deletions | additions       diff --git a/clumps.tex b/clumps.tex  index 66267ac..eb9f5a2 100644  --- a/clumps.tex  +++ b/clumps.tex 
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\begin{table*}  \begin{minipage}[t]{\textwidth} \begin{minipage}{\textwidth}  \caption{Properties of the envelope convection zones in our 20 and 60 $\mso$ models of solar metallicity. These are the same models shown in the top panel of Fig.~\ref{20zsunsurf} and in Fig.~\ref{60zsunsurf}. The values in the table refer  to t=\ttwenty for the 20 $\mso$ model and t=\tsixty for the 60 $\mso$ model.}  \label{clumps}  \renewcommand{\footnoterule}{}  \centering  \begin{tabular}{l|ccccccccc} \begin{tabular}{lccccccccc}  \hline\hline  M \T & Zone & $\hp$ & $\vca$ & $\Delta M_{\rm conv}$\footnote{Mass contained in the convective region.} & $\Delta M_{\rm top}$\footnote{Mass in the radiative layer between the stellar surface and the upper boundary of the convective zone.} & $N_{\rm cells}$\footnote{Expected number of convective cells, $N_{\rm cells}:= (R_{\star}/H_{\rm P})^2$.} & $\tau_{\rm turn}$\footnote{Convective turnover time, $\tau_{\rm turn}:= H_{\rm P}/\vca$.} & $\tau_{\rm conv}$\footnote{Time that a piece of stellar material spends   inside a convective region, $\tau_{\rm conv}:= \Delta M_{\rm conv}/\dot M$.} & $ \dot{M}$ \\