universe radius when kBT ~ 10 Mev; for smaller a it should rise beyond the value it has a amax in order to cause a bounce.
c) From the above equations, 
So r+ 3p must be negative in the 'smaller a" region of b).
18-30
a) We need r(c) and z(c) such that the geometry to be embedded can be written
dS2 = dc2 + sinh2cdf2 = dr2 + r2 df2 + dz2
Evidently r(c) = sinh(c), but then
| |  | æ è
 | d\z dc
 
 | ö ø
 | 2 
 
 
 | = 1 - cosh2c <  0 | 
 | 
does not work.
b) Exchange sinh and cosh in the above, and the equation does have a solution namely
| | r(u) = cosh u     z(u) = | ó õ
 | u 
 0
 
 | (1 - sinh2u¢)1/2 du¢ | 
 | 
which defines an embedded surface but only up to u = sinh-1(1) = 0.88.