Planet formation in slightly inclined binary systems

Details Planet formation in slightly inclined binary systems Planet formation in slightly inclined binary systems

Jul 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epjwc..1605003x&link_type=abstract

Research, Science and Technology of Brown Dwarfs and Exoplanets: Proceedings of an International Conference held in Shangai on O

Computer Science

Scientific paper

One of the major problems of planet formation in close binary systems, such as α Centauri AB, is the formation of planetary embryos or cores by mutual accretion of km-sized planetesimals. In this contribution, we test the planetesimal accretion in such close binary systems but with small inclinations iB = 0.1-10° between the binary orbital plane and the gas disk plane. Compared to previous studies (coplanar case with iB = 0), we find that (1) planetesimal disk is stratified in the vertical direction and planetesimals are redistributed on different orbit groups with respect to their sizes, thus (2) collisions between similar-sized bodies dominate, leading to low dV and favoring planetesimal accretion (3) the planetesimal collision timescale at 1-2 AU is estimated as: T ˜ (1 + 100iB) × 103 yrs, where 0 ≤ iB ≤ 10°. As a conclusion, although planetesimal accretion are much more favored in slightly inclined binary systems, it is significantly less efficient and slowed-down as compared to the single-star case.

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