Rapid Formation of Jupiter and Wide-orbit Exoplanets in Disks with Pressure Bumps
Rapid Formation of Jupiter and Wide-orbit Exoplanets in Disks with Pressure Bumps
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木星和宽轨道系外行星在带有压力凸点的圆盘中快速形成
DOI：
10.3847/1538-4357/abfaa4
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发表时间：
2021
期刊：
影响因子：
--
通讯作者：
J. Chambers
中科院分区：
文献类型：
--
作者：
J. Chambers
在原行星盘的寿命内形成气体巨行星是一个挑战，特别是远离星星。巨行星核心快速形成的一个很有希望的模型是卵石吸积，其中相遇过程中的气体阻力导致高吸积率。大多数卵石吸积模型考虑的是具有单调径向压力分布的圆盘。这就造成了卵石的不断向内流动和低效的生长。在这里，我们研究行星形成的磁盘与多个，内在的压力颠簸。在外盘中，鹅卵石被困在这些凸起附近，允许在合适的条件下快速生长。在内盘中，由于向内的气体平流速度太高，可能不存在卵石陷阱。这里的鹅卵石被迅速清除。在外盘，生长对初始行星质量和湍流强度非常敏感。这是因为湍流密度波动提高了行星的离心率，增加了行星-卵石的相对速度。超过距离依赖的临界质量的行星种子在0.5- 300万年内增长到木星质量，在0.03太阳质量的盘中至少增长到60 Au。较小的天体保持在它们的初始质量附近，导致生长结果的尖锐二分法。对于湍流α = 1 e-4，在9和75 Au处的临界质量分别为1 e-4 M和1 e-3 M。圆盘中的压力隆起可以解释巨行星和柯伊伯带天体之间的巨大质量差异，以及某些系统中宽轨道行星的存在。
The formation of gas-giant planets within the lifetime of a protoplanetary disk is challenging especially far from a star. A promising model for the rapid formation of giant-planet cores is pebble accretion in which gas drag during encounters leads to high accretion rates. Most models of pebble accretion consider disks with a monotonic, radial pressure profile. This causes a continuous inward flux of pebbles and inefficient growth. Here we examine planet formation in a disk with multiple, intrinsic pressure bumps. In the outer disk, pebbles become trapped near these bumps allowing rapid growth under suitable conditions. In the inner disk, pebble traps may not exist because the inward gas advection velocity is too high. Pebbles here are rapidly removed. In the outer disk, growth is very sensitive to the initial planet mass and the strength of turbulence. This is because turbulent density fluctuations raise planetary eccentricities, increasing the planet-pebble relative velocity. Planetary seeds above a distance-dependent critical mass grow to a Jupiter mass in 0.5–3 Myr out to at least 60 au in a 0.03 solar-mass disk. Smaller bodies remain near their initial mass, leading to a sharp dichotomy in growth outcomes. For turbulent α = 1e-4, the critical masses are 1e-4M ⊕ and 1e-3M ⊕ at 9 and 75 au, respectively. Pressure bumps in disks may explain the large mass difference between the giant planets and Kuiper Belt objects, and also the existence of wide-orbit planets in some systems.
DOI：
10.3847/2041-8213/aaf742
发表时间：
2018-12
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
C. Dullemond;T. Birnstiel;Jane Huang;N. Kurtovic;S. Andrews;V. Guzm'an;L. P'erez;A. Isella;Zhaohuan Zhu;M. Benisty;D. Wilner;X. Bai;J. Carpenter;Shangjia Zhang;L. Ricci
通讯作者：
C. Dullemond;T. Birnstiel;Jane Huang;N. Kurtovic;S. Andrews;V. Guzm'an;L. P'erez;A. Isella;Zhaohuan Zhu;M. Benisty;D. Wilner;X. Bai;J. Carpenter;Shangjia Zhang;L. Ricci
DOI：
10.3847/1538-4365/aaceae
发表时间：
2018-06
期刊：
The Astrophysical Journal Supplement Series
影响因子：
--
作者：
Ł. Tychoniec;J. Tobin;A. Karska;C. Chandler;M. Dunham;R. Harris;K. Kratter;Zhi-Yun Li;L. Looney;C. Melis;L. P'erez;S. Sadavoy;D. Segura-Cox;E. V. van Dishoeck
通讯作者：
Ł. Tychoniec;J. Tobin;A. Karska;C. Chandler;M. Dunham;R. Harris;K. Kratter;Zhi-Yun Li;L. Looney;C. Melis;L. P'erez;S. Sadavoy;D. Segura-Cox;E. V. van Dishoeck
影响因子：
7.9
作者：
Andrews, Sean M.;Huang, Jane;Ricci, Luca
通讯作者：
Ricci, Luca