Turbulent motions and shocks waves in galaxy clusters simulated with adaptive mesh refinement

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Table 1:

Main characteristics of the runs. ``D'' stands for AMR triggered by gas/DM over-density, while ``V'' stands for AMR triggered by velocity jumps. $\Delta$ is the peak gas spatial resolution. $\delta$ specifies the value adopted to trigger AMR, see Sect. 3 for explanations.
ID	$N_{\rm grid}$	$M_{\rm dm}$ [ $M_{\odot}/h$ ]	$\Delta$ [kpc]	AMR
v256-4	256³	$6.76 \times 10^{8}$	18	D+V( $\delta>10$ )
v256-3	256³	$6.76 \times 10^{8}$	36	D+V( $\delta>3$ )
v128-3	128³	$5.39 \times 10^{9}$	36	D+V( $\delta>3$ )
v64-3	64³	$4.32 \times 10^{10}$	36	D+V( $\delta>3$ )
d128	128³	$5.39 \times 10^{9}$	36	D
v128-10	128³	$5.39 \times 10^{9}$	36	D+V( $\delta>10$ )
v128-1	128³	$5.39 \times 10^{9}$	36	D+V( $\delta>1$ )
v128-z2	128³	$5.39 \times 10^{9}$	36	D+V( $\delta>3$ ,z>2)

Source LaTeX | All tables | In the text

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