Other
Scientific paper
Sep 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ess.....2.3402m&link_type=abstract
American Astronomical Society, ESS meeting #2, #34.02
Other
Scientific paper
We study the stability of planets in the mean-motion resonances with numerical simulations.
Nowadays, about 550 planets and 1235 KOI candidates are observed. There are 8 systems and 158 candidate systems that are composed of multi super-Earths or Neptunes.
Most of systems are not in mean-motion resonances.
Numerical works suggest protoplanets migrate toward their central stars due to the interaction with the gas disk. Migration is stopped when a protoplanet arrives at the inner edge of the gas disk.
Protoplanets are captured at the locations of mean-motion resonances near the inner edge (Terquem & Papaloizou 2007). Normally, the resonant systems are stable longer than the system age.
Ogihara & Ida (2009) performed N-body simulations of planetary accretion in the case of weaker type I migration than the linear value. In such a case, planets become unstable after the gas depletion. Then final configure of planets are in large orbital separations and not in the mean-motion resonances.
There are differences in the configuration of planetary systems. A question arises which parameter is most responsible to make systems offset from the resonances. So we calculate the stability time of resonant systems changing parameters. We put on innermost planet at 0.1AU and put the other planets on m+1:m resonant orbits.
We find that when the number of planets becomes some value, the stability time of resonant system decreases rapidly.
With a fixed mass of planets, this critical number is smaller as the orbital separation, which is normalized by Hill radius becomes narrower. With fixed orbital separation, the critical number is smaller as the planetary mass gets smaller.
Exopanet systems whose planets are not in resonances is thought to be formed by the scenario that planets over critical number are trapped in resonances and these planets cause orbital instability after gas depletion.
Ida Shigeru
Matsumoto Yuji
Nagasawa Michiyasu
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