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Planet formation around intermediate mass stars

Published online by Cambridge University Press:  01 October 2007

Katherine A. Kretke ,
D. N. C. Lin  and
Neal J. Turner
Katherine A. Kretke
Affiliation:
Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA
D. N. C. Lin
Affiliation:
Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA Kavli Institute of Astronomy and Astrophysics, Peking University, Beijing, China
Neal J. Turner
Affiliation:
Jet Propulsion Lab, Pasadena, CA
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Abstract

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We present a mechanism by which gas giants form efficiently around intermediate mass stars. MRI-driven turbulence effectively drives angular momentum transport in regions of the disk with sufficiently high ionization fraction. In the inner regions of the disk, where the midplane temperature is above ∼1000K, thermal ionization effectively couples the disk to the magnetic field, providing a relatively large viscosity. A pressure maximum will develop outside of this region as the gaseous disk approaches a steady-state surface density profile, trapping migrating solid material. This rocky material will coagulate into planetesimals which grow rapidly until they reach isolation mass. Around intermediate mass stars, viscous heating will push the critical radius for thermal ionization of the midplane out to around 1 AU. This will increase the isolation mass for solid cores. Planets formed here may migrate inwards due to type II migration, but they will induce the formation of subsequent giant planets at the outer edge of the gap they have opened. In this manner, gas giants can form around intermediate mass stars at a few AU.

Keywords

planetary systems: formationprotoplanetary disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S249: Exoplanets: Detection, Formation and Dynamics , October 2007 , pp. 293 - 300
Copyright
Copyright © International Astronomical Union 2008

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