Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.4013l&link_type=abstract
American Astronomical Society, DPS meeting #42, #40.13; Bulletin of the American Astronomical Society, Vol. 42, p.1001
Astronomy and Astrophysics
Astronomy
Scientific paper
Using the Canada-France Ecliptic Plane Survey (CFEPS) we have performed detailed modeling of Trans-Neptunian Objects (TNOs) in mean-motion resonances with Neptune, producing absolute population estimates for ten resonances. Because CFEPS is well-characterized, we are able to de-bias the survey to study the internal structure of the most populated resonances, especially the 3:2. To de-bias, we must account for the survey's pointings: TNOs will come to perihelion at specific ecliptic positions which depend on the resonant angle and the libration amplitude distribution. For the plutino Kozai subcomponent, the biases are more complicated, because pericenter will occur at high ecliptic latitudes. This results in ecliptic surveys being inherently biased against detecting Kozai resonators. We discuss constraints we can place on the inherent plutino Kozai fraction. For the 3:2 and 5:2 resonances, we are able to constrain the power-law H-magnitude distribution as well as the eccentricity, inclination, and libration amplitude distributions. The n:3, n:4, and 2:1 resonances have fewer detections, and we provide population estimates and constrain the inclination distributions. For poorly-sampled resonances (the 3:1 and 5:1), we give only rough population estimates. These are the first absolute population estimates for most of these resonances. In particular, we find the populations of H < 9 objects in the 3:2 and 5:2 resonances to be roughly equal. Although somewhat model-dependent, we find that the population of the 2:1 resonance is a factor of 4 smaller than that of the 3:2 resonance. If resonant TNOs were emplaced during migration late in the giant planet formation process, these population ratios may give clues about the state of the Kuiper Belt at the time of planet migration and about the migration rate. Our nominal 3:2/2:1/5:2 population ratios of 4/1/4 are not produced in published models of resonant TNO production.
Gladman Brett
Jones Rebecca
Kavelaars John J.
Lawler Samantha
Parker Joel
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