Highly inclined and eccentric massive planets - I. Planet-disc interactions
Highly inclined and eccentric massive planets - I. Planet-disc interactions
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高度倾斜和偏心的大质量行星 - I. 行星盘相互作用
DOI：
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发表时间：
2013
期刊：
影响因子：
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通讯作者：
E. Lega
中科院分区：
文献类型：
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作者：
B. Bitsch;A. Crida;Anne;E. Lega
在太阳系中，行星相对于太阳赤道平面的倾角很小，但有证据表明，在太阳系外的系统中，倾角可能非常大。这种自旋-轨道错位是出乎意料的，因为行星形成于原行星盘中，据推测与恒星自旋对齐。行星与行星之间的相互作用被认为会导致相互倾斜，但原行星盘的影响仍然未知。因此，我们调查行星盘的相互作用，行星以上1M_JUP。我们检查的倾角i，偏心率e，和质量M_p的行星的影响。我们进行3D数值模拟的原行星盘嵌入高质量的行星。给出了i和e作为i、e和M_p的函数的阻尼公式，并与数值结果进行了拟合。对于高度倾斜的大质量行星，差距的开口减小，i的阻尼发生在10^-4度/年M_disc/（0.01 M_星星）量级的时间尺度上，e的阻尼发生在更小的时间尺度上。当小行星质量（<5M_Jup）的倾角总是被阻尼时，大行星质量和大i可以与圆盘一起经历Kozai循环。这些Kozai周期在时间上是阻尼的。偏心率一般是阻尼的，除了非常大质量的行星（M_p = 5M_Jup），偏心率可以增加低倾角。动力学趋向于最终状态：行星最终处于中平面，然后随着时间的推移，由于与圆盘的相互作用，它们的偏心率会增加。与盘的相互作用导致高质量行星散射事件后i和e的阻尼。如果i被充分地减小，则由于与盘的相互作用，偏心率可以被泵送。如果行星被分散到高倾角，它可能会经历一个Kozai循环，这使得很难预测行星的确切运动及其轨道参数。
In the Solar System, planets have a small inclination with respect to the equatorial plane of the Sun, but there is evidence that in extrasolar systems the inclination can be very high. This spin-orbit misalignment is unexpected, as planets form in a protoplanetary disc supposedly aligned with the stellar spin. Planet-planet interactions are supposed to lead to a mutual inclination, but the effects of the protoplanetary disc are still unknown. We investigate therefore planet-disc interactions for planets above 1M_Jup. We check the influence of the inclination i, eccentricity e, and mass M_p of the planet. We perform 3D numerical simulations of protoplanetary discs with embedded high-mass planets. We provide damping formulae for i and e as a function of i, e, and M_p that fit the numerical data. For highly inclined massive planets, the gap opening is reduced, and the damping of i occurs on time-scales of the order of 10^-4 deg/yr M_disc/(0.01 M_star) with the damping of e on a smaller time-scale. While the inclination of low planetary masses (<5M_Jup) is always damped, large planetary masses with large i can undergo a Kozai-cycle with the disc. These Kozai-cycles are damped in time. Eccentricity is generally damped, except for very massive planets (M_p = 5M_Jup) where eccentricity can increase for low inclinations. The dynamics tends to a final state: planets end up in midplane and can then, over time, increase their eccentricity as a result of interactions with the disc. The interactions with the disc lead to damping of i and e after a scattering event of high-mass planets. If i is sufficiently reduced, the eccentricity can be pumped up because of interactions with the disc. If the planet is scattered to high inclination, it can undergo a Kozai-cycle with the disc that makes it hard to predict the exact movement of the planet and its orbital parameters at the dispersal of the disc.