Planetary influence in the gap of a protoplanetary disk: structure formation and an application to V1247 Ori
Abstract
We present a set of hydrodynamical models of a planetary system embedded in a protoplanetary disk in order to extract the number of dust structures formed in the disk, their masses and sizes, within optical depth ranges τ≤0.5, 0.5<τ<2 and τ≥2. The study of the structures shows: (1) an increase in the number of planets implies an increase in the creation rate of massive structures; (2) a lower planetary mass accretion corresponds to slower time effects for optically thin structures; (3) an increase in the number of planets allows a faster evolution of the structures in the Hill radius for the different optical depth ranges of the inner planets. An ad-hoc simulation was run using the available information of the stellar system V1247 Ori, leading to a model of a planetary system which explains the SED and is consistent with interferometric observations of structures.
- Publication:
-
Revista Mexicana de Astronomia y Astrofisica
- Pub Date:
- October 2017
- Bibcode:
- 2017RMxAA..53..275A
- Keywords:
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- accretion;
- accretion disks;
- hydrodynamics;
- planets and satellites: formation;
- protoplanetary disks