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Stella Offner added begin_deluxetable_lccccccc_tablecolumns_8__.tex
over 8 years ago
Commit id: 56eefb15b6496248c151f17bf46f8be651ff4d49
deletions | additions
diff --git a/begin_deluxetable_lccccccc_tablecolumns_8__.tex b/begin_deluxetable_lccccccc_tablecolumns_8__.tex
new file mode 100644
index 0000000..dbd991a
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+++ b/begin_deluxetable_lccccccc_tablecolumns_8__.tex
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\begin{deluxetable}{lccccccc}
\tablecolumns{8}
\tablecaption{Model Properties\tablenotemark{a} \label{simprop}}
\tablehead{ \colhead{Model } &
\colhead{B($\mu G$)} &
\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). }
\tablenotetext{c}{Same wind model as W2\_T2 but a different initial magnetic field. }
\tablenotetext{d}{Same initial turbulence as run W2\_T2, but containing only a single isolated star with the given mass-loss rate.}
\end{deluxetable}
