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...

Descripción completa

Guardado en:
Detalles Bibliográficos
Autores principales: Charalambous, C., Beaugé, C.
Formato: Articulo
Lenguaje:Inglés
Publicado: 2021
Materias:
Ciencias Astronómicas
planet-disk interactions
protoplanetary disks
celestial mechanics
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/165454
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-165454
record_format dspace
spelling I19-R120-10915-1654542024-04-29T20:03:40Z http://sedici.unlp.edu.ar/handle/10915/165454 The 8/5 resonance between TRAPPIST-1 innermost planets Charalambous, C. Beaugé, C. 2021 2024-04-29T16:47:38Z en Ciencias Astronómicas planet-disk interactions protoplanetary disks celestial mechanics 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. La interacción entre los planetas y el disco protoplanetario produce que éstos migren a una tasa que depende de las características del disco de gas y la masa de los planetas migrantes. Debido a la incerteza en la determinación de las masas de los planetas del sistema TRAPPIST-1, sus tasas de migración no están bien determinadas. En este trabajo presentamos el resultado de simulaciones de A-cuerpos con migración de tipo I para reproducir la configuración general de TRAPPIST-1 y estudiar su estado multiresonante. Encontramos que la escala de tiempo de circularización orbital, caracterizada mediante el factor de decaimiento de la excentricidad Qe, es un parámetro crítico para reproducir su arquitectura. Si Qe &lt; 0.1 la órbita se circulariza más rápidamente y es posible encontrar una captura en la resonancia de movimientos medios 8/5 entre los dos planetas más internos. Asociación Argentina de Astronomía Articulo Articulo http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) application/pdf 41-43
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Ciencias Astronómicas
planet-disk interactions
protoplanetary disks
celestial mechanics
spellingShingle Ciencias Astronómicas
planet-disk interactions
protoplanetary disks
celestial mechanics
Charalambous, C.
Beaugé, C.
The 8/5 resonance between TRAPPIST-1 innermost planets
topic_facet Ciencias Astronómicas
planet-disk interactions
protoplanetary disks
celestial mechanics
description 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.
format Articulo
Articulo
author Charalambous, C.
Beaugé, C.
author_facet Charalambous, C.
Beaugé, C.
author_sort Charalambous, C.
title The 8/5 resonance between TRAPPIST-1 innermost planets
title_short The 8/5 resonance between TRAPPIST-1 innermost planets
title_full The 8/5 resonance between TRAPPIST-1 innermost planets
title_fullStr The 8/5 resonance between TRAPPIST-1 innermost planets
title_full_unstemmed The 8/5 resonance between TRAPPIST-1 innermost planets
title_sort 8/5 resonance between trappist-1 innermost planets
publishDate 2021
url http://sedici.unlp.edu.ar/handle/10915/165454
work_keys_str_mv AT charalambousc the85resonancebetweentrappist1innermostplanets
AT beaugec the85resonancebetweentrappist1innermostplanets
AT charalambousc 85resonancebetweentrappist1innermostplanets
AT beaugec 85resonancebetweentrappist1innermostplanets
_version_ 1807223056326721536

Ejemplares similares