TY - JOUR
T1 - A deep dive into the 2 g+ h resonance
T2 - separatrices, manifolds and phase space structure of navigation satellites
AU - Daquin, Jérôme
AU - Legnaro, Edoardo
AU - Gkolias, Ioannis
AU - Efthymiopoulos, Christos
N1 - Funding Information:
J.D. is a postdoctoral researcher of the ‘Fonds de la Recherche Scientifique’—FNRS. J.D. acknowledges the support of the ERC project 677793 ‘Stable and Chaotic Motions in the Planetary Problem’ leaded by Prof. Gabriella Pinzari. I.G. acknowledges the support of the ERC project 679086 COMPASS ‘Control for Orbit Manoeuvring through Perturbations for Application to Space Systems.’ E. L. has been supported by the Marie Curie Initial Training Network Stardust-R, Grant Agreement Number 813644 under the H2020 research and innovation program. C. E. was partially supported by EU-ITN Stardust-R and MIUR-PRIN 20178CJA2B ‘New Frontiers of Celestial Mechanics: theory and Applications.’ The authors acknowledge feedback and discussions with Elisa Maria Alessi.
Funding Information:
J.D. is a postdoctoral researcher of the ?Fonds de la Recherche Scientifique??FNRS. J.D. acknowledges the support of the ERC project 677793 ?Stable and Chaotic Motions in the Planetary Problem? leaded by Prof.?Gabriella Pinzari. I.G. acknowledges the support of the ERC project 679086 COMPASS ?Control for Orbit Manoeuvring through Perturbations for Application to Space Systems.? E.?L. has been supported by the Marie Curie Initial Training Network Stardust-R, Grant Agreement Number 813644 under the H2020 research and innovation program. C.?E. was partially supported by EU-ITN Stardust-R and MIUR-PRIN 20178CJA2B ?New Frontiers of Celestial Mechanics: theory and Applications.? The authors acknowledge feedback and discussions with Elisa Maria Alessi.
Publisher Copyright:
© 2022, The Author(s), under exclusive licence to Springer Nature B.V.
PY - 2022/2
Y1 - 2022/2
N2 - Despite extended past studies, several questions regarding the resonant structure of the medium-Earth orbit (MEO) region remain hitherto unanswered. This work describes in depth the effects of the 2 g+ h lunisolar resonance. In particular, (i) we compute the correct forms of the separatrices of the resonance in the inclination-eccentricity (i, e) space for fixed semi-major axis a. This allows to compute the change in the width of the 2 g+ h resonance as the altitude increases. (ii) We discuss the crucial role played by the value of the inclination of the Laplace plane, iL. Since iL is comparable to the resonance’s separatrix width, the parametrization of all resonance bifurcations has to be done in terms of the proper inclination ip, instead of the mean one. (iii) The subset of circular orbits constitutes an invariant subspace embedded in the full phase space, the center manifold C, where actual navigation satellites lie. Using ip as a label, we compute its range of values for which C becomes a normally hyperbolic invariant manifold (NHIM). The structure of invariant tori in C allows to explain the role of the initial phase h noticed in several works. (iv) Through Fast Lyapunov Indicator (FLI) cartography, we portray the stable and unstable manifolds of the NHIM as the altitude increases. Manifold oscillations dominate in phase space between a= 24,000 km and a= 30,000 km as a result of the sweeping of the 2 g+ h resonance by the [InlineEquation not available: see fulltext.] and [InlineEquation not available: see fulltext. resonances. The noticeable effects of the latter are explained as a consequence of the relative inclination of the Moon’s orbit with respect to the ecliptic. The role of the phases [InlineEquation not available: see fulltext.] in the structures observed in the FLI maps is also clarified. Finally, (v) we discuss how the understanding of the manifold dynamics could inspire end-of-life disposal strategies.
AB - Despite extended past studies, several questions regarding the resonant structure of the medium-Earth orbit (MEO) region remain hitherto unanswered. This work describes in depth the effects of the 2 g+ h lunisolar resonance. In particular, (i) we compute the correct forms of the separatrices of the resonance in the inclination-eccentricity (i, e) space for fixed semi-major axis a. This allows to compute the change in the width of the 2 g+ h resonance as the altitude increases. (ii) We discuss the crucial role played by the value of the inclination of the Laplace plane, iL. Since iL is comparable to the resonance’s separatrix width, the parametrization of all resonance bifurcations has to be done in terms of the proper inclination ip, instead of the mean one. (iii) The subset of circular orbits constitutes an invariant subspace embedded in the full phase space, the center manifold C, where actual navigation satellites lie. Using ip as a label, we compute its range of values for which C becomes a normally hyperbolic invariant manifold (NHIM). The structure of invariant tori in C allows to explain the role of the initial phase h noticed in several works. (iv) Through Fast Lyapunov Indicator (FLI) cartography, we portray the stable and unstable manifolds of the NHIM as the altitude increases. Manifold oscillations dominate in phase space between a= 24,000 km and a= 30,000 km as a result of the sweeping of the 2 g+ h resonance by the [InlineEquation not available: see fulltext.] and [InlineEquation not available: see fulltext. resonances. The noticeable effects of the latter are explained as a consequence of the relative inclination of the Moon’s orbit with respect to the ecliptic. The role of the phases [InlineEquation not available: see fulltext.] in the structures observed in the FLI maps is also clarified. Finally, (v) we discuss how the understanding of the manifold dynamics could inspire end-of-life disposal strategies.
KW - Chaotic dynamics
KW - GNSS
KW - Manifold dynamics
KW - Medium- Earth orbit
KW - Orbital resonances
KW - Satellite orbits
UR - http://www.scopus.com/inward/record.url?scp=85123069776&partnerID=8YFLogxK
U2 - 10.1007/s10569-021-10060-6
DO - 10.1007/s10569-021-10060-6
M3 - Article
AN - SCOPUS:85123069776
SN - 0923-2958
VL - 134
JO - Celestial Mechanics & Dynamical Astronomy
JF - Celestial Mechanics & Dynamical Astronomy
IS - 1
M1 - 6
ER -