Oligarchic planetesimal accretion and giant planet formation II

Home

All issues

Volume 500 / No 3 (June IV 2009)

A&A, 500 3 (2009) 1249-1252

Full HTML

Free Access

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.

Source LaTeX | All tables | In the text

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.