All Tables

Table 1: Some properties of the initial model: total mass M, stellar population, metal content Z, mass $M_{\rm He}$ and radius $R_{\rm He}$ of the helium core ( $X(^{4}{\rm He}) > 0.98$ ), nuclear energy production in the helium core $L_{\rm He}$ , maximum temperature of the star $T_{\rm max}$ , and radius $r_{\rm max}$ and density $\rho _{\rm max}$ at the temperature maximum.
Table 2: Some properties of the 1D simulations: number of radial grid points ( $N_{\rm r}$ ), radial resolution ( $\Delta r$ in 10⁶ cm), time up to the thermonuclear runaway $t_{\rm trn}$ , and maximum evolution time $t_{\rm max}$ (both in s).
Table 3: Some properties of the 2D simulations: number of grid points in radial ( $N_{\rm r}$ ) and angular ( $N_{\theta }$ ) direction, radial ( $\Delta r$ in 10⁶ cm) and angular grid resolution ( $\Delta \theta$ ), characteristic length scale $l_{\rm c}$ of the flow (in 10⁸ cm), characteristic rms velocity $v_{\rm c}$ of the flow (in $10^{6}\mbox{\ cm s${}^{-1}$ }$ ) averaged over the width of the convection zone R $\sim$ $l_{\rm c}$ , Reynolds number $R_{\rm n}$ associated with the numerical viscosity of our code (Porter & Woodward 1994), damping timescale due to the numerical viscosity $t_{\rm n}$ , typical convective turnover time $t_{\rm o} = 2~R/v_{\rm c}$ , and maximum evolution time $t_{\rm max}$ (in s), respectively.