Hydrodynamics of Saturn’s Dense Rings

M. Seiß; F. Spahn

Mathematical Modelling of Natural Phenomena (2011)

  • Volume: 6, Issue: 4, page 191-218
  • ISSN: 0973-5348

Abstract

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The space missions Voyager and Cassini together with earthbound observations revealed a wealth of structures in Saturn’s rings. There are, for example, waves being excited at ring positions which are in orbital resonance with Saturn’s moons. Other structures can be assigned to embedded moons like empty gaps, moon induced wakes or S-shaped propeller features. Furthermore, irregular radial structures are observed in the range from 10 meters until kilometers. Here some of these structures will be discussed in the frame of hydrodynamical modeling of Saturn’s dense rings. For this purpose we will characterize the physical properties of the ring particle ensemble by mean field quantities and point to the special behavior of the transport coefficients. We show that unperturbed rings can become unstable and how diffusion acts in the rings. Additionally, the alternative streamline formalism is introduced to describe perturbed regions of dense rings with applications to the wake damping and the dispersion relation of the density waves.

How to cite

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Seiß, M., and Spahn, F.. "Hydrodynamics of Saturn’s Dense Rings." Mathematical Modelling of Natural Phenomena 6.4 (2011): 191-218. <http://eudml.org/doc/222216>.

@article{Seiß2011,
abstract = {The space missions Voyager and Cassini together with earthbound observations revealed a wealth of structures in Saturn’s rings. There are, for example, waves being excited at ring positions which are in orbital resonance with Saturn’s moons. Other structures can be assigned to embedded moons like empty gaps, moon induced wakes or S-shaped propeller features. Furthermore, irregular radial structures are observed in the range from 10 meters until kilometers. Here some of these structures will be discussed in the frame of hydrodynamical modeling of Saturn’s dense rings. For this purpose we will characterize the physical properties of the ring particle ensemble by mean field quantities and point to the special behavior of the transport coefficients. We show that unperturbed rings can become unstable and how diffusion acts in the rings. Additionally, the alternative streamline formalism is introduced to describe perturbed regions of dense rings with applications to the wake damping and the dispersion relation of the density waves. },
author = {Seiß, M., Spahn, F.},
journal = {Mathematical Modelling of Natural Phenomena},
keywords = {granular gas; instabilities; hydrodynamics; planetary rings},
language = {eng},
month = {7},
number = {4},
pages = {191-218},
publisher = {EDP Sciences},
title = {Hydrodynamics of Saturn’s Dense Rings},
url = {http://eudml.org/doc/222216},
volume = {6},
year = {2011},
}

TY - JOUR
AU - Seiß, M.
AU - Spahn, F.
TI - Hydrodynamics of Saturn’s Dense Rings
JO - Mathematical Modelling of Natural Phenomena
DA - 2011/7//
PB - EDP Sciences
VL - 6
IS - 4
SP - 191
EP - 218
AB - The space missions Voyager and Cassini together with earthbound observations revealed a wealth of structures in Saturn’s rings. There are, for example, waves being excited at ring positions which are in orbital resonance with Saturn’s moons. Other structures can be assigned to embedded moons like empty gaps, moon induced wakes or S-shaped propeller features. Furthermore, irregular radial structures are observed in the range from 10 meters until kilometers. Here some of these structures will be discussed in the frame of hydrodynamical modeling of Saturn’s dense rings. For this purpose we will characterize the physical properties of the ring particle ensemble by mean field quantities and point to the special behavior of the transport coefficients. We show that unperturbed rings can become unstable and how diffusion acts in the rings. Additionally, the alternative streamline formalism is introduced to describe perturbed regions of dense rings with applications to the wake damping and the dispersion relation of the density waves.
LA - eng
KW - granular gas; instabilities; hydrodynamics; planetary rings
UR - http://eudml.org/doc/222216
ER -

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