Cosmic-ray driven dynamo in the interstellar medium of irregular galaxies

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Table 3:

Summary of the simulations results.
$\begin{displaymath}\begin{tabular}{lr@{.}lr@{.}lr@{.}lr@{.}lccl} \hline \hline\n... ... 209 & SN activity during first 50 Myr \\ \hline \end{tabular}\end{displaymath}$ Notes. The subsequent columns show: the model name, the mean value of total magnetic energy $\bar{E}_B^{\rm end}$ over past 50 Myr, the total outflow of magnetic energy during whole simulation (see Eq. (12)), the ratio of these two quantities, the final mean value of the magnetic field in a disc midplane $\langle B\rangle$ (\|z\|< 20 pc), the e-folding time of magnetic flux increase $t_{\rm e}$ , galaxy revolution timescale $T_\Omega$ , and a short description of a model. Superscripts are explained in Table 2. Values of magnetic field energy are normalized to the initial value.

Source LaTeX | All tables | In the text

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