Problem Set 4: Due Thursday, Octber 31
AST 352, Fall 2013
Problem 1
The Rosseland mean opacity is defined to be:
B
T d
1
2h 3
= 0
, where B is the Planck function B (T ) = 2 (e h kT 1) .
1 B
c
T d
0
Calculate the Rosseland mean opacity for the case of

Problem Set 1: Due Tuesday, September 17
AST 352, Fall 2013
Problem 1
a. Use the equations of stellar structure to find the mass-luminosity relation and the massradius relation of Main Sequence stars. You may use Homology and drop all constants to
find si

Problem Set 3: Due Thursday, October 17
AST 352, Fall 2013
Problem 1
Write a computer program to solve the Lane-Emden equation:
1 d $ 2 d '
n
&
) = , for a polytrope of index n . The equation can be re-written in the
2 d % d (
2
more useful form: " = " n

Final Project: Due Friday, December 13
AST 352, Fall 2013
Part 1
Create a computer model that solves the structure of a star assuming a set of central
boundary conditions. Specifically, solve a star of mass M = 7.08M sun , with solar
composition: X = 0.7,

Problem Set 5: Due Tuesday, November 19
AST 352, Fall 2013
Problem 1
The energy-averaged cross section is given by v = CS0 2e , where C and S0 are
19.721W 1 3
2 2 A j Ak
constants, is given by =
, where Z, A are the
1 3 and W = Z j Z k
A j + Ak
(T 107 K )

Problem Set 2: Due Thursday, October 3
AST 352, Fall 2013
Problem 1
Calculate the gravitational potential energy of a star in terms of its mass and radius
GM 2
(i.e., calculate the q factor in the expression q
), in the cases where the density
R
profile o