Angular Momentum Transport in Astrophysical Disks

Details Angular Momentum Transport in Astrophysical Disks Angular Momentum Transport in Astrophysical Disks

Jan 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008apj...672l.127g&link_type=abstract

The Astrophysical Journal, Volume 672, Issue 2, pp. L127-L130.

Astronomy and Astrophysics

Astronomy

6

Galaxies: Kinematics And Dynamics, Stars: Planetary Systems: Formation, Solar System: Formation

Scientific paper

The evolution of astrophysical disks is dominated by instabilities of gravity perturbations (e.g., those produced by a spontaneous disturbance). We develop a hydrodynamic theory of nonresonant Jeans instability in a dynamically cold subsystem (identified as the gaseous component) of a disk. We show analytically that gravitationally unstable systems, such as disks of rotationally supported galaxies, protoplanetary disks, and, finally, the solar nebula are efficient at transporting mass and angular momentum: already on a timescale of on the order of 2-3 rotational periods an unstable disk sees a large portion of its angular momentum transferred outward, and mass transferred both inward and outward.

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