Gravitationally unstable protoplanetary discs

Details Gravitationally unstable protoplanetary discs Gravitationally unstable protoplanetary discs

Jan 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006mnras.365.1007g&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 365, Issue 3, pp. 1007-1011.

Astronomy and Astrophysics

Astronomy

8

Planets And Satellites: Formation, Planetary Systems: Formation

Scientific paper

The possibility that protoplanetary gaseous discs are dynamically unstable to axisymmetric and non-axisymmetric gravity perturbations (e.g. those produced by spontaneous disturbances) with characteristic scales larger than the vertical scale height is discussed analytically, using a local Wentzel-Kramers-Brillouin (WKB) approach. It is shown that such discs might be clumpy, and these gravitationally bound clumps may later collapse to become giant planets (`hot Jupiters'). The chief aim in this paper is to underscore a fact of vital importance for application in the planetary formation process: gravitationally unstable non-axisymmetric (spiral) perturbations can effectively transport both the angular momentum and the mass in a spatially inhomogeneous disc.

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