Collisional Evolution Of The Trans-neptunian Region In A Dynamical Mass Depletion Environment.

Details Collisional Evolution Of The Trans-neptunian Region In A Dynamical Mass Depletion Environment. Collisional Evolution Of The Trans-neptunian Region In A Dynamical Mass Depletion Environment.

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.5504b&link_type=abstract

American Astronomical Society, DPS meeting #41, #55.04

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Scientific paper

Models of the collisional evolution of the trans-Neptunian region starting from a given initial distribution and mass lead to collisional mass grinding up to the 80-90%, depending on different boundary and physical conditions [1]. On the other hand, dynamical effects on their own are able to deplete most of the initial mass, as shown by the Nice model. The aim of the model presented here -furtherly developing our detailed collisional evolution model of the TNO region [1]- is to accurately follow the collisional evolution of different TNO populations, in the frame of the Nice model migration and dynamical excitation scenario[2], taking into account dynamical mass depletion at the same time. One of the constraints of that scenario is that, after some 700 Myr of moderate dynamical depletion, the mass needed at the beginning of the LHB period, in order to trigger the Jupiter-Saturn 2:1 resonance that caused the massive depletion of the disk and migration of planets to their present situation, was about 24 ME. We use this in order to constrain the possible initial mass and size distributions in the disk populations.
Our model tries to reproduce three observable constraints available: a) the number of objects larger than 2000 km with semimajor axes between 35 and 48 AU, b) the estimated number of the so-called classical "cold” population of TNOs with Hg<10 (CFEPS [3]), c) the size distribution slope estimated for objects larger than 100 km.
This study introduces interesting conclusions on the initial mass and size distribution required to get the present situation within the assumed frame, as well as considerations about the present day dynamical populations and the number and size of bodies yet to be discovered in the trans-Neptunian region.
[1] Benavidez & Campo Bagatin (2009)
[2] Levison et al. (2008)
[3] Kavelaars et al. (2009)

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