Journal
ASTROPHYSICAL JOURNAL
Volume 656, Issue 2, Pages L89-L92Publisher
UNIV CHICAGO PRESS
DOI: 10.1086/512235
Keywords
accretion, accretion disks; equation of state; hydrodynamics; instabilities; molecular tprocesses
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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 hydrodynamic 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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