Resonance Occupation in the Kuiper Belt: Case Examples of the 5:2 and Trojan Resonances

@article{Chiang2003ResonanceOI,
  title={Resonance Occupation in the Kuiper Belt: Case Examples of the 5:2 and Trojan Resonances},
  author={Eugene Chiang and Amy B. Jordan and Robert L. Millis and Marc Buie and Lawrence H. Wasserman and James L. Elliot and Susan Diane Kern and David E. Trilling and Karen J. Meech and R. Mark Wagner},
  journal={The Astronomical Journal},
  year={2003},
  volume={126},
  pages={430 - 443}
}
As part of our ongoing Deep Ecliptic Survey (DES) of the Kuiper belt, we report on the occupation of the 1 : 1 (Trojan), 4 : 3, 3 : 2, 7 : 4, 2 : 1, and 5 : 2 Neptunian mean motion resonances (MMRs). The previously unrecognized occupation of the 1 : 1 and 5 : 2 MMRs is not easily understood within the standard model of resonance sweeping by a migratory Neptune over an initially dynamically cold belt. Among all resonant Kuiper belt objects (KBOs), the three observed members of the 5 : 2 MMR… 
Neptune's 5:2 Resonance in the Kuiper Belt
Observations of Kuiper Belt objects (KBOs) in Neptune’s 5:2 resonance present two puzzles: this third-order resonance hosts a surprisingly large population, comparable to the prominent populations of
Formation of the Resonant Populations in the Kuiper Belt
Kuiper belt objects (KBOs) have most of their orbits within a thick disk outside that of Neptune as they are located around heliocentric distances in the range 35-50 AU. On the basis of their orbital
Resonant motion of trans-Neptunian objects in high-eccentricity orbits
A substantial fraction of the Edgeworth-Kuiper belt objects are presently known to move in resonance with Neptune (the principal commensurabilities are 1/2, 3/5, 2/3, and 3/4). We have found that
THE COLOR DIFFERENCES OF KUIPER BELT OBJECTS IN RESONANCE WITH NEPTUNE
The optical colors of 58 objects in mean motion resonance with Neptune were obtained. The various Neptune resonant populations were found to have significantly different surface color distributions.
Neptune migration model with one extra planet
NEPTUNE’S ORBITAL MIGRATION WAS GRAINY, NOT SMOOTH
The Kuiper Belt is a population of icy bodies beyond the orbit of Neptune. The complex orbital structure of the Kuiper Belt, including several categories of objects inside and outside of resonances
The Orbital and Spatial Distribution of the Kuiper Belt
Models of the evolution of Neptune’s migration and the dynamical processes at work during the formation of the outer solar system can be constrained by measuring the orbital distribution of the
EVIDENCE FOR SLOW MIGRATION OF NEPTUNE FROM THE INCLINATION DISTRIBUTION OF KUIPER BELT OBJECTS
Much of the dynamical structure of the Kuiper Belt can be explained if Neptune migrated over several AU, and/or if Neptune was scattered to an eccentric orbit during planetary instability. An
Stability of Neptune’s Distant Resonances in the Presence of Planet Nine
Trans-Neptunian Objects (TNOs) in the scattered disk with 50 ≲ a ≲ 100 au are thought to cluster near Neptune’s n:1 resonances (e.g., 3:1, 4:1, and so on). While these objects spend lengthy periods
...
...

References

SHOWING 1-10 OF 34 REFERENCES
On the Plutinos and Twotinos of the Kuiper Belt
We illuminate dynamical properties of Kuiper belt objects (KBOs) in the 3 : 2 (Plutino) and 2 : 1 ("Twotino") Neptunian resonances within the model of resonant capture and migration. We analyze a
Mean Motion Resonances in the Transneptunian Region. Part II: The 1 : 2, 3 : 4, and Weaker Resonances
Abstract The stability of orbits in the transneptunian region is numerically computed. It is found that, in analogy to the asteroid belt, there exist many chaotic layers associated with thin
Large Kuiper Belt Objects: The Mauna Kea 8K CCD Survey
We describe a large-area ecliptic survey designed to assess the sky-plane surface density of bright Kuiper Belt objects. We used an 8192 × 8192 pixel CCD mosaic to image 51.5 deg2 to a 50% detection
The Edge of the Solar System
We have surveyed for Kuiper Belt objects (KBOs) in six fields of the ecliptic (total sky area 1.5 deg2) to limiting magnitudes between R = 24.9 and R = 25.9. This is deep enough to detect KBOs of
Accretion in the Early Kuiper Belt. II. Fragmentation
We describe new planetesimal accretion calculations in the Kuiper Belt that include fragmentation and velocity evolution. All models produce two power-law cumulative size distributions, NC ∝ r-2.5
Keck Pencil-Beam Survey for Faint Kuiper Belt Objects
We present the results of a pencil-beam survey of the Kuiper Belt using the Keck 10 m telescope. A single 0.01 deg2 field is imaged 29 times for a total integration time of 4.8 hr. Combining
How Long-Lived Are the Hypothetical Trojan Populations of Saturn, Uranus, and Neptune?
We investigate the possibility that fractions of the primordial populations at the triangular Lagrangian points of Saturn, Uranus, and Neptune have survived to the present and form (as yet
Possible Origin and Early Dynamical Evolution of the Pluto-Charon Binary
Abstract The dynamical state of the Pluto-Charon binary is distinctive in several respects including its well-known position in the Neptune 3:2 mean motion resonance, its librating argument of
The Radial Distribution of the Kuiper Belt
We examine the radial distribution of the Kuiper Belt objects (KBOs) using a method that is insensitive to observational bias effects. This technique allows the use of the discovery distances of all
The Effect of the Nebula on the Trojan Precursors
Abstract Numerical and analytical calculations demonstrate that small planetesimals exhibit long-term stability of libration about the L4 and L5 Lagrange equilibrium points at a proto-Jupiter's
...
...