原行星盘引力不稳定性的热调节。IV。包络辐照模拟
The Thermal Regulation of Gravitational Instabilities in Protoplanetary Disks. IV. Simulations with Envelope Irradiation
摘要：
一般认为，包层中的原行星盘质量更大，因此比暴露在外的盘更容易受到引力不稳定性的影响。我们提出了三维辐射流体动力学模拟的原行星盘与信封照射的存在。对于一个半径为40 AU，质量为0.07 Msun的盘，围绕着一颗0.5 Msun的年轻恒星，随着辐射通量的增加，包络辐射趋于减弱甚至抑制GI。由GI引起的整体质量输运由低阶模式主导，并且照射优先抑制高阶模式。因此，重力力矩和质量流入率实际上增加了温和的照射。没有一个模拟产生密集的团块或通过对流快速冷却，反对通过盘不稳定直接形成巨行星，至少在辐射盘中。然而，致密的气体环和径向质量集中产生，这些可能有助于加速行星核心的形成。模拟一个大规模的嵌入式磁盘的初步结果与嵌入源L1551 IRS5中的磁盘之一的物理特性相似，表明辐射冷却时间长，没有碎片。在这个磁盘中的地理信息系统是由全球的双臂和三臂模式。
英文摘要：
It is generally thought that protoplanetary disks embedded in envelopes are more massive and thus more susceptible to gravitational instabilities (GIs) than exposed disks. We present three-dimensional radiative hydrodynamics simulations of protoplanetary disks with the presence of envelope irradiation. For a disk with a radius of 40 AU and a mass of 0.07 Msun around a young star of 0.5 Msun, envelope irradiation tends to weaken and even suppress GIs as the irradiating flux is increased. The global mass transport induced by GIs is dominated by lower-order modes, and irradiation preferentially suppresses higher-order modes. As a result, gravitational torques and mass inflow rates are actually increased by mild irradiation. None of the simulations produce dense clumps or rapid cooling by convection, arguing against direct formation of giant planets by disk instability, at least in irradiated disks. However, dense gas rings and radial mass concentrations are produced, and these might be conducive to accelerated planetary core formation. Preliminary results from a simulation of a massive embedded disk with physical characteristics similar to one of the disks in the embedded source L1551 IRS5 indicate a long radiative cooling time and no fragmentation. The GIs in this disk are dominated by global two and three-armed modes.
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