Computer Science
Scientific paper
Oct 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epsc.conf.1280g&link_type=abstract
EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France. http://meetings.copernicus.org/epsc-dps2011, p.1280
Computer Science
Scientific paper
Sufficiently ionized sections of protoplanetary discs are thought to be in a turbulent state powered by the magnetorotational instability (MRI). Previous work [1, 2] has shown that a swarm of planetesimals embedded in a fully turbulent disc is subject to strong excitation of its velocity dispersion, along with significant radial diffusion of semi-major axes. Implications include the collisional destruction of small bodies, and levels of large-scale spread of populations incompatible with the observed distribution within the asteroid belt. The picture remains unchanged when vertical stratification is included [3], and we suggest that planetesimal growth via mutual collisions cannot occur in a fully MRI-active disc. By contrast, a magnetically dead zone may provide a safe haven in which km-sized planetesimals can avoid mutual destruction [3]. First preliminary results from new simulations indicate that this finding also holds for increased disc masses, i.e., for more extended dead zones.
Gressel Oliver
Nelson Richard P.
Turner Neal James
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