Evolution of protoplanetary discs with magnetically driven disc winds (Corrigendum)
Evolution of protoplanetary discs with magnetically driven disc winds (Corrigendum)
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DOI：
10.1051/0004-6361/201628955
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发表时间：
2016-09
期刊：
影响因子：
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通讯作者：
T. Suzuki;M. Ogihara;A. Morbidelli;A. Crida;T. Guillot
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文献类型：
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作者：
T. Suzuki;M. Ogihara;A. Morbidelli;A. Crida;T. Guillot
目标：我们利用磁驱动盘风和粘性加热研究原行星盘（以下简称 PPD）的演化。方法：我们考虑一个初始质量约为 0.1 Msun 的圆盘来追踪 PPD 早期阶段的演化。我们通过在吸积盘标准阿尔法模型的框架内考虑粘性加热以及盘风造成的质量和角动量的损失来解决表面密度和温度的时间演化。我们的模型参数、湍流粘度、圆盘风质量损失和圆盘风扭矩是从局部磁流体动力学模拟中采用的，并受到重力吸积的全局能量学的约束，很大程度上取决于PPD的物理条件，特别是弱电离PPD中垂直磁通量的演变。结果：尽管剩余垂直磁通量的演化仍然存在不确定性，但表面密度显示出很大的变化，具体取决于这三个参数的组合，其中一些与标准吸积物预期的表面密度有很大不同。当 PPD 处于“风驱动吸积”状态并保留垂直磁场时，表面密度的径向相关性在内部区域 <1-10 au 中可能为正。即使在磁流体动力学湍流水平非常低的情况下，质量吸积率也与观测结果一致。表面密度的这种正径向斜率对行星的形成产生了很大的影响，因为（i）它抑制了向内漂移甚至导致卵石/巨石大小的固体向外漂移，并且（ii）它还使原行星的向内I型迁移减慢甚至逆转。结论：我们计算的 PPD 的多样性应该会产生各种各样的系外行星系统。
Aims: We investigate the evolution of protoplanetary discs (PPDs hereafter) with magnetically driven disc winds and viscous heating. Methods: We consider an initially massive disc with ~0.1 Msun to track the evolution from the early stage of PPDs. We solve the time evolution of surface density and temperature by taking into account viscous heating and the loss of the mass and the angular momentum by the disc winds within the framework of a standard alpha model for accretion discs. Our model parameters, turbulent viscosity, disc wind mass loss, and disc wind torque, which are adopted from local magnetohydrodynamical simulations and constrained by the global energetics of the gravitational accretion, largely depends on the physical condition of PPDs, particularly on the evolution of the vertical magnetic flux in weakly ionized PPDs. Results: Although there are still uncertainties concerning the evolution of the vertical magnetic flux remaining, surface densities show a large variety, depending on the combination of these three parameters, some of which are very different from the surface density expected from the standard accretion. When a PPD is in a "wind-driven accretion" state with the preserved vertical magnetic field, the radial dependence of the surface density can be positive in the inner region <1-10 au. The mass accretion rates are consistent with observations, even in the very low level of magnetohydrodynamical turbulence. Such a positive radial slope of the surface density gives a great impact on planet formation because (i)it inhibits the inward drift or even results in the outward drift of pebble/boulder-sized solid bodies, and (ii) it also makes the inward type-I migration of proto-planets slower or even reversed. Conclusions: The variety of our calculated PPDs should yield a wide variety of exoplanet systems.