Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ess.....2.1605i&link_type=abstract
American Astronomical Society, ESS meeting #2, #16.05
Astronomy and Astrophysics
Astronomy
Scientific paper
We have studied effects of dynamical interactions between planets/embryos (eccentricity excitation and ejection due to close scattering, merging, and resonant trapping) on mass-semimajor axis-eccentricity distributions and frequency of extrasolar giant planets and super-Earths, using our sequential planet formation model with newly added the effects of the dynamical interactions.
Our model clearly reproduces dependences of eccentricity distributions on planetary mass or semimajor axis for giant planets that are found by radial velocity surveys, while the semimajor axis distribution of gas giants is not fully reproduced, which suggests some important physical processes (e.g., migration trap) are missing in the calculations. We also found that distant jupiters on nearly circular orbits, which are observed by direct imaging, are formed by scattering of cores and eccentricity damping followed by runaway gas accretion that is induced by very low planetesimal accretion rate in the distant regions. The scattering also produces a large population of free floating planets, which are detected by gravitational microlensing.
Our model produces a large population of close-in super-Earths. We will discuss comparison with radial velocity and Kepler data. We found that in most massive disks, super-Earths do not survive scattering by gas giants, while they are not formed in least massive disks. Close-in super-Earths are formed in moderately massive disks, if type I migration is halted near disk inner edge. We also found that close-in super-Earths are mostly rocky, while they tend to be icy around M dwarfs.
Ida Shigeru
Lin Doug N. C.
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