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Dead zones and the diversity of exoplanetary systems

Published online by Cambridge University Press:  10 November 2011

Yasuhiro Hasegawa  and
Ralph E. Pudritz
Yasuhiro Hasegawa
Affiliation:
Department of Physics and Astronomy McMaster University, Hamilton ON, L8S 4M1, Canada email: [email protected]
Ralph E. Pudritz
Affiliation:
Department of Physics and Astronomy McMaster University, Hamilton ON, L8S 4M1, Canada email: [email protected] Origins Institute, McMaster University, Hamilton ON, L8S 4M1, Canada email: [email protected]
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Abstract

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Planetary migration provides a theoretical basis for the observed diversity of exoplanetary systems. We demonstrate that dust settling - an inescapable feature of disk evolution - gives even more rapid type I migration by up to a factor of about 2 than occurs in disks with fully mixed dust. On the other hand, type II migration becomes slower by a factor of 2 due to dust settling. This even more problematic type I migration can be resolved by the presence of a dead zone; the inner, high density region of a disk which features a low level of turbulence. We show that enhanced dust settling in the dead zone leaves a dusty wall at its outer edge. Back-heating of the dead zone by this wall produces a positive radial gradient for the disk temperature, which acts as a barrier for type I migration.

Keywords

accretionaccretion disksradiative transferturbulenceplanetary systems: protoplanetary disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S276: The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution , October 2010 , pp. 430 - 431
Copyright
Copyright © International Astronomical Union 2011

References

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