The internal energy for molecular hydrogen in gravitationally unstable protoplanetary disks
The internal energy for molecular hydrogen in gravitationally unstable protoplanetary disks
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DOI：
10.1086/512235
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发表时间：
2007-02-20
影响因子：
4.9
通讯作者：
Michael, Scott
中科院分区：
文献类型：
--
作者：
Boley, Aaron C.;Hartquist, Thomas W.;Michael, Scott
气体状态方程可能是气态巨行星形成盘不稳定性理论的关键因素之一。本文讨论了在重力不稳定盘的流体动力学模拟中H-2的处理。在我们的讨论中，我们指出了错误的比内能关系、不连续的近似比内能关系和常数Gamma(1)假设的可能后果。此外，我们考虑了H-2在原行星盘中的正对位比是否应该被动态地处理，如果物种处于平衡状态。初步模拟表明，当T = 30-50 K时，正确的处理方法对于研究重力不稳定性尤为重要。
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.