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Transitional disk archeology from exoplanet population synthesis

Published online by Cambridge University Press:  13 January 2020

Germán Chaparro Molano ,
Frank Bautista  and
Yamila Miguel
Germán Chaparro Molano
Affiliation:
Vicerrectoría de Investigación, Universidad ECCI, Bogotá, Colombia, email: [email protected]
Frank Bautista
Affiliation:
Departamento de Física, Universidad Nacional de Colombia, Bogotá, Colombia, email: [email protected]
Yamila Miguel
Affiliation:
Sterrewacht Leiden, Leiden University, Leiden, The Netherlands
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Abstract

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Increasingly better observations of resolved protoplanetary disks show a wide range of conditions in which planets can be formed. Many transitional disks show gaps in their radial density structure, which are usually interpreted as signatures of planets. It has also been suggested that observed inhomogeneities in transitional disks are indicative of dust traps which may help the process of planet formation. However, it is yet to be seen if the configuration of fully evolved exoplanetary systems can yield information about the later stages of their primordial disks. We use synthetic exoplanet population data from Monte Carlo simulations of systems forming under different density perturbation conditions, which are based on current observations of transitional disks. The simulations use a core instability, oligarchic growth, dust trap analytical model that has been benchmarked against exoplanetary populations.

Keywords

planetary systems: formationprotoplanetary disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S345: Origins: From the Protosun to the First Steps of Life , August 2018 , pp. 152 - 155
Copyright
© International Astronomical Union 2020 

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