Hybrid Mechanisms for Gas/Ice Giant Planet Formation

Details Hybrid Mechanisms for Gas/Ice Giant Planet Formation Hybrid Mechanisms for Gas/Ice Giant Planet Formation

2004-09-29

arxiv.org/abs/astro-ph/0409730v2

Astrophys.J. 629 (2005) 549-555

Astronomy and Astrophysics

Astrophysics

8 pages, 3 figures, 12pt preprint, emulateapj style; two sections added addressing shear-dominated accretion & disk conditions

Scientific paper

10.1086/431272

The effects of gas pressure gradients on the motion of solid grains in the solar nebula substantially enhances the efficiency of forming protoplanetary cores in the standard core accretion model in 'hybrid' scenarios for gas/ice giant planet formation. Such a scenario is enhanced core accretion which results from Epstein-drag induced inward radial migration of mm-sized grains and subsequent particle subdisk gravitational instability needed to build up a population of 1 km planetesimals. Solid/gas ratios can be enhanced by nearly $\sim 10\times$ over those in Minimum Mass Solar Nebula (MMSN) in the outer solar nebula (a $>$ 20 AU), increasing the oligarchic core masses and decreasing formation timescales for protoplanetary cores. A 10 $M_{\oplus}$ core can form on $\sim 10^{6}-10^{7}$ year timescales at 15 - 25 AU compared to $\sim 10^{8}$ years in the standard model,alleviating the major problem plaguing the core accretion model for gas/ice giant planet formation.

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