Evolution of Jovian planets in a self-gravitating planetesimal disk
Evolution of Jovian planets in a self-gravitating planetesimal disk
复制标题
DOI：
10.1051/0004-6361/201015601
复制
发表时间：
2011-04
影响因子：
6.5
通讯作者：
Jian Li;Li-Yong Zhou;Yi-sui Sun
中科院分区：
文献类型：
--
作者：
Jian Li;Li-Yong Zhou;Yi-sui Sun
目标。我们探索了嵌入在自引力行星盘中的四颗木星行星的轨道演化，以及原天王星和原海王星同时吸积小天体的情况。方法：研究方法。我们采用在GRAPE型专用计算机上运行的程序NBODY4对太阳系外的原始演化进行了数值模拟，其中考虑了太阳、木星四颗行星和大质量行星体的总引力。结果。原天王星和原海王星在其迁徙阶段没有明显的吸积，仅在地球质量的0.1量级。自引力盘可以在海王星以外的几个AU范围内向散射区提供新的小行星补充，导致海王星的径向位移比非自引力盘中的大。海王星目前的位置需要在∼35AU处有一个原始的行星小盘外缘。幸存的小行星的分布与观测到的柯伊伯带非常相似。
Aims. We explore the orbital evolution of the four Jovian planets embedded in a self-gravitating planetesimal disk, along with the simultaneous accretion of small bodies by proto-Uranus and proto-Neptune. Methods. We adopt the code NBODY4 running on the GRAPE-type special-purpose computer for numerically simulating the primordial evolution of the outer Solar System, where the total gravitational forces due to the Sun, the four Jovian planets, and the massive planetesimals are all taken into account. Results. There is no significant accretion of proto-Uranus and proto-Neptune during their migration stage, only on the order of 0.1 Earth mass. The self-gravitating disk can provide a new replenishment of planetesimals outside a few AU beyond Neptune into the scattering zone, resulting in larger radial displacement of Neptune than in the non-self-gravitating disk. The present location of Neptune requires an original planetesimal disk outer edge at ∼35 AU. The distribution of the surviving planetesimals is very similar to the observed Kuiper belt.