\relax 
\@writefile{toc}{\contentsline {section}{\numberline {1} What is an eclipsing binary star?}{1}}
\@writefile{toc}{\contentsline {section}{\numberline {2} Describing the Star System}{1}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces  How large the stars are can make the difference between having an eclipse and not. The large stars on the left eclipse each other, but the small stars on the right do not.}}{2}}
\newlabel{largesmall}{{1}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces  If a star is very large, the gravitational force from the other star will pull it out into a teardrop shape.}}{2}}
\newlabel{teardrop}{{2}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces  The size of the star can be expressed by the ``Roche lobe filling factor'', which tells you how large the star is compared to how large it can be before gas starts to get pulled off of the star. In the figure on the left, the smaller star has a Roche lobe filling factor of 0.5, while the larger star has a Roche lobe filling factor of 1.0. This means that the large star is just big enough for gas to fall onto the smaller star. In the middle figure, both stars have a Roche lobe filling factor of 1.0, so they just barely touch in the middle. In the figure on the right, the stars have a Roche lobe filling factor larger than one, so they have actually merged into a single object.}}{3}}
\newlabel{roche}{{3}{3}}
\@writefile{toc}{\contentsline {section}{\numberline {3}How to Use Nightfall}{3}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.1}Overview}{4}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.2}Figuring out the Right Parameters}{7}}
\@writefile{toc}{\contentsline {section}{\numberline {4}Publication}{7}}