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Effects of planetary mass accretion on the planets migration: the disk structures

Published online by Cambridge University Press:  05 January 2015

Ramiro Álvarez  and
Erick Nagel
Ramiro Álvarez
Affiliation:
Departamento de Astronomía, Universidad de Guanajuato, Guanajuato, Gto 36240, Mexico email: [email protected]
Erick Nagel
Affiliation:
Departamento de Astronomía, Universidad de Guanajuato, Guanajuato, Gto 36240, Mexico email: [email protected]
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Abstract

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We develop numerical tools to detect and quantify the mass and area for all structures of a protoplanetary disk with different optical depths. We consider two planets of 0.1 MJ. They are initially at 12.5 and 20 AU embedded in a viscous disk, where planetary mass accretion and migration are allowed. We find a gap region with optically thick streams, this region is characterized by an optically thin filling factor near to 1. Additionally, we generate the Spectral Energy Distribution of each structure of the disk considering silicate dust. Our tools are useful to identify the locations of structures and sub-structures as possible sites where the material is accumulated.

Keywords

planets and satellites: formationplanetary systems: protoplanetary diskstructure formationpre-transitional disktransitional disk
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S310: Complex Planetary Systems , July 2014 , pp. 212 - 213
Copyright
Copyright © International Astronomical Union 2014 

References

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