Phys/Astro 228: Extragalactic Astronomy and Cosmology
September 8 2006
C.–P. Ma
Problem Set 1
Due: Friday September 15 in class
Homework Policy
:
No late homework
. You should make all efforts to solve the problems entirely
on your own. You may consult a classmate for inspiration if you are really stuck, but once you have
received the hints, you should resolve and write up the solutions by yourself.
Readings: Chapter 1 of Dodelson and Sec 19.1 of “Big Bang Cosmology” from Review
of Particle Physics (see link at course website).
The latter is a brief summary of a subset of
the equations we have derived in class. Note two differences in conventions: (1) We use dimensionless
a
and they use dimensional
R
for the scale factor; (2) Our cosmological constant Λ is included in the
energy density
ρ
in the Friedmann equation while they write it out as a separate term in their (19.8).
1.
Time Evolution of
Ω
As we discussed in class, the density parameter Ω generally is not a constant in time.
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 Fall '06
 CHUNGPEIMA
 Cosmology, General Relativity, Physical cosmology, Cosmological constant, Friedmann, Friedmann equation

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