IN SITU ACCRETION OF HYDROGEN-RICH ATMOSPHERES ON SHORT-PERIOD SUPER-EARTHS: IMPLICATIONS FOR THE KEPLER-11 PLANETS

被引:138
|
作者
Ikoma, M. [1 ,2 ]
Hori, Y. [3 ]
机构
[1] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan
[2] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan
[3] Natl Inst Nat Sci, Natl Astron Observ Japan, Div Theoret Astron, Mitaka, Tokyo 1818588, Japan
来源
ASTROPHYSICAL JOURNAL | 2012年 / 753卷 / 01期
关键词
planets and satellites: formation; MASS-RADIUS RELATIONSHIPS; GAS GIANT FORMATION; SOLID EXOPLANETS; MEAN OPACITIES; HOT JUPITERS; EVOLUTION; ENVELOPES; NEPTUNES; STARS; CORES;
D O I
10.1088/0004-637X/753/1/66
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Motivated by recent discoveries of low-density super-Earths with short orbital periods, we have investigated in situ accretion of H-He atmospheres on rocky bodies embedded in dissipating warm disks, by simulating quasi-static evolution of atmospheres that connect to the ambient disk. We have found that the atmospheric evolution has two distinctly different outcomes, depending on the rocky body's mass: while the atmospheres on massive rocky bodies undergo runaway disk-gas accretion, those on light rocky bodies undergo significant erosion during disk dispersal. In the atmospheric erosion, the heat content of the rocky body that was previously neglected plays an important role. We have also realized that the atmospheric mass is rather sensitive to disk temperature in the mass range of interest in this study. Our theory is applied to recently detected super-Earths orbiting Kepler-11 to examine the possibility that the planets are rock-dominated ones with relatively thick H-He atmospheres. The application suggests that the in situ formation of the relatively thick H-He atmospheres inferred by structure modeling is possible only under restricted conditions, namely, relatively slow disk dissipation and/or cool environments. This study demonstrates that low-density super-Earths provide important clues to understanding of planetary accretion and disk evolution.
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页数:6
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