Transitional disk archeology from exoplanet population synthesis

Abstract

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.

arXiv comment5 pages, accepted to the Proceedings IAU Symposium No. 345, 2019 conference book

References in corpus (4)

• Debris Disks: Structure, Composition, and Variability
• Homogeneous Analysis of the Dust Morphology of Transition Disks Observed with ALMA: Investigating dust trapping and the origin of the cavities
• Migration-driven diversity of super-Earth compositions
• The Diversity of Planetary Systems Architectures: Contrasting Theory with Observations

Cited by in corpus (1)

• The New Generation Planetary Population Synthesis (NGPPS). V. Predetermination of planet types in global core accretion models