deletions | additions       diff --git a/Physical parameters.tex b/Physical parameters.tex  index 3aa6a25..1c2f183 100644  --- a/Physical parameters.tex  +++ b/Physical parameters.tex 
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The second set of ELC models uses constraints from atmosphere modeling, and breaks the light curves into ``chunks'' to search for stellar activity on the timescale of one orbital period.  % Write more here  In both cases, we use ELC to solve for 16 parameters: orbital period $P_{orb}$, $T_{conj}$ (a zeropoint that sets the deeper primary eclipse to orbital phase $\phi_{ELC} = 0.5$), orbital inclination $i$, $e \sin \omega$ and $e \cos \omega$ (where $e$ is eccentricity and $\omega$ is the longitude of periastron), the temperature of the primary star $T_1$, the mass of the primary star $M_1$, the amplitude of the primary star's radial velocity curve $K_1$, the fractional radii of each star $R_1/a$ and $R_2/a$ (where $a$ is the average orbital seperation), the \emph{Kepler} contamination factor, and stellar limb darkening parameters for the quadratic limb darkening law. Because all binaries obey the relation  \begin{equation}  \frac{M_1}{M_2} = \frac{K_2}{K_1},  \end{equation}  the final result from an ELC model includes masses and radii for both stars.  %The final model values are presented somewhere useful, like a table, with error bars.