Planetesimal dynamics in hydromagnetic turbulence

Details Planetesimal dynamics in hydromagnetic turbulence Planetesimal dynamics in hydromagnetic turbulence

Nov 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..276..424g&link_type=abstract

The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution, Proceedings of the International Astronomi

Astronomy and Astrophysics

Astrophysics

Accretion Disks, Mhd, Methods: Numerical, Planetary Systems: Formation, Planetary Systems: Protoplanetary Disks

Scientific paper

Planet formation theory is founded on the concept of dust coagulation and subsequent growth into planetesimals. This process is by no means an isolated one, but possibly happens in a turbulent nebula. It is therefore crucial to understand how particles of different sizes are affected by their gaseous environment via stochastic forcing and aerodynamic damping. We here report on the effects of magneto-rotational (MRI) turbulence in the presence of non-uniform ionisation leading to the formation of a magnetically inactive dead-zone. While we find that collisional growth is impeded by fully-active MRI, it may be possible within a dead-zone.

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