| 研究実績の概要 |
Firstly, targeting at various fidelity requirements, the researcher established a series dynamical models of Mars-Phobos system considering multiple perturbations. Then, based on the perturbation theory, the mechanism of Mars gravity on periodic motion in Phobos vicinity is discussed. By single-averaging method, the Mars gravity perturbation on the periodic motion near Phobos is divided to secular and osculating parts mathematically. Importantly, the perturbed dynamics is established in two cases, i.e., outsides and insides the sphere of influence of Phobos, respectively. It is demonstrated numerically that its secular perturbation contributes to the continuous decreasing or increasing "ω" (the argument of pericenter) of distant retrograde orbit family outsides and insides the sphere of influence of Phobos, respectively. The osculating effect of Mars gravity perturbation is critical to the different variation of "ω" for two satellite orbit families, i.e., g and g’ families. Furthermore, in detecting the dynamical flow in energy space of satellite orbits, polygonal-like resonant periodic families are gained and show multiple loops above the Phobos surface. Enlightened by the aforementioned results, the researcher is developing a jumping mechanism on the Phobos surface by arcs of g and g’ families and their invariant tori. The current results demonstrate a feasible point-to-point transfer mechanism with flexible time of flight and proper initial relative velocity.
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| 現在までの達成度 (区分) |
現在までの達成度 (区分)
2: おおむね順調に進展している
理由
The current status of the research goes well as scheduled in JSPS application. So far, a series dynamical models of Mars-Phobos system are established according to different fidelity requirements, which fundamentally support the research on interdisciplinary research of celestial mechanics and planetary science in next stage. Importantly, based on the perturbation theory, the mechanism of Mars gravity on periodic motion in Phobos vicinity is discussed. Wherein the dynamics near Phobos is described by six canonical variables. Not only some valuable results are obtained by so, but also the current analysis can be extended to the study of a mathematical problem, i.e., coplanar motion, explaining the disturbed motion very close to Phobos. Furthermore, instead of the “popular” distant retrograde orbit family, the potential application of two satellite families consisting of prograde orbits is being studied, which provides us a new view to examine the periodic motion around Phobos. As an assistance to the research, the engagement to the research group, and the institution is getting on the right track. The abundant resources both academic and industrial, and both domestic and international from the institution are promoting the researcher’s early career. However, the current research is suffering from the spread of Coronavirus inevitably to some degree. Remarkably amount of time and efforts are spent on the settle-down and initialization in the early stage of the research in FY 2019. Thus, the current status is better to be regarded as moderate.
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| 今後の研究の推進方策 |
The researcher is planning to conduct and extend the current results from the following aspects: 1) study the coplanar motion near Phobos in the sense of formation dynamics by perturbation theory. The truncation of perturbation series function is avoided so the coplanar motion very close to Phobos with an altitude of 10-50 km is better described. 2) apply the jumping dynamics to point-to-point transfer along Phobos 3D surface. The spatial satellite orbit families are employed. A jumping strategy is developed. Through such chess-jumping, routines between two and several valuable locations, e.g., craters Clustril and Drunlo are planned as an example. 3) combine weak stability boundary with periodic motion near Phobos. A new concept of dynamical influence of sphere of Phobos is developed considering periodic perturbations, such as Mars orbital eccentricity and solar perturbation. The capture by Phobos is achieved by implementing a proper kick at the apocenter of resonant orbits around Mars. 4) explore the potential distribution of dust tori around Phobos. A new description of the distribution of dust tori is employed by introducing the concept of space density matrix. The dynamics of dust tori is established by partial differential equations considering Mars orbital eccentricity and solar perturbation etc.
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