Abstract
Gravitational instabilities (GIs) can occur in any region of a gas disk that becomes sufficiently cool or develops a high enough surface density. In the nonlinear regime, GIs can produce local and global spiral waves, self-gravitating turbulence, mass and angular momentum transport, and disk fragmentation into dense clumps and substructure. It has been quite some time since the idea was first suggested by Kuiper (1951) and Cameron (1978), and revived by Boss (1997, 1998) stating that the dense clumps in a disk fragmented by GIs may become self-gravitating precursors to gas giant planets. This particular idea for gas giant planet formation has come to be known as the disk instability theory. The idea is appealing since gravitational instability develops on very short timescales compared to the accumulation of planetesimals by gravity and the subsequent accretion of gas by a rocky core, the conventional two-stage giant planet formation theory known as core accretion (see the chapter by Marzari et al.).
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Notes
- 1.
The first adiabatic index Γ 1 for a simple perfect gas is the same as γ and is equal to 1 + R g ∕ (μ g C V ).
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Acknowledgments
We thank Richard H. Durisen and Nader Haghighipour for their improvements to the manuscript. APB’s work is supported in part by the NASA Planetary Geology and Geophysics Program under grants NNG05GH30G and NNX07AP46G, and is contributed in part to the NASA Astrobiology Institute under grant NCC2-1056. Parts of this work were carried out under the auspices of the National Nuclear Security Administration of the U.S. Department of Energy at Los Alamos National Laboratory under Contract No. DE-AC52-06NA25396, for which this is publication LA-UR-07-7370.
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Mayer, L., Boss, A., Nelson, A.F. (2010). Gravitational Instability in Binary Protoplanetary Disks. In: Haghighipour, N. (eds) Planets in Binary Star Systems. Astrophysics and Space Science Library, vol 366. Springer, Dordrecht. https://doi.org/10.1007/978-90-481-8687-7_8
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