Constraining The Initial Conditions Of Trans-neptunian Populations

Details Constraining The Initial Conditions Of Trans-neptunian Populations Constraining The Initial Conditions Of Trans-neptunian Populations

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.2839b&link_type=abstract

American Astronomical Society, DPS meeting #42, #28.39

Physics

Scientific paper

After almost two decades of observations of the trans-neptunian region, we begin to understand the overall structure of the TNO populations in terms of dynamical features and absolute magnitudes number distributions. This knowledge is generated by a number of observables to which the outcomes of the models of the collisional and dynamical evolution of the region.
At the same time, the TNO region can be inserted in the global frame of the dynamical evolution of the giant planets, as described by the Nice model. This adds a constraint to the evolution of TNOs: the mass of the region, just before the start of the Late Heavy Bombardment (LHB) period, must overcome some 24 ME (Earth masses) (Levison et al., 2008).
We have improved our previous collisional evolution model (Benavidez & Campo Bagatin, 2009) and have developed a more complex code package (Asteroid-LIke Collisional ANd Dynamical Evolution Package: ALICANDEP) that includes statistical elimination of objects by dynamical effects within a frame of a disc migrating and gradually dynamically exciting, as well as the dynamical migration of objects between regions. Moreover, we added the possibility to distinguish between dynamically cold and hot bodies in the plutinos and classical regions and to keep track of primordial bodies in those regions.
Finally, we performed a large number of numerical simulations varying physical parameters and initial conditions in order to match the observables cited above and the dynamical conditions of the Nice model. Our results are in agreement with current observables. This allows to constraint the fragmentation physics and some of the initial conditions, like the initial mass, the distribution in different zones and the size distribution of objects. Some indication about the primordial existence, in the studied regions, of objects larger than current dwarf planets is also given.

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