TY - JOUR
T1 - The 3:1 mean motion resonance between Miranda and the inner Uranian satellites, Cressida and Desdemona
AU - Verheylewegen, Emilie
AU - Lemaitre, Anne
PY - 2014
Y1 - 2014
N2 - We build a simple dissipative analytical model considering an averaged restricted 3-body problem taking into account the effect of the oblateness of a planet on a small satellite and on its perturber. We apply this model to the inner Uranian system and we follow the dynamical evolution of the satellites Cressida or Desdemona, these latter being close to a 3:1 commensurability with the large satellite Miranda. Our analysis shows that the positions of the two inner satellites, on both sides of the exact resonance, are temporary, Cressida having already crossed the resonance, and Desdemona approaching the commensurability to jump over later on.
AB - We build a simple dissipative analytical model considering an averaged restricted 3-body problem taking into account the effect of the oblateness of a planet on a small satellite and on its perturber. We apply this model to the inner Uranian system and we follow the dynamical evolution of the satellites Cressida or Desdemona, these latter being close to a 3:1 commensurability with the large satellite Miranda. Our analysis shows that the positions of the two inner satellites, on both sides of the exact resonance, are temporary, Cressida having already crossed the resonance, and Desdemona approaching the commensurability to jump over later on.
KW - Inner Uranian system
KW - Miranda-Cressida-Desdemona
KW - Oblateness
KW - Restricted 3-body problem
UR - http://www.scopus.com/inward/record.url?scp=84905753988&partnerID=8YFLogxK
U2 - 10.1007/s10569-014-9550-y
DO - 10.1007/s10569-014-9550-y
M3 - Article
AN - SCOPUS:84905753988
SN - 0923-2958
VL - 119
SP - 283
EP - 299
JO - Celestial Mechanics & Dynamical Astronomy
JF - Celestial Mechanics & Dynamical Astronomy
IS - 3-4
ER -