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Home All issues Volume 499 / No 1 (May III 2009) A&A, 499 1 (2009) 279-290 Full HTML
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Table 1:

Properties of the envelope convection zones in our 20 and 60  $~{M}_\odot$ models of solar metallicity. These are the same models shown in the top panel of Figs. 2 and in 3. The values in the table refer to t =  $6.41\times 10^6$ for the 20  $~{M}_\odot$ model and t =  $2.37\times 10^6$for the 60  $~{M}_\odot$ model.
M Zone ${H}_{{\rm P}}$ $\langle{\varv_{\rm c}}\rangle$ $\Delta M_{\rm conv}$a $\Delta M_{\rm top}$b $N_{\rm cells}$c $\tau_{\rm turn}$d $\tau_{\rm conv}$e $ \dot{M}$
$M_{\odot}$   $R_{\odot}$ km s-1 $M_{\odot}$ $M_{\odot}$   days days $~{M}_\odot~\rm { yr}^{-1}$
20 He 0.025 0.08 $7.6\times10^{-9}$ $1.9\times10^{-9}$ $1.8\times10^{5}$ 2.5 38 $7.3\times10^{-8} $
20 Fe 0.08 2.40 $3.6\times10^{-6}$ $5.8\times10^{-7}$ $1.8\times10^{4}$ 0.25 18 250 $7.3\times10^{-8} $
60 Fe 0.24 2.25 $1.6\times10^{-5}$ $9.8\times10^{-7}$ $8.5\times10^{3}$ 0.83 1570 $3.7\times10^{-6}$
a Mass contained in the convective region. b Mass in the radiative layer between the stellar surface and the upper boundary of the convective zone. c Expected number of convective cells, $N_{\rm cells}:= (R_{\star}/H_{\rm P})^2$. d Convective turnover time, $\tau_{\rm turn}:= H_{\rm P}/\langle{\varv_{\rm c}}\rangle$. e Time that a piece of stellar material spends inside a convective region, $\tau_{\rm conv}:= \Delta M_{\rm conv}/\dot M$.


Source LaTeX | All tables | In the text

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