deletions | additions       diff --git a/Ryan_modify_table_to_reflect__.tex b/Ryan_modify_table_to_reflect__.tex  index e42d123..2dccb4e 100644  --- a/Ryan_modify_table_to_reflect__.tex  +++ b/Ryan_modify_table_to_reflect__.tex 
...
\end{table}  %Aastex ApJ table format.  \begin{table}{lccccccc} \begin{table}{lccccc}  %\tablecolumns{8}  \tablecaption{Model Properties\tablenotemark{a} \label{simprop}}  \tablehead{ \colhead{Model } &  
...
\colhead{ $\beta$} &  \colhead{$t_{\rm evol}$(Myr)} &  \colhead{$\dot M_{\rm tot}(10^{-6 }\msun {\rm yr}^{-1})$\tablenotemark{b}} &  \colhead{ $v_{\rm max}$ ($\kms$)} &  \colhead{ $d_{x}$ (AU)} &  \colhead{Driving }}  \startdata  W1\_T1\_t1 & 13.5 & 0.1 & 0.1 & 41.7 & 200 &10$^3$ &N  \\ %2a W1\_T2 & 13.5 & 0.1 & 0.2 & 41.7 & 200 &10$^3$ &N  \\ %2b W2\_T2 & 13.5 & 0.1 & 0.2 & 4.5 & 200 &10$^3$ &Y  \\ %3a W2\_T3\tablenotemark{c} &5.6 & 0.6 & 0.1 & 4.5 & 200 &10$^3$ &Y  \\ %3b W2\_T4\tablenotemark{c} &30.1 & 0.02 & 0.1 & 4.5 & 200 &10$^3$ &N  \\ %3c \enddata  \tablenotetext{a}{[Ryan modify to reflect the outputs you analyzed] Model name, initial mean magnetic field, ratio of thermal to magnetic pressure, the evolutionary time, the total stellar mass-loss rate, the maximum wind velocity, minimum grid resolution, and whether external driving is continued simultaneously with winds or whether winds alone inject energy. All models have $L=5$pc, $M=3762 \msun$, $T_i=10$K and $N_*=5$. } %rho=2.04d-21  \tablenotetext{b}{The estimated mass-loss rate from all stellar winds in Perseus is $9.49 \times 10^{-6}\msun$yr$^{-1}$ (Arce et al.~2011). }