论文标题
3D恒星辐射的积聚磁盘中散开行星的迁移
Migration of gap-opening planets in 3D stellar-irradiated accretion disks
论文作者
论文摘要
语境。中等分离的巨型行星的起源$ \ simeq $$ 1 $$ - $$ 10 $ au仍然不完全了解，因为对原星磁盘中II型迁移的数值研究通常可以预测太快的半毛轴轴的衰减。根据最近的2D模拟，如果外部间隙边缘因中央恒星的辐射加热并膨胀，可以放慢缝隙行星的内向迁移。 目标。在这里，我们研究了恒星照射如何减少磁盘驱动的扭矩并影响更现实的3D磁盘的迁移。 方法。使用3D流体动力模拟和辐射转移，我们研究了作用于嵌入被动加热积聚盘中的单个间隙开放的行星上的静态扭矩。 结果。我们的模拟证实，在辐照的外间隙边缘建立了温度反转，尺度高度的局部增加会降低负外部林金扭矩的幅度。但是，温度过量比2D模拟中的假设小，并且扭矩减小仅在特定参数中显着。对于粘度$α= 10^{ - 3} $，对于行星质量的总扭矩从$ 0.1 $ $ $ 0.7 $ $木星质量降低，最强的减少量为$ -0.17 $（暗示向外迁移）的Saturn-Mass Planet $ -0.17 $。对于木星质量行星，随着$α$的增加，扭矩的降低变得更强（当$α= 5 \ times10^{ - 3} $时，扭矩减半。 结论。我们得出的结论是，敞开的宽度和深度间隙的行星受到最大的扭矩修改，并且由于间隙边缘照明，它们的II型迁移可能会停滞不前。然后，我们认为降低扭矩可以帮助稳定形成的巨型行星的轨道，以$ \ gtrsim $$ 1 $ au。
Context. The origin of giant planets at moderate separations $\simeq$$1$$-$$10$ au is still not fully understood because numerical studies of Type II migration in protoplanetary disks often predict a decay of the semi-major axis that is too fast. According to recent 2D simulations, inward migration of a gap-opening planet can be slowed down or even reversed if the outer gap edge becomes heated by irradiation from the central star, and puffed up. Aims. Here we study how stellar irradiation reduces the disk-driven torque and affects migration in more realistic 3D disks. Methods. Using 3D hydrodynamic simulations with radiation transfer, we investigated the static torque acting on a single gap-opening planet embedded in a passively heated accretion disk. Results. Our simulations confirm that a temperature inversion is established at the irradiated outer gap edge and the local increase of the scale height reduces the magnitude of the negative outer Lindblad torque. However, the temperature excess is smaller than assumed in 2D simulations and the torque reduction only becomes prominent for specific parameters. For the viscosity $α=10^{-3}$, the total torque is reduced for planetary masses ranging from $0.1$ to $0.7$ Jupiter mass, with the strongest reduction being by a factor of $-0.17$ (implying outward migration) for a Saturn-mass planet. For a Jupiter-mass planet, the torque reduction becomes stronger with increasing $α$ (the torque is halved when $α=5\times10^{-3}$). Conclusions. We conclude that planets that open moderately wide and deep gaps are subject to the largest torque modifications and their Type II migration can be stalled due to gap edge illumination. We then argue that the torque reduction can help to stabilize the orbits of giant planets forming at $\gtrsim$$1$ au.
