Growth efficiency of dust aggregates through collisions with high mass ratios⋆
Planetary Exploration Research Center, Chiba Institute of
2-17-1 Tsudanuma, Narashino,
2 Institute of Low Temperature Science, Hokkaido University, 060-0819 Sapporo, Japan
3 Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Meguro-ku, 152-8511 Tokyo, Japan
4 Department of Physics, Nagoya University, Nagoya, 464-8602 Aichi, Japan
5 Nagano City Museum, Hachimanpara Historical Park Ojimada-machi, 381-2212 Nagano, Japan
6 Graduate School of Science, Kobe University, c/o CPS (Center for Planetary Science), Chuo-ku Minatojima Minamimachi 7-1-48, 650-0047 Kobe, Japan
7 CPS (Center for Planetary Science), Kobe University, Chuo-ku Minatojima Minamimachi 7-1-48, 650-0047 Kobe, Japan
Accepted: 5 September 2013
Context. Collisional growth of dust aggregates is an essential process in forming planetesimals in protoplanetary disks, but disruption through high-velocity collisions (disruption barrier) could prohibit the dust growth. Mass transfer through very different-sized collisions has been suggested as a way to circumvent the disruption barrier.
Aims. We examine how the collisional growth efficiency of dust aggregates with different impact parameters depends on the size and the mass ratio of colliding aggregates.
Methods. We used an N-body code to numerically simulate the collisions of different-sized aggregates.
Results. Our results show that high values for the impact parameter are important and that the growth efficiency averaged over the impact parameter does not depend on the aggregate size, although the growth efficiency for nearly head-on collisions increases with size. We also find that the averaged growth efficiency tends to increase with increasing mass ratio of colliding aggregates. However, the critical collision velocity, above which the growth efficiency becomes negative, does not strongly depend on the mass ratio. These results indicate that icy dust can grow through high-velocity offset collisions at several tens of m s-1, the maximum collision velocity experienced in protoplanetary disks, whereas it is still difficult for silicate dust to grow in protoplanetary disks.
Key words: planets and satellites: formation / protoplanetary disks / methods: numerical
A complete set of our numerical results is available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/559/A62
© ESO, 2013