Figure 2 - available via license: Creative Commons Attribution 4.0 International
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(left) The characteristic curve of the circular family CR for the ellipsoid (dashed curve) and 433-Eros (solid curve) projected on the plane y0 − z0. The points Bm indicate the y0-position of the v.c.o. with the subscript m being the multiplicity. The red segment indicates the part of the family with unstable orbits. (right) The variation of the stability indices b1 and b2 along the CR-family of ellipsoid and Eros.
Source publication
In Karydis et al. (2021) we have introduced the method of shape continuation in order to obtain periodic orbits in the complex gravitational field of an irregularly-shaped asteroid starting from a symmetric simple model. What’s more, we map the families of periodic orbits of the simple model to families of the real asteroid model. The introduction...
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Context 1
... et al. (2020)). In the ellipsoid model, we consider the family of planar (z = 0) circular retrograde orbits, C R , which is fully stable. The family is also vertically stable but there are v.c.o. for higher period multiplicities (m = 2, 3, 4, ..). Their y 0 -position (where y 0 is the approximate radius of the orbit) is shown in the left panel of Fig. 2. The right panel shows the stability indicies b i along the family (dashed curves). The C R is continued when asymmetric terms are added in the potential in order to simulate the potential of the asteroid. The computed family for 433-Eros consists of orbits which are no longer planar and symmetric but are almost circular. The family is ...
Context 2
... right panel shows the stability indicies b i along the family (dashed curves). The C R is continued when asymmetric terms are added in the potential in order to simulate the potential of the asteroid. The computed family for 433-Eros consists of orbits which are no longer planar and symmetric but are almost circular. The family is presented in Fig. 2 with solid curves. The major part of C R of Eros consists of stable orbits and this is also the case close to the radius of the v.c.o. B 3 and B 4 . Therefore, such a situation implies scheme I for the 3D orbits emanating in the symmetric model from these v.c.o.. However, it is evident that the introduced asymmetries caused an unstable ...