The Effect of a Strong Pressure Bump in the Sun’s Natal Disk: Terrestrial Planet Formation via Planetesimal Accretion Rather than Pebble Accretion
The Effect of a Strong Pressure Bump in the Sun’s Natal Disk: Terrestrial Planet Formation via Planetesimal Accretion Rather than Pebble Accretion
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太阳本命盘中强烈压力冲击的影响：通过星子吸积而不是卵石吸积形成类地行星
DOI：
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发表时间：
2021
影响因子：
4.9
通讯作者：
R. Dasgupta
中科院分区：
文献类型：
--
作者：
A. Izidoro;B. Bitsch;R. Dasgupta
碳质和非碳质陨石的质量无关同位素异常显示出明显的二分性，表明太阳系内外的有效分离。观测表明，原行星盘中毫米大小的鹅卵石分布中的环状结构很常见。这些构造通常与漂移的鹅卵石被气盘中的局部压力极大值捕获有关。类似的结构也可能存在于太阳的出生盘中，这可以自然地解释陨石/行星的同位素二分法。在这里，我们测试了外盘(例如，∼5 Au)中的强烈压力碰撞对内太阳系形成的影响。我们模拟尘埃凝结和演化、小行星的形成，以及通过小行星和卵石吸积的胚胎生长。我们的结果表明，地球胚胎是通过行星微小的吸积作用而不是卵石吸积作用形成的。在我们的模型中，鹅卵石的径向漂移促进了小行星的形成。然而，一旦压力凸起形成，内盘中的鹅卵石就会通过漂移丢失，然后它们才能被生长在⪆1 Au的胚胎有效地吸收。∼0.5Au-1.0Au内的胚胎生长相对较快，能更有效地附着鹅卵石。然而，这些胚胎生长到更大的质量，因此它们应该向内迁移，这与当前的太阳系不一致。因此，类地行星很可能是从月球的巨大撞击中吸积而来的，形成了大约与火星质量相当的行星胚胎，形成于⪆1.0Au附近。最后，我们的模拟产生了地球区域小行星的陡峭的径向质量分布，这与表明小行星带出生时质量较低的形成模型定性地一致。
Mass-independent isotopic anomalies of carbonaceous and noncarbonaceous meteorites show a clear dichotomy suggesting an efficient separation of the inner and outer solar system. Observations show that ring-like structures in the distribution of millimeter-sized pebbles in protoplanetary disks are common. These structures are often associated with drifting pebbles being trapped by local pressure maxima in the gas disk. Similar structures may also have existed in the Sun’s natal disk, which could naturally explain the meteorite/planetary isotopic dichotomy. Here, we test the effects of a strong pressure bump in the outer disk (e.g., ∼5 au) on the formation of the inner solar system. We model dust coagulation and evolution, planetesimal formation, as well as embryo growth via planetesimal and pebble accretion. Our results show that terrestrial embryos formed via planetesimal accretion rather than pebble accretion. In our model, the radial drift of pebbles fosters planetesimal formation. However, once a pressure bump forms, pebbles in the inner disk are lost via drift before they can be efficiently accreted by embryos growing at ⪆1 au. Embryos inside ∼0.5–1.0 au grow relatively faster and can accrete pebbles more efficiently. However, these same embryos grow to larger masses so they should migrate inwards substantially, which is inconsistent with the current solar system. Therefore, terrestrial planets most likely accreted from giant impacts of Moon to roughly Mars-mass planetary embryos formed around ⪆1.0 au. Finally, our simulations produce a steep radial mass distribution of planetesimals in the terrestrial region, which is qualitatively aligned with formation models suggesting that the asteroid belt was born low mass.
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影响因子：
64.8
作者：
D. Segura-Cox;A. Schmiedeke;J. Pineda;I. Stephens;M. Fern'andez-L'opez;L. Looney;P. Caselli;
通讯作者：
D. Segura-Cox;A. Schmiedeke;J. Pineda;I. Stephens;M. Fern'andez-L'opez;L. Looney;P. Caselli;
影响因子：
6.5
作者：
Ł. Tychoniec;C. Manara;G. Rosotti;E. V. van Dishoeck;A. Cridland;T. Hsieh;N. Murillo;D. Segura-Cox-D.-Se
通讯作者：
Ł. Tychoniec;C. Manara;G. Rosotti;E. V. van Dishoeck;A. Cridland;T. Hsieh;N. Murillo;D. Segura-Cox-D.-Se
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
影响因子：
6.5
作者：
M. Flock;J. P. Ruge;N. Dzyurkevich;T. Henning;H. Klahr;S. Wolf
通讯作者：
M. Flock;J. P. Ruge;N. Dzyurkevich;T. Henning;H. Klahr;S. Wolf
影响因子：
7.9
作者：
Andrews, Sean M.;Huang, Jane;Ricci, Luca
通讯作者：
Ricci, Luca