Planetary Rings and Other Astrophysical Disks

Latter, Henrik N.; Ogilvie, Gordon I.; Rein, Hanno

doi:10.1017/9781316286791.020

Cited by 4 publications

(2 citation statements)

References 365 publications

(405 reference statements)

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“…This structural richness is indicative of an underlying dynamical richness (Burns & Cuzzi 2006;Schmidt et al 2009;Cuzzi et al 2018) which has been exposed in the rings. Due to their proximity and consequent accessibility by spacecraft, Saturn's rings can serve as a "local laboratory" to study processes, such as accretion and disk-satellite interactions, which are also at work in protoplanetary disks (Cuzzi et al 2010;Latter et al 2018). Furthermore, it may be expected that future missions, such as the planned ring skimmer mission (Tiscareno et al 2020) will provide observations of Saturn's rings with an even higher level of detail, which will help to further support the improvement of theories describing astrophysical disks.…”

Section: Introductionmentioning

confidence: 99%

Density waves and the viscous overstability in Saturn’s rings

Lehmann

Schmidt

Salo

2019

A&A

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This paper addresses resonantly forced spiral density waves in a dense planetary ring which is close to the threshold for viscous overstability. We solve numerically the hydrodynamical equations for a dense thin disk in the vicinity of an inner Lindblad resonance with a perturbing satellite. Our numerical scheme is one-dimensional so that the spiral shape of a density wave is taken into account through a suitable approximation of the advective terms arising from the fluid orbital motion. This paper is a first attempt to model the co-existence of resonantly forced density waves and short-scale free overstable wavetrains as observed in Saturn's rings, by conducting large-scale hydrodynamical integrations. These integrations reveal that the two wave types undergo complex interactions, not taken into account in existing models for the damping of density waves. In particular it is found that, depending on the relative magnitude of both wave types, the presence of viscous overstability can lead to a damping of an unstable density wave and vice versa. The damping of the short-scale viscous overstability by a density wave is investigated further by employing a simplified model of an axisymmetric ring perturbed by a nearby Lindblad resonance. A linear hydrodynamic stability analysis as well as local N-body simulations of this model system are performed and support the results of our large-scale hydrodynamical integrations.

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Section: Introductionmentioning

confidence: 99%

Density waves and the viscous overstability in Saturn’s rings

Lehmann

Schmidt

Salo

2019

A&A

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“…We bring up in this section rings and disks around planets, but there are ringstructures everywhere in the Universe within an unimaginable range of sizes (see, for example, the review by Latter et al 2017).…”

Section: Ringsmentioning

confidence: 99%

Special Cases: Moons, Rings, Comets, and Trojans

Cabrera

Jiménez

Muñoz

2017

Handbook of Exoplanets

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Non-planetary bodies provide valuable insight into our current understanding of planetary formation and evolution. Although these objects are challenging to detect and characterize, the potential information to be drawn from them has motivated various searches through a number of techniques. Here, we briefly review the current status in the search of moons, rings, comets, and trojans in exoplanet systems and suggest what future discoveries may occur in the near future.

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Viscous overstability in dense planetary rings – effect of vertical motions and dense packing

Lehmann,

Salo

2023

Monthly Notices of the Royal Astronomical Society

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We investigate the linear axisymmetric viscous overstability in dense planetary rings with typical values of the dynamical optical depth τ ≳ 0.5. We develop a granular flow model which accounts for the particulate nature of a planetary ring subjected to dissipative particle collisions. The model captures the dynamical evolution of the disc’s vertical thickness, temperature, and effects related to a finite volume filling factor of the ring fluid. We compute equilibrium states of self-gravitating and non-self-gravitating rings, which compare well with existing results from kinetic models and N-Body simulations. Subsequently, we conduct a linear stability analysis of our model. We briefly discuss the different linear eigenmodes of the system and compare with existing literature by applying corresponding limiting approximations. We then focus on the viscous overstability, analysing the effect of temperature variations, radial and vertical self-gravity, and for the first time the effects of vertical motions on the instability. In addition, we perform local N-body simulations incorporating radial and vertical self-gravity. Critical values for the optical depth and the filling factor for the onset of instability resulting from our N-body simulations compare well with our model predictions under the neglect of radial self-gravity. When radial self-gravity is included, agreement with N-body simulations can be achieved by adopting enhanced values of the bulk viscous stress.

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Planetary Rings and Other Astrophysical Disks

Cited by 4 publications

References 365 publications

Density waves and the viscous overstability in Saturn’s rings

Density waves and the viscous overstability in Saturn’s rings

Special Cases: Moons, Rings, Comets, and Trojans

Viscous overstability in dense planetary rings – effect of vertical motions and dense packing

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