3D Simulations of the Collapse of Protoplanetary Clumps in Disk Instability Using a New Equation of State.

Details 3D Simulations of the Collapse of Protoplanetary Clumps in Disk Instability Using a New Equation of State. 3D Simulations of the Collapse of Protoplanetary Clumps in Disk Instability Using a New Equation of State.

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ess.....2.3306g&link_type=abstract

American Astronomical Society, ESS meeting #2, #33.06

Astronomy and Astrophysics

Astronomy

Scientific paper

We present the first realistic study of the evolution of protoplanetary clumps formed in disk instability, in order to assess whether or not they can collapse into gas giant planets.
As a first step, we derive a new equation of state for a mixture of atomic and molecular hydrogen which takes into account para-ortho ratio for molecular hydrogen, freezing of degrees of
freedom at low temperatures and the dissociation of molecular hydrogen. We run our simulations with a new version of Gasoline implementing this new equation of state, and taking our initial
condition for the clumps from global 3D simulations
of accreting protoplanetary disks by T. Hayfield and L. Mayer (see eg Boley et al. 2010). Our results show that the code is able to resolve the collapse through dissociation, covering several
orders of magnitude in density.
As a second step, we study how the internal angular momentum and the non-axisymmetry of a self-gravitating clump affect its evolution.
Preliminary results show that rotating clumps collapse into a slowly rotating, dense core surrounded by a fast rotating envelope/circumplanetary disk, due to the redistribution of angular momentum
and mass induced by bar-like and spiral instabilities. We then determine the collapse time of clumps of a variety of masses including radiative cooling, and we compare with published semi-analytical
work assuming spherical, quasi-static collapse.
By being able to determine the collpase time and the configuration of the clump after it contracts dynamically following dissociation we also lay out a scheme for implementing a sub-grid
model of clump evolution and collapse in global disk simulations.

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