% -*- latex -*-
% FILE: "/home/evmik/jobs/wm/2013_spring_Modern_Astrophysics_476/hw10/hw10.tex"
% LAST MODIFICATION: "Wed, 03 Apr 2013 16:18:23 -0400 (evmik)"
% (C) 2010 by Eugeniy Mikhailov, <evgmik@gmail.com>
% $Id:$
\documentclass[letter,12pt]{article}

%---------------------------------------------------------------
\usepackage{listings}
\usepackage{color}
\usepackage{fullpage}
%---------------------------------------------------------------

\begin{document}
\newcommand{\problem}[1]{%
	{\flushleft  \bf #1\\}
}
\newcommand{\hw}[1]{%
	\begin{center}
		\Large  \bf Homework #1%
	\end{center}%
}
\newcommand{\mat}[1]{% matlab code
{\color{blue}\texttt{#1}}%
}

%---------------------------------------------------------------
\hw{10}

\problem{Problem 1 (5 points)}
%---------------------------------------------------------------

Take a star with mass of 4.5~M$_\odot$ and  radius of 44.5~R$_\odot$
find the period of pulsation of this star due governed by pressure support.
Does this period matches $\delta$ Cephei.


\problem{Problem 2 (5 points)}
%---------------------------------------------------------------
Does this star has a larger magnitude when it is 
compressed or when it is expanded. Why so?


\problem{Problem 3 (5 points)}
%---------------------------------------------------------------
$\delta$ Cephei changes its magnitude from 2 to 10 over the period. What is
required relative radius change to achieve such luminosity modulation?
Assume that process is adiabatic and linearization holds even for large
deviations. 

\problem{Problem 4 (5 points)}
%---------------------------------------------------------------
Starting from formula 12.14 for Jeans mass arrive to formula 12.17 and show
that with simple model we should use $C_{BE} = C_{J} = 5.46$




%---------------------------------------------------------------
\end{document}
%---------------------------------------------------------------