Forming Diverse Super-Earth Systems In Situ

被引:24
|
作者
MacDonald, Mariah G. [1 ]
Dawson, Rebekah I. [1 ]
Morrison, Sarah J. [1 ,2 ]
Lee, Eve J. [3 ,4 ]
Khandelwal, Arjun [5 ]
机构
[1] Penn State Univ, Dept Astron & Astrophys, Ctr Exoplanets & Habitable Worlds, 525 Davey Lab, University Pk, PA 16802 USA
[2] Missouri State Univ, Dept Phys Astron & Mat Sci, Springfield, MO 65897 USA
[3] McGill Univ, Dept Phys, 3550 Rue Univ, Montreal, PQ H3A 2T8, Canada
[4] McGill Univ, McGill Space Inst, 3550 Rue Univ, Montreal, PQ H3A 2T8, Canada
[5] Haverford Coll, 370 Lancaster Ave, Haverford, PA 19041 USA
来源
ASTROPHYSICAL JOURNAL | 2020年 / 891卷 / 01期
基金
美国国家科学基金会;
关键词
Exoplanet dynamics; Exoplanet formation; Exoplanet astronomy; Exoplanets; STABILITY; MASS; EVOLUTION; NEPTUNES; GROWTH; SOLAR;
D O I
10.3847/1538-4357/ab6f04
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Super-Earths and mini-Neptunes exhibit great diversity in their compositional and orbital properties. Their bulk densities span a large range, from those dense enough to be purely rocky to those needing a substantial contribution from volatiles to their volumes. Their orbital configurations range from compact, circular multitransiting systems like Kepler-11 to systems like our solar system's terrestrial planets with wider spacings and modest but significant eccentricities and mutual inclinations. Here we investigate whether a continuum of formation conditions resulting from variation in the amount of solids available in the inner disk can account for the diversity of orbital and compositional properties observed for super-Earths, including the apparent dichotomy between single and multitransiting systems. We simulate in situ formation of super-Earths via giant impacts and compare to the observed Kepler sample. We find that intrinsic variations among disks in the amount of solids available for in situ formation can account for the orbital and compositional diversity observed among Kepler's transiting planets. Our simulations can account for the planets' distributions of orbital period ratios, transit duration ratios, and transit multiplicity; higher eccentricities for planets in single transiting systems than for those in multitransiting systems; smaller eccentricities for larger planets; scatter in the mass-radius relation, including lower densities for planets with masses measured with transit timing variations instead of with radial velocity; and similarities in planets' sizes and spacings within each system. Our findings support the theory that variation among super-Earth and mini-Neptune properties is primarily locked in by different in situ formation conditions, rather than arising stochastically through subsequent evolution.
引用
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页数:14
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