English Scientific Article (Journal Article)

Published: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 0035-8711 1365-2966 496 (3) pp. 3700-3707 2020

- SJR Scopus - Astronomy and Astrophysics: Q1

Identifiers

- MTMT: 31696677
- DOI: 10.1093/mnras/staa1727
- WoS: 000574919300069

Subjects:

Although the search for extrasolar co-orbital bodies has not had success so far, it
is believed that they must be as common as they are in the Solar system. Co-orbital
systems have been widely studied, and there are several works on stability and even
on formation. However, for the size and location of the stable regions, authors usually
describe their results but do not provide a way to find them without numerical simulations,
and, in most cases, the mass ratio value range is small. In this work, we study the
structure of co-orbital stable regions for a wide range of mass ratio systems and
build empirical equations to describe them. It allows estimating the size and location
of co-orbital stable regions from a few system parameters. Thousands of massless particles
were distributed in the co-orbital region of a massive secondary body and numerically
simulated for a wide range of mass ratios (mu) adopting the planar circular restricted
three-body problem. The results show that the upper limit of horseshoe regions is
between 9.539 x 10(-4) < mu < 1.192 x 10(-3), which corresponds to a minimum angular
distance from the secondary body to the separatrix of between 27.239 degrees and 27.802
degrees. We also found that the limit to existence of stability in the co-orbital
region is about mu = 2.3313 x 10(-2), much smaller than the value predicted by the
linear theory. Polynomial functions to describe the stable region parameters were
found, and they represent estimates of the angular and radial widths of the co-orbital
stable regions for any system with 9.547 x 10(-5) <= mu <= 2.331 x 10(-2).

2021-09-21 22:37