Gas dynamics around a Jupiter-mass planet - I. Influence of protoplanetary disk properties

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Table 3

Total mass inflow, $| {\dot{M}}_{i} |$ $\[\left|\dot{M}_i\right|\]$ and outflow, ${\dot{M}}_{o}$ $\[\dot{M}_o\]$ rates.

Model	$\| {\dot{M}}_{i} \|$ $\[\left\|\dot{M}_i\right\|\]$	${\dot{M}}_{o}$ $\[\dot{M}_o\]$	$\dot{M}$ $\[\dot{M}\]$ [M_⊕/yr]
N	0.104	0.075	0.029
Lm	0.0115	0.0022	0.009
LmLv	0.0023	0.00074	0.00156

Notes. The data are obtained from the sum of the values ${\dot{M}}_{i} (z)$ $\[\dot{M}_i(z)\]$ and ${\dot{M}}_{o} (z)$ $\[\dot{M}_o(z)\]$ plotted in Fig. 8. The resulting values have been multiplied by 2 to take into account the whole Hill sphere. The fourth column is simply the difference between the inflow and the outflow rates and provides the net accretion rate on the Hill sphere. The computation is done on a snapshot at five of the planet’s orbital periods.

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