The Mimas-Tethys and Enceladus-Dione systems
نویسندگان
چکیده
منابع مشابه
Tidal evolution of Mimas, Enceladus, and Dione
The tidal evolution through several resonances involving Mimas, Enceladus, and/or Dione is studied numerically with an averaged resonance model. We find that, in the Enceladus–Dione 2:1 e-Enceladus type resonance, Enceladus evolves chaotically in the future for some values of k2/Q. Past evolution of the system is marked by temporary capture into the Enceladus–Dione 4:2 ee ′-mixed resonance. We ...
متن کاملSaturn ’ S Diffuse E Ring and Its Connection with Enceladus
Introduction: Saturn’s E ring is the second largest planetary ring in the solar system, encompassing the icy satellites of Mimas (rM = 3.07RS), Enceladus (rE = 3.95RS), Tethys (rT = 4.88RS), Dione (rD = 6.25RS), Rhea (rR = 8.73R), and Titan (rR = 20.25RS). Enceladus was proposed early on as the dominant source of ring particles [1], since the edge-on brightness profile peaks near the moon’s mea...
متن کاملInternal Structure of Enceladus and Dione from Orbital Constraints
Introduction Enceladus is emitting measurable heat (37 GW) from a region centered on its South Pole [1]. Radioactive and accretional heating are expected to be minimal for such a small, low-density body, implying that the observed heat flow is due to past or present tidal dissipation [2]. The tidal heat production for which Enceladus’ eccentricity is in steady state, however, cannot exceed 1.1 ...
متن کاملClassification of Satellite Resonances in the Solar System
Several pairs of solar system satellites occupy mean motion resonances (MMRs). We divide these into two groups according to their proximity to exact resonance. Proximity is measured by the existence of a separatrix in phase space. MMRs between Io–Europa, Europa–Ganymede, and Enceladus–Dione are too distant from exact resonance for a separatrix to appear. A separatrix is present only in the phas...
متن کاملRecent orbital evolution and the internal structures of Enceladus and Dione
We study the orbital behavior of Saturn’s satellites Enceladus and Dione during their passage through the 2:1 mean-motion resonances to constrain their interior structures, parameterized by the quantity k2=Q (assumed constant). Enceladus’ evolution after escape from the second-order e-Enceladus e-Dione resonance requires that ðk2=QÞEnceladus < 8 10 , for that QSaturn > 18;000. This result is in...
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ژورنال
عنوان ژورنال: Symposium - International Astronomical Union
سال: 1996
ISSN: 0074-1809
DOI: 10.1017/s0074180900127251