Three-dimensional Dynamics of Narrow Planetary Rings

@article{Chiang2003ThreedimensionalDO,
  title={Three-dimensional Dynamics of Narrow Planetary Rings},
  author={Eugene Chiang and Christopher J. Culter},
  journal={The Astrophysical Journal},
  year={2003},
  volume={599},
  pages={675-685}
}
Narrow planetary rings are eccentric and inclined. Particles within a given ring must therefore share the same pericenter and node. We solve for the three-dimensional geometries and mass distributions that enable the Uranian α- and β-rings and the Saturnian Maxwell and Colombo (Titan) rings to maintain simultaneous apsidal and nodal lock. Ring self-gravity, interparticle collisions, and the quadrupole field of the host planet balance each other to achieve this equilibrium. We prove that such an… 
The Torque at a Lindblad Vertical Resonance
A fairly uniform, rapidly and differentially rotating disk of rarely colliding particles (when the frequency of interparticle collisions is much smaller than the local orbital frequency) in a
Collisional Particle Disks
We present a new, simple, fast algorithm to numerically evolve disks of inelastically colliding particles surrounding a central star. Our algorithm adds negligible computational cost to the fastest
Secular Evolution Driven by Massive Eccentric Disks/Rings: An Apsidally Aligned Case
Massive eccentric disks (gaseous or particulate) orbiting a dominant central mass appear in many astrophysical systems, including planetary rings, protoplanetary and accretion disks in binaries, and
The Circumbinary Ring of KH 15D
The light curves of the pre-main-sequence star KH 15D from the years 1913-2003 can be understood if the star is a member of an eccentric binary that is encircled by a vertically thin, inclined ring
STIS Coronagraphic Imaging of Fomalhaut: Main Belt Structure and the Orbit of Fomalhaut b
We present new optical coronagraphic data of Fomalhaut obtained with HST/STIS in 2010 and 2012. Fomalhaut b is recovered at both epochs to high significance. The observations include the discoveries
Constraining the circumbinary disc tilt in the KH 15D system
KH 15D is a system which consists of a young, eccentric, eclipsing binary, and a circumbinary disk which obscures the binary as the disk precesses. We develop a self-consistent model that provides a

References

SHOWING 1-10 OF 14 REFERENCES
APSE ALIGNMENT OF NARROW ECCENTRIC PLANETARY RINGS
The boundaries of the Uranian ∈, α, and β rings can be fitted by Keplerian ellipses. The pair of ellipses that outline a given ring share a common line of apsides. Apse alignment is surprising
THE DYNAMICS OF ELLIPTICAL RINGS
We investigate the evolution of eccentric rings under the influence of (1) differential precession due to the planetary quadrupole moment; (2) self-gravity; (3) viscous forces due to interparticle
Towards a theory for the uranian rings
Interparticle collisions, radiation drag and differential precession all tend to disrupt the rings of Uranus. The first two effects lead to radial spreading which would disrupt a free ring in ≲108
Apse Alignment of the Uranian Rings
Abstract An explanation of the dynamical mechanism for apse alignment of the eccentric uranian rings is necessary before observations can be used to determine properties such as ring masses, particle
EXCITATION OF ORBITAL ECCENTRICITIES BY REPEATED RESONANCE CROSSINGS: REQUIREMENTS
Divergent migration of planets within a viscous circumstellar disk can engender resonance crossings and dramatic excitation of orbital eccentricities. We provide quantitative criteria for the
Sharp edges of planetary rings
The ring systems of Saturn and Uranus exhibit several sharp edges across which the optical depth drops from order unity to essentially zero. At least two and perhaps all of these features are
Shepherding of the Uranian Rings. II. Dynamics
We explore the dynamical significance of the orbital resonances, identified in Paper I (Porco and Goldreich 1987), involving the satellites 1986U7 and 1986U8, and the є, δ, and y rings. We
Precession of inclined rings
Differential precession due to the planet's quadrupole moment tends to destroy the alignment of particles in inclined rings. We propose that alignment is maintained by the self-gravity of the ring.
Narrow rings: Observations and theory
Precession of the epsilon ring of Uranus
The boundaries of the epsilon ring can be fit by aligned Keplerian ellipses. Differential precession due to the quadrupole moment of Uranus tends to destroy the apse alignment. We propose that apse
...
1
2
...