Formation Of The Haumea System: Checking Alternative Scenarios By N-body Based Numerical Simulations.

Details Formation Of The Haumea System: Checking Alternative Scenarios By N-body Based Numerical Simulations. Formation Of The Haumea System: Checking Alternative Scenarios By N-body Based Numerical Simulations.

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.4009t&link_type=abstract

American Astronomical Society, DPS meeting #42, #40.09; Bulletin of the American Astronomical Society, Vol. 42, p.1000

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Haumea is one of the most studied and probably one of the most interesting Trans-Neptunian Objects (TNOs) and a fast spinning dwarf planet (Rabinowitz et al., 2006; Thirouin et al. 2010) that has at least two satellites and whose orbital elements are related to a group/family of bodies.
A catastrophic collision at high relative velocity (around 3 km/s) between two bodies in the 1000-1500 km size range and a mass ratio 0.2 has been suggested for the formation of the 'family' and the presence of satellites (Brown et al. 2007). Leinhardt et al. (2010) proposed another mechanism in which two 1300 km size bodies undergo a grazing collision with reacculumation of part of the mass and dispersion of the rest, partly into satellites. The likelihood of both scenarios is small when tested against collisional and dynamical evolution model predictions of collisional probabilities. Furthermore, these mechanisms have trouble in explaining the velocity dispersion of the family members and the fast spin of Haumea.
Schlichting and Sari (2009) proposed that a former collision at low
speed formed a proto-satellite that should lately undergo a final impact finally leading to the current observed system.
In this work, we propose alternative mechanisms for the formation of the Haumea system ant test them by means of N-body numerical simulations (PKDGRAV code. Richardson, 1994).

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