with arbitrary eccentricities and inclinations

1: Departamento Astronomia, Facultad de Ciencias, Uruguay

2: Universidad Nacional de Cordoba, Observatorio Astronomico - IATE, Argentina

www.fisica.edu.uy/~gallardo/atlas/plares.html

The present code is a model that describes the resonance strength, width, location and stability of fixed points, as well as periods of small-amplitude librations. The model is valid to any two gravitationally interacting massive bodies, and thus applicable to planets in mutual resonance around single stars or planets in resonance with binary stars. It can be applied to satellites around planets only when planetary oblateness can be ignored.

Given a system of N gravitationally interacting bodies, the codes allow to determine the resonant structure in a region of the phase space obtained, for example, by varying the initial conditions of one of its members. See the paper by Gallardo, Beauge and Giuppone (2021, Astron. Astrophys. 646, A148) for details (ArXiv).

Example of what the program generates. Taking a "pseudo" planet Mars moving its position in semi-major axis and eccentricity, the code calculates the widths of the stable resonances with Venus (green), Earth (blue) and Jupiter (red). Two interesting things: a) the resonances with Venus and Earth are stronger, and b) note that Mars is located in a region relatively void of strong resonances (its actual position is indicated). Input and output files for generating this plot here. |

Another example. Megno map for a circumbinary system in the (a,e) plane. Dark blue corresponds to more regular orbits, and lighter tones of green indicate increasingly chaotic motion. Brown corresponds to ejections. The libration widths of the most relevant MMRs determined with the model are plotted as white lines. The top scale indicates the positions of N/1 resonances with respect to the mean motion of the binary. Additionally, we plot the position of some similar CB systems. Taken from paper by Gallardo, Beauge and Giuppone (2021). |