Modification of Angular Velocity Distribution by Inhomogeneous Growth of MRI in Protoplanetary Disks

Details Modification of Angular Velocity Distribution by Inhomogeneous Growth of MRI in Protoplanetary Disks Modification of Angular Velocity Distribution by Inhomogeneous Growth of MRI in Protoplanetary Disks

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.7603k&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #76.03; Bulletin of the American Astronomical Society, V

Astronomy and Astrophysics

Astronomy

Scientific paper

We have performed two-dimensional CIP -MOCCT simulations of Magneto Rotational Instability (MRI) in accretion disks with nonzero ohmic resistivity. An accretion disk is formed as the gas around a protostar accretes to the central star. In the disk the formation of a planetary system proceeds. When the accretion disks have a weak magnetic field, it is well known that the Magneto Rotational Instability (MRI) is excited in the disks (Balbus & Hawley, 1991). Linear analyses by Sano & Miyama (1998) show that MRI growth rates are affected by various factors, such as weaker vertical magnetic field reducing growth rates in the presence of finite resistivity. A protoplanetary disk is considered to be weakly ionized. Then there can be a radial inhomogeneity of the MRI growth rate due to a spatial variation in the magnetic configuration. We have performed simulations of cases in which a MRI unstable and a MRI stable annulus are situated. Inhomogeneous MRI growth is observed and the angular momentum exchange proceeds vigorously only within the MRI unstable annulus. As a result, the radial profile of the angular velocity is modified such that, with the rigid rotation inside the unstable annulus as the extreme case, the angular velocity decline with distance from the central star is slower than the Kepler profile in and adjacent to the unstable annulus. As a result some parts of the accretion disk have the gas to rotate faster than the dust particles. The implication is that the process may lead to the prevention of dusts from falling to the central star and further to the formation of planetesimals. We also have performed three-dimensional simulations with test particles included and have examined the dust dynamic in detail.

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