On the identification of the first two young asteroid families in g-type non-linear secular resonances
Journal article, 2024
Linear secular resonances happen when there is a commensurability between the precession frequency of the pericenter, g, or longitude of the node, s, of an asteroid and a planet. Non-linear resonances are higher order combinations of these frequencies. Here, we studied the three most diffusive g-type non-linear secular resonances using Artificial Neural Networks. We identified a population of more than 2100 resonant objects in the g − 2g6 + g5 and g − 3g6 + 2g5 resonances. This allows the creation of a Convolutional Neural Network model for the g − 2g6 + g5 resonance, able to predict the status of several thousands of asteroids in seconds. We identified 12 new possible dynamical groups among the resonant population, including the 5507 and 170776 families, which have both estimated ages of less than 7 Myr. These are the two first-ever identified young families in resonant configurations of the investigated resonances, which allows for setting limits on their original ejection velocity field.
minor planets, asteroids: individual
astronomical data bases: miscellaneous
minor planets, asteroids: general
Author
V. Carruba
Laboratório Interinstitucional de e-Astronomia
São Paulo State University (UNESP)
S. Aljbaae
Instituto Nacional de Pesquisas Espaciais
Z. Knežević
Institute for the Serbian Language of SASA
M. Mahlke
Institut d'Astrophysique Spatiale
J. R. Masiero
California Institute of Technology (Caltech)
F. Roig
Observatorio Nacional
R. C. Domingos
São Paulo State University (UNESP)
M. Huaman
Universidad Tecnológica del Perú
A. Alves
São Paulo State University (UNESP)
B. S. Martins
São Paulo State University (UNESP)
G. Caritá
Instituto Nacional de Pesquisas Espaciais
M. Lourenço
São Paulo State University (UNESP)
Sofia Cvetkovic Destouni
Chalmers, Space, Earth and Environment, Physical Resource Theory
Monthly Notices of the Royal Astronomical Society
0035-8711 (ISSN) 1365-2966 (eISSN)
Vol. 528 1 796-814Subject Categories (SSIF 2011)
Condensed Matter Physics
DOI
10.1093/mnras/stad3968