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Protostellar Disks, Planet Traps, and the Origins of Exoplanetary Systems

Published online by Cambridge University Press:  06 January 2014

Ralph E. Pudritz  and
Yasuhiro Hasegawa
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]
Yasuhiro Hasegawa
Affiliation:
EACOA fellow, Institute of Astronomy and Astrophysics, Academia Sinica (ASIAA), Taipei 10641, Taiwan email: [email protected]
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Abstract

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The mass-semimajor axis diagram for exoplanets is populated by at least three distinct planetary populations: hot Jupiters at small orbital radii, more massive Jovian planets gathered at about 1 AU, and a rapidly growing population of SuperEarths at short periods. Our work shows that low mass and rapidly migrating planetary cores get trapped at disk inhomogeneities, where strong density or thermal gradients exist (namely dead zone boundaries, ice lines, and disk heating transition regions). Planet growth and movement occur at rates dictated by planetary accretion, and the slow radial inward motion of the traps due to falling disk accretion rates during disk evolution. By combining the theory of traps in evolving disks with standard ideas about how protoplanets accrete, we develop evolutionary tracks of how planets evolve in the mass- semimajor axis diagram. Our models account for the planetary “pile-up” at 1AU, the origin of SuperEarths and hot Jupiters, and the relative scarcity of Jovian planets at large distances.

Keywords

accretion disks(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. 365 - 369
Copyright
Copyright © International Astronomical Union 2013 

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