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### ASTR 3740 Relativity & Cosmology Spring 2004. Problem Set 6. Due Wed 14 Apr

This problem set may take you some time to complete, so please do not wait until the last day to start it.

1. Anti-gravity

(a) Condition for an accelerating Universe

Suppose that the Universe contains only matter energy (M) and vacuum energy (a cosmological constant L), and that it is geometrically flat

 WM + WL = 1
(1.1)
where WM º rM/rc and WL º rL/rc are the contributions to Omega in matter and vacuum. How big must WL be for the Universe to be accelerating? [Hint: Friedmann's equation for the acceleration d2a / d t2 of the cosmic scale factor a(t) is
 ..a

a

= - 4
3
p G ( r + 3 p )
(1.2)
which shows that the Universe is accelerating if r + 3 p < 0. Ordinary matter has mass-energy density rM but essentially no pressure, pM = 0, while vacuum has negative pressure equal to its mass-energy density, pL = - rL.]

Papers describing latest results from the two high-redshift supernova teams are at http://arXiv.org/abs/astro-ph/0309368 and http://arXiv.org/abs/astro-ph/0402512 . The websites of the two teams are the "Supernova Cosmology Project" at http://supernova.lbl.gov and the "High-Z Supernova Search" at http://cfa-www.harvard.edu/cfa/oir/Research/supernova/ (sadly, the website of the High-Z SN team appears out of date). A good place to start searching for more information about supernovae is "Supernova and Supernova Remnant Pages on the WWW" http://rsd-www.nrl.navy.mil/7212/montes/sne.html .

What are the latest results from the two high-redshift supernova teams? Do they agree with regard to their measurements of WM and WL? What is this w thing that they both report?

2. Solutions to Friedmann's equations in a Flat Universe

Suppose that the Universe is flat, k = 0, so that Friedmann's energy equation reduces to

 .a 2

a2

= 8
3
p G r  .
(2.1)
Suppose further that the Universe is dominated by stuff whose mass-energy density r varies with cosmic scale factor a as
 r µ a-n
(2.2)
as the Universe expands, with n a constant. For example, n = 3 for ordinary matter, n = 4 for radiation, and n = 0 for vacuum energy.

(a) Case n ¹ 0

Solve Friedmann's equation to show that, for n ¹ 0,

 a µ t2/n  .
(2.3)
[Hint: You should find that Friedmann's equation can be recast in the form t = ò f(ada where f(a) is some function of cosmic scale factor a. You may set a = 0 at t = 0, which says that the Universe had zero size at zero age.]

(b) Deceleration or acceleration?

For what range of n is the Universe decelerating (da/dt < 0) or accelerating (da/dt > 0)? Is the Universe decelerating or accelerating in the particular cases of a matter-dominated (n = 3) or radiation-dominated (n = 4) Universe?

(c) Case n = 0

The case n = 0 corresponds to vacuum density, which remains constant as the Universe expands. Solve Friedmann's equation for this case to show that

 a µ eH t
(2.4)
where H º (da/dt)/a, the Hubble constant, is in this case a constant in time as well as space. What is the Hubble constant H here in terms of the vacuum energy rL?

(d) For your information (no credit)

You may be wondering whether there is a relation between the index n in this question and the pressure p in the Anti-Gravity question. The answer is yes. It is straightforward to show (but I'm not asking you to do this) from the energy equation d (ra3 ) + p d (a 3) = 0 (which you may recognize as the equation dE + p dV = 0 of thermodynamics) that

 n = 3 æçè 1 + p r ö÷ø .
(2.5)

3. Flatness Problem

An amusing statement of this cosmological problem can be found on Ned Wright's graph.

(a) Yet another version of Friedmann's equation

Use the definitions H2 = (8/3) p G rc of the critical density rc, and W º r/rc of Omega, to show that Friedmann's equation (including the curvature term)

 H2 = 8 3 p G r - k c2 a2
(3.1)
can be rewritten in the form
 W - 1 W = 3 k c2 8 p G r a2 .
(3.2)

(b) Evolution of W with a

Suppose once again that r µ a-n. Show that (a simple consequence of [3.2])

 W - 1 W µ  a?
(3.3)
where ? is an exponent which you should derive (in terms of n).

(c) Here's the flatness problem

Suppose that the temperature at the moment of the Big Bang was about the Planck temperature ~ 1032 K. The radiation temperature of the Universe today is of course that of the CMB, about 3 K. If W0 (subscript 0 means the present time) is of order, but not equal to, one at the present time (W0 ~ 0.3, say), roughly how close to one was W at the Big Bang? [Hint: Define the small quantity e º W - 1, and use (3.3) to estimate e at the Big Bang. Note that for tiny e, you can approximate 1 + e » 1. Assume that T µ a-1 during the expansion of the Universe, and assume for simplicity that the Universe has been radiation-dominated for most of that expansion, so that n » 4.]