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Disk Inhomogeneities and the Origins of Planetary System Architectures and Observational Properties

Published online by Cambridge University Press:  06 January 2014

Yasuhiro Hasegawa  and
Ralph E. Pudritz
Yasuhiro Hasegawa
Affiliation:
EACOA fellow, Institute of Astronomy and Astrophysics, Academia Sinica (ASIAA), Taipei 10641, Taiwan email: [email protected]
Ralph E. Pudritz
Affiliation:
Department of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1, Canada Origins Institute, McMaster University, Hamilton, ON L8S 4M1, Canada email: [email protected]
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Abstract

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Recent high-resolution observations show that protoplanetary disks have various kinds of structural properties or inhomogeneities. These are the consequence of a mixture of a number of physical and chemical processes taking place in the disks. Here, we discuss the results of our comprehensive investigations on how disk inhomogeneities affect planetary migration. We demonstrate that disk inhomogeneities give rise to planet traps - specific sites in protoplanetary disks at which rapid type I migration is halted. We show that up to three types of traps (heat transitions, ice lines and dead zones) can exist in a single disk, and that they move differently as the disk accretion rate decreases with time. We also demonstrate that the position of planet traps strongly depends on stellar masses and disk accretion rates. This indicates that host stars establish preferred (initial) scales of their planetary systems. Finally, we discuss the possible observational signatures of disk inhomogeneities.

Keywords

accretionaccretion disksradiative transferturbulence(stars:) planetary systems: formation(stars:) planetary systems: protoplanetary disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S299: Exploring the Formation and Evolution of Planetary Systems , June 2013 , pp. 190 - 193
Copyright
Copyright © International Astronomical Union 2013 

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