Abstract
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Trans-Neptunian Objects (TNOs) are icy-rocky objects of various sizes, which move around the Sun beyond the orbit of Neptune in the so-called Edgeworth-Kuiper belt.
Aside from their most well-known representative, the dwarf planet Pluto, over a thousand such minor planets are cataloged, and new discoveries are still to be made in the area.
A more thorough exploration and better understanding of the characteristics of TNOs can also contribute to our knowledge of the processes shaping solar systems (including our own) all through their existence.
The current examination was dedicated to a detailed mapping of a narrower area of the field, namely, the dynamical parameters of the 5:2 resonance zone.
First, we will introduce the Edgeworth-Kuiper belt itself, and provide a short summary of the resonance phenomenon, which is one of the primary factors shaping the structure of the Trans-Neptunian domain.
Next, we will discuss the findings of the numerical simulations we used in order to map Neptune's 5:2 mean motion resonance zone.
Various interesting results will be covered, such as the broadening of the domain resonant TNOs may occupy in the a-e (semi-major axis – orbital eccentricity) plane, or the regularities discovered in the initial orbital elements M (mean anomaly) and ω (argument of pericenter) leading to resonant behaviour.
We look forward to presenting the meaning of these findings, as well as how they relate to our preexisting knowledge of the Trans-Neptunian belt.
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