The 8/5 resonance between TRAPPIST-1 innermost planets
Interactions between the planets with the protoplanetary gas disk produce migration, whose rates depend on the features of the gas-disk and the mass of the migrating planets. Due to the uncertainties in the estimations of masses of the TRAPPIST-1 planets, their migration rates are not well determine...
| Autores: | , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2021 |
| País: | Argentina |
| Institución: | Universidad Nacional de La Plata |
| Repositorio: | SEDICI (UNLP) |
| Idioma: | inglés |
| OAI Identifier: | oai:sedici.unlp.edu.ar:10915/165454 |
| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/165454 |
| Access Level: | acceso abierto |
| Palabra clave: | Ciencias Astronómicas planet-disk interactions protoplanetary disks celestial mechanics |
| Sumario: | Interactions between the planets with the protoplanetary gas disk produce migration, whose rates depend on the features of the gas-disk and the mass of the migrating planets. Due to the uncertainties in the estimations of masses of the TRAPPIST-1 planets, their migration rates are not well determined. In this work, we present A-body simulations including type-I migration, to reproduce the general configuration of the TRAPPIST- 1 system and analyze its multi-resonant state. We found that the circularization timescale, characterized by the Qe eccentricity damping factor, is a critical parameter in reproducing its architecture. When Qe <0.1 the orbit circularizes faster and we are able to find resonance trapping in the 8/5 mean motion resonance between the two innermost planets. |
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