PROTOPLANETARY DISK WINDS VIA MAGNETOROTATIONAL INSTABILITY: FORMATION OF AN INNER HOLE AND A CRUCIAL ASSIST FOR PLANET FORMATION
PROTOPLANETARY DISK WINDS VIA MAGNETOROTATIONAL INSTABILITY: FORMATION OF AN INNER HOLE AND A CRUCIAL ASSIST FOR PLANET FORMATION
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DOI：
10.1088/0004-637x/718/2/1289
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发表时间：
2009-11
期刊：
影响因子：
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通讯作者：
T. Suzuki;T. Muto;S. Inutsuka
中科院分区：
文献类型：
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作者：
T. Suzuki;T. Muto;S. Inutsuka
通过建立一个基于三维局部磁流体动力学模拟的全局模型，我们发现由磁旋转不稳定性（MRI）驱动的盘风在原行星盘气体成分的分散中起着重要作用。由于核磁共振驱动的圆盘风的质量损失时间尺度与当地的开普勒旋转周期成正比，因此气体盘从内部区域动态蒸发，可能形成一个逐渐扩大的内部孔，而相当数量的气体留在外部区域。盘风高度依赖于时间，在每个半径处具有数倍于开普勒自转周期的准周期性，这将作为原恒星-原行星盘系统的时间变异性来观察。即使存在死区，这些特征也会持续存在，因为圆盘风来自电离宇宙射线和高能光子可以穿透的表面区域。此外，预测的由内而外的清理显著抑制了巨石落向中心恒星和原行星的I型迁移，这有利于行星的形成和生存。
By constructing a global model based on three-dimensional local magnetohydrodynamical simulations, we show that the disk wind driven by magnetorotational instability (MRI) plays a significant role in the dispersal of the gas component of protoplanetary disks. Because the mass loss timescale of the MRI-driven disk winds is proportional to the local Keplerian rotation period, a gas disk dynamically evaporates from the inner region, possibly creating a gradually expanding inner hole, while a sizable amount of the gas remains in the outer region. The disk wind is highly time dependent with a quasi-periodicity of several times the Keplerian rotation period at each radius, which will be observed as the time variability of protostar–protoplanetary disk systems. These features persistently hold even if a dead zone exists because the disk winds are driven from the surface regions where ionizing cosmic rays and high energy photons can penetrate. Moreover, the predicted inside–out clearing significantly suppresses the infall of boulders to a central star and the type I migration of proto-planets, which are favorable for the formation and survival of planets.