Planet migration in three-dimensional radiative discs
Planet migration in three-dimensional radiative discs
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DOI：
10.1051/0004-6361/200912072
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发表时间：
2009-08
影响因子：
6.5
通讯作者：
W. Kley;B. Bitsch;Hubert Klahr University of Tuebingen;Max-Planck Institue of Astronomy
中科院分区：
文献类型：
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作者：
W. Kley;B. Bitsch;Hubert Klahr University of Tuebingen;Max-Planck Institue of Astronomy
上下文生长中的原行星的迁移取决于周围圆盘的热力学。使用局部等温盘的标准模型表明，在低行星质量状态下存在向内（I型）迁移。考虑到非等温效应，最近的研究表明，I型迁移的方向可以从向内到向外改变。目标。在本文中，我们扩展了以前的二维研究和调查的行星盘相互作用的粘性，辐射盘使用全三维辐射流体动力学模拟的原行星吸积盘嵌入行星，行星质量的范围。方法.我们使用一个明确的三维（3D）流体动力学代码NIRVANA，包括全张量粘度。我们在通量限制扩散近似中添加了隐式辐射输运，为了显著加快模拟速度，我们在3D环境中重新调整并实施了FARGO算法。结果首先，我们提出了测试模拟的结果，证明了新实施的FARGO方法在3D中的准确性。对于一个20 Mearth的行星质量，我们然后表明，包括辐射效应也会产生一个完整的3D扭矩反转。对于相同的不透明度定律，由于光盘稍薄，3D中的效果甚至比相应的2D模拟更强。最后，我们通过计算一系列行星质量来证明扭矩反转的程度。结论.通过对粘性辐射盘中嵌入行星的全三维模拟，我们证实了迁移可以向外定向到大约33 Mearth的行星质量。因此，这种效应可能有助于解决行星在I型阶段向内迁移太快的问题。
Context. The migration of growing protoplanets depends on the thermodynamics of the ambient disc. Standard modelling, using locally isothermal discs, indicate an inward (type-I) migration in the low planet mass regime. Taking non-isothermal effects into account, recent studies have shown that the direction of the type-I migration can change from inward to outward. Aims. In this paper we extend previous two-dimensional studies and investigate the planet-disc interaction in viscous, radiative discs using fully three-dimensional radiation hydrodynamical simulations of protoplanetary accretion discs with embedded planets, for a range of planetary masses. Methods. We use an explicit three-dimensional (3D) hydrodynamical code NIRVANA that includes full tensor viscosity. We have added implicit radiation transport in the flux-limited diffusion approximation, and to speed up the simulations significantly we have newly adapted and implemented the FARGO-algorithm in a 3D context. Results. First, we present results of test simulations that demonstrate the accuracy of the newly implemented FARGO-method in 3D. For a planet mass of 20 Mearth, we then show that including radiative effects also yields a torque reversal in full 3D. For the same opacity law, the effect is even stronger in 3D than in the corresponding 2D simulations, due to a slightly thinner disc. Finally, we demonstrate the extent of the torque reversal by calculating a sequence of planet masses. Conclusions. Through full 3D simulations of embedded planets in viscous, radiative discs, we confirm that the migration can be directed outwards up to planet masses of about 33 Mearth. As a result, the effect may help to resolve the problem of inward migration of planets that is too rapid during their type-I phase.