Oligarchic planetesimal accretion and giant planet formation II

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Table 3:

Input parameters for cases J1, J3 and J7 of P96^a.
Case	$\Sigma$	$\rho$	T	$r_{\rm p}$	$t_{\rm cross}$	$M_{\rm cross}$
	[g ${\rm cm^{-2}}$ ]	[g ${\rm cm^{-3}}$ ]	[K]	[km]	[My]	[ ${M_{\oplus}}$ ]
J1	10	$5 \times 10^{-11}$	150	100	7.58	16.17
J3	15	$5 \times 10^{-11}$	150	100	1.51	29.61
J7	10	$5 \times 10^{-11}$	150	1	6.94	16.18

^a Here $\Sigma$ is the solids surface density of the disc, $\rho$ is the nebular density, T is the nebular temperature (all at the position of Jupiter) and $r_{\rm p}$ is the radius of accreted planetesimals. The results of P96 for $t_{\rm cross}$ and $M_{\rm cross}$ are also listed.

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