Sub-surface convection zones in hot massive stars and their observable consequences

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, $\tau_{\rm conv}:= \Delta M_{\rm conv}/\dot M$ .

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