Planetesimal collisions in binary systems

We study the collisional evolution of kilometre-sized planetesimals in tight binary star systems to investigate whether accretion towards protoplanets can proceed despite the strong gravitational perturbations from the secondary star. The orbits of planetesimals are numerically integrated in two dim...

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Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society. Letters 2010-03, Vol.403 (1), p.L64-L68
Main Authors: Paardekooper, S.-J., Leinhardt, Z. M.
Format: Article
Language:English
Subjects:
planetary systems: protoplanetary discs
planets and satellites: formation
stars: individual: α Centauri
stars: individual: γ Cephei
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Summary:We study the collisional evolution of kilometre-sized planetesimals in tight binary star systems to investigate whether accretion towards protoplanets can proceed despite the strong gravitational perturbations from the secondary star. The orbits of planetesimals are numerically integrated in two dimensions under the influence of the two stars and gas drag. The masses and orbits of the planetesimals are allowed to evolve due to collisions with other planetesimals and accretion of collisional debris. In addition, the mass in debris can evolve due to planetesimal—planetesimal collisions and the creation of new planetesimals. We show that it is possible in principle for kilometre-sized planetesimals to grow by two orders of magnitude in size if the efficiency of planetesimal formation is relatively low. We discuss the limitations of our two-dimensional approach.
ISSN:1745-3925
1745-3933
DOI:10.1111/j.1745-3933.2010.00816.x