Table 2: Computational setup for the 2D AMR calculation T310a. (see Sect. 6.2). The initial and final times over which the inner and outer grid boundaries were held fixed at  $r_{\rm in}$ and  $r_{\rm out}$, are denoted by $t_{\rm i}$ and $t_{\rm f}$, respectively. $\Delta r$ is the (absolute) resolution and  $N^{\rm eff}_{\rm r}$ the number of equidistant radial zones that would have been required to cover the entire star in order to achieve a resolution of $\Delta r$. Exponents are given in brackets.
$t_{\rm i}$ [s] $t_{\rm f}$ [s] $r_{\rm in}$ [cm] $r_{\rm out}$ [cm] $\Delta r$ [km] $N^{\rm eff}_{\rm r}$
0.8(+0) 2.3(+0) 1.0(+8) 4.8(+9) 1.5(+1) 2 599 933

2.3(+0)

 8.0(+0) 1.7(+8) 1.4(+10) 4.6(+1) 847 804

8.0(+0)

 3.4(+1) 3.9(+8) 4.3(+10) 1.4(+2) 280 568

3.4(+1)

 1.2(+2) 9.9(+8) 1.3(+11) 4.2(+2) 93 299

1.2(+2)

 2.8(+2) 2.3(+9) 2.6(+11) 8.4(+2) 46 650

2.8(+2)

 6.5(+2) 3.9(+9) 5.2(+11) 1.7(+3) 23 282

6.5(+2)

 1.5(+3) 6.8(+9) 1.0(+12) 3.4(+3) 11 634

1.5(+3)

 3.6(+3) 1.2(+10) 2.1(+12) 6.7(+3) 5810

3.6(+3)

 2.0(+4) 2.0(+10) 3.9(+12) 1.3(+4) 3072


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