Anders Johansen
Professor
The role of pebble fragmentation in planetesimal formation II. Numerical simulations
Author
Summary, in English
Some scenarios for planetesimal formation go through a phase of collapse of gravitationally bound clouds of millimeter- to centimeter-size pebbles. Such clouds can form, for example, through the streaming instability in protoplanetary disks. We model the collapse process with a statistical model to obtain the internal structure of planetesimals with solid radii between 10 and 1000 km. During the collapse, pebbles collide, and depending on their relative speeds, collisions have different outcomes. A mixture of particle sizes inside a planetesimal leads to better packing capabilities and higher densities. In this paper we apply results from new laboratory experiments of dust aggregate collisions (presented in a companion paper) to model collision outcomes. We find that the internal structure of a planetesimal is strongly dependent on both its mass and the applied fragmentation model. Low-mass planetesimals have no/few fragmenting pebble collisions in the collapse phase and end up as porous pebble piles. The number of fragmenting collisions increases with increasing cloud mass, resulting in wider particle size distributions and higher density. The collapse is nevertheless "cold" in the sense that collision speeds are damped by the high collision frequency. This ensures that a significant fraction of large pebbles survive the collapse in all but the most massive clouds. Our results are in broad agreement with the observed increase in density of Kuiper Belt objects with increasing size, as exemplified by the recent characterization of the highly porous comet 67P/Churyumov-Gerasimenko.
Department/s
- Lund Observatory - Has been reorganised
Publishing year
2017-01-20
Language
English
Publication/Series
Astrophysical Journal
Volume
835
Issue
1
Document type
Journal article
Publisher
American Astronomical Society
Topic
- Astronomy, Astrophysics and Cosmology
Keywords
- methods: analytical
- methods: numerical
- planets and satellites: formation
Status
Published
ISBN/ISSN/Other
- ISSN: 0004-637X