Transitional disk archeology from exoplanet population synthesis

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 inho...

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Bibliographic Details
Published in:Proceedings of the International Astronomical Union 2018-08, Vol.14 (S345), p.152-155
Main Authors: Chaparro Molano, Germán, Bautista, Frank, Miguel, Yamila
Format: Article
Language:English
Subjects:
Accretion disks
Archaeology
Astronomy
Computer simulation
Contributed Papers
Density
Dust
Extrasolar planets
Perturbation
Planet formation
Planetary systems
Protoplanets
Stability analysis
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Summary: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.
ISSN:1743-9213
1743-9221
DOI:10.1017/S1743921319001662