Cassini Imaging Science: Initial Results on Saturn's Rings and Small Satellites

Porco, C. C.; Baker, Emily J.; Barbara, J.; Beurle, K.; Brahic, A.; Burns, Joseph A.; Charnoz, Sébastien; Cooper, Nicholas J.; Dawson, D. D.; Genio, Anthony D. Del; Denk, T.; Dones, L.; Dyudina, Ulyana A.; Evans, Michael; Giese, B.; Grazier, Kevin R.; Helfenstein, P.; Ingersoll, Andrew P.; Jacobson, R. A.; Johnson, T. V.; McEwen, A. S.; Murray, C. D.; Neukum, G.; Owen, W. M.; Perry, Jason; Roatsch, Thomas; Spitale, J. N.; Squyres, S. W.; Thomas, P. C.; Tiscareno, Matthew S.; Turtle, E. P.; Vasavada, A. R.; Veverka, J.; Wagner, Roland; West, Robert A.

doi:10.1126/science.1108056

Cited by 184 publications

(139 citation statements)

References 60 publications

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“…3(d)). Porco et al 2005 pointed out that the non-null value of the current Pallene's eccentricity (∼ 0.004, similar to the Enceladus'), could be explained by some secular resonance. Here we identify a possible candidate, but it is a quasi-resonance, and its effect is not strong enough to increase the eccentricity of the small satellite.…”

Section: Icy Bodies Of the Solar Systemmentioning

confidence: 99%

“…In spite of some recent investigations (Porco et al 2005, Callegari & Yokoyama 2008, long-term numerical integrations (i.e, in time scales of millennia), of the orbits of the three small satellites are not reported yet in the literature. Ephemeris of Methone, Anthe and Pallene are limited to 1,000 years (Horizons data system, http://ssd.jpl.nasa.gov).…”

Section: Introductionmentioning

confidence: 99%

“…Short-term dynamics (i.e., time scales of a few years), and determinations of orbital elements of Methone and Pallene, are reported in (Porco et al 2005, Spitale et al 2006, Porco et al 2007, Jacobson et al 2008). Anthe's orbit, the most recent small body detected in Saturnian system, is studied in Cooper et al 2008.…”

Section: Introductionmentioning

confidence: 99%

“…In our code, the mass of the small body is equal to the mass of a spherical body with density similar to the Mimas's and ∼3 km in diameter (e.g. Porco et al 2005, Porco et al 2007). …”

Section: Introductionmentioning

confidence: 99%

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Long-term dynamics of Methone, Anthe and Pallene

Callegari

Yokoyama

2009

Proc. IAU

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Abstract. We numerically investigate the long-term dynamics of the Saturn's small satellites Methone (S/2004 S1), Anthe (S/2007 S4) and Pallene (S/2004 S2). In our numerical integrations, these satellites are disturbed by non-spherical shape of Saturn and the six nearest regular satellites. The stability of the small bodies is studied here by analyzing long-term evolution of their orbital elements.We show that long-term evolution of Pallene is dictated by a quasi secular resonance involving the ascending nodes (Ω) and longitudes of pericentric distances ( ) of Mimas (subscript 1) and Pallene (subscript 2), which critical argument is 2 − 1 − Ω1 + Ω2 . Long-term orbital evolution of Methone and Anthe are probably chaotic since: i) their orbits randomly cross the orbit of Mimas in time scales of thousands years); ii) long-term numerical simulations involving both small satellites are strongly affected by small changes in the initial conditions.

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Section: Icy Bodies Of the Solar Systemmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

“…In our code, the mass of the small body is equal to the mass of a spherical body with density similar to the Mimas's and ∼3 km in diameter (e.g. Porco et al 2005, Porco et al 2007). …”

Section: Introductionmentioning

confidence: 99%

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Long-term dynamics of Methone, Anthe and Pallene

Callegari

Yokoyama

2009

Proc. IAU

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“…4) [18][19][20][21][22]. A major and persistent problem is that the rotation period taken as a reference frame for the atmospheric motions is not fixed from radio-rotation measurements, and ranges between 10 hr 39 min 24 s and 10 hr 46 min [18,[23][24][25].…”

Section: Meteorology and Atmospheric Dynamicsmentioning

confidence: 99%

Kronos: exploring the depths of Saturn with probes and remote sensing through an international mission

et al. 2008

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Kronos is a mission aimed to measure in situ the chemical and isotopic compositions of the Saturnian atmosphere with two probes and also by remote sensing, in order to understand the origin, formation, and evolution of giant planets in general, including extrasolar planets. Xe/ 129 Xe isotopic ratios will be measured by mass spectrometry on two probes entering the atmosphere of Saturn at two different locations near mid-latitudes, down to a pressure of 10 Bar. The global composition of Saturn will be investigated through these measurements, together with microwave radiometry determination of H 2 O and NH 3 and their 3D variations. The dynamics of Saturn's atmosphere will be investigated from: (1) measurements of pressure, temperature, vertical distribution of clouds and wind speed along the probes' descent trajectories, and (2) determination of deep winds, differential rotation and convection with combined probe, gravity and radiometric measurements. Besides these primary goals, Kronos will also measure the intensities and characteristics of Saturn's magnetic field inside the D ring as well as Saturn's gravitational field, in order to constrain the abundance of heavy elements in Saturn's interior and in its central core. Depending on the preferred architecture (flyby versus orbiter), Kronos will be in a position to measure the properties of Saturn's innermost magnetosphere and to investigate the ring structure in order to understand how these tiny structures could have formed and survived up to the present times.

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Hydrodynamic Description of Planetary Rings

Spahn

Schmidt

2006

GAMM-Mitteilungen

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We demonstrate the suitability of a hydrodynamic description of the dynamics of a dense planetary ring considering as an example the viscous oscillatory instability. For the successful application of hydrodynamics the transport coefficients must be known as functions of surface mass density σ and the granular temperature T of the ring material. We arrange scaling laws for these quantities and use parameters determined from particle simulations of a planetary ring. With such a preparation, the theory predicts an oscillatory instability of a dense ring: waves of radial wavelengths λ ≈ 100m...200m evolve, driven by the combined effects of viscous momentum flux and Coriolis force. These predictions are confirmed by direct particle simulations: wavelengths of the unstable modes, their growth rates, as well as the properties of the eigenfunctions of the perturbations. This success bears the hope to explain a class of so-called fine-structure in Saturn's rings, which are poorly understood to date. The experiments of the Cassini-spacecraft in orbit around Saturn offer the unique chance to identify the predicted density features by analyzing the imaging and occultation data.

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Cassini Imaging Science: Initial Results on Saturn's Rings and Small Satellites

Cited by 184 publications

References 60 publications

Long-term dynamics of Methone, Anthe and Pallene

Long-term dynamics of Methone, Anthe and Pallene

Kronos: exploring the depths of Saturn with probes and remote sensing through an international mission

Hydrodynamic Description of Planetary Rings

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