Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011acasn..52..355w&link_type=abstract
Acta Astronomica Sinica, vol. 52, no.4, p. 355-356
Astronomy and Astrophysics
Astronomy
Stars: Planetary System, Planets And Satellites: Formation, Celestial Mechanics, Planet-Disk Interactions, Methods: Numerical
Scientific paper
To date, more than 431 exoplanets have been detected since 1995, among them there are 45 multiple planetary systems. There are lots of differences between the solar system and the extrasolar planetary systems. We study several important factors and phases in the formation process of exoplanet system, including scattering process, mean motion resonance (MMR) capture, resonance crossing and the speed of type I migration for low-mass planets. Those processes will decide the final configurations of semi-major axes and eccentricities in the system and whether there are terrestrial and habitable planets in the system.
We mainly study three configurations: (1) Near-separatrix motion which is one of the properties of the multiple exoplanet systems. According to our research, during the formation process, planet scattering will lead to the near-separatrix motion which is common in exoplanet systems. (2) OGLE-06-109L system is an analog of the solar system especially the Jupiter-Saturn configuration in semi-major axes and eccentricities. So the two systems may undergo the same process. We study three possible reasons that can lead to this configuration: MMR capture during the smooth convergent migration, planetary scattering and MMR crossing during the divergent migration. They will lead to different properties of the final configuration of the system. After the resonance capture, two planets will be in MMR until some processes destroy it. Scattering process will excite the eccentricities of the planets and lead them into near-separatrix motion. Then the evolution period of the eccentricities of planets will be in the period of secular motion. Resonance crossing will also excite the eccentricities of planets. The evolution period of the eccentricities will be in the period of MMR which they just crossed. According to the present observational data, we can not decide which mechanism is the best one, but in the future they will be checked out. (3) We study the configuration of near 1:2:4 resonances (Laplace resonance) using HD40307 as an example. The three planets in the system are all massive terrestrial planets. We suggest that they all formed near the snow-line of the system and migrate to the locations where they are observed through type I migration. In order to form the configuration of near 1:2:4, the speed of type I migration may be one tenth of the linear analysis result. When they migrate to the locations close to the central star, the tidal effect from the star will lead them into the nominal locations. Finally, we study the distributions of the habitable planets and terrestrial planets in dwarf stars under the effect of the speed of type I migration. We use OGLE-06-109L as an example. Through our study on the type I migration and water content in planet, if we know the masses and the water contents of the habitable planets in the system, we will deduce the migration speeds during the formation processes and whether they have gone through merging process during the formation.
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