The Internal Energy for Molecular Hydrogen in Gravitationally Unstable Protoplanetary Disks

Details The Internal Energy for Molecular Hydrogen in Gravitationally Unstable Protoplanetary Disks The Internal Energy for Molecular Hydrogen in Gravitationally Unstable Protoplanetary Disks

2007-01-05

arxiv.org/abs/astro-ph/0701146v1

Astrophys.J.656:L89-L92,2007

Astronomy and Astrophysics

Astrophysics

13 pages, 3 figures. To appear in ApJL

Scientific paper

10.1086/512235

The gas equation of state may be one of the critical factors for the disk instability theory of gas giant planet formation. This letter addresses the treatment of H$_2$ in hydrodynamical simulations of gravitationally unstable disks. In our discussion, we point out possible consequences of erroneous specific internal energy relations, approximate specific internal energy relations with discontinuities, and assumptions of constant $\Gamma_1$. In addition, we consider whether the ortho/para ratio for H$_2$ in protoplanetary disks should be treated dynamically as if the species are in equilibrium. Preliminary simulations indicate that the correct treatment is particularly critical for the study of gravitational instability when $T = 30$-50 K.

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