Origin Of The Structure Of The Kuiper Belt During A Giant Planets Orbital Instability

Details Origin Of The Structure Of The Kuiper Belt During A Giant Planets Orbital Instability Origin Of The Structure Of The Kuiper Belt During A Giant Planets Orbital Instability

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.5403m&link_type=abstract

American Astronomical Society, DPS meeting #38, #54.03; Bulletin of the American Astronomical Society, Vol. 38, p.583

Astronomy and Astrophysics

Astronomy

1

Scientific paper

Despite 15 years of observations and modeling, the main properties of the Kuiper belt remain quite puzzling. In particular, there is no comprehensive model that can explain simultaenously: (i) the mass deficit of the Kuiper belt, (ii) its outer edge at the 1:2 mean motion resonance with Neptune, (iii) the co-existence of dynamically distinct populations (usually referred to as `hot' and `cold') with different physical properties and (iv) the characteristic semi-major axis vs. eccentricity distribution of the KBO orbits.
We propose a new dynamical model that can explain all the properties listed above. The primordial sculpting of the Kuiper belt is achieved in the framework of the `Nice model': a giant planet evolution model proposed in Tsiganis et al. (2005) and Gomes et al. (2005) to explain the orbital structure of the giant planets and the origin of the late heavy bombardment of the terrestrial planets.
In the light of our result, the Kuiper belt is most likely the relic of the planetesimal disk, that carries the scars of the violent restructuring of the outer solar system that occurred at the time of the late heavy bombardment.

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