Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.0912i&link_type=abstract
American Astronomical Society, DPS meeting #42, #9.12; Bulletin of the American Astronomical Society, Vol. 42, p.957
Astronomy and Astrophysics
Astronomy
Scientific paper
There are several known bodies in the solar system that share the same mean orbit. This kind of motion is denominated co-orbital and is characterized according to the center of libration of the critic argument θ=λ- λ', where λ and λ' represents the mean longitude of the minor and major bodies respectively. When the body librates around L4 or L5 the orbit is said tadpole, when oscillates around θ=180, involving L3, L4 e L5 the orbit is called horseshoe, and when the oscillation occurs close to zero, the body is a quasi-satellite. In this work we studied the effects of different satellite/planet mass ratios and different satellite-planet distance during the formation of co-orbital objects through of the congenital formation model. The dynamic system studied consists of a central body, a secondary body and a cloud of planetesimals randomly distributed in a sector around L4 or L5. The sector is delimited by an arc of 70°, centered on the Lagrangian point, and the extreme orbital radii of the largest tadpole orbit. The preliminary results show that for satellite-planet mass ratio equals to 1e-3 occurs the formation of bodies with relative mass larger than 0.6e-6 of the central body's mass, which is a the limit found by Beaugé et al. (2007). However, in this case, we used a radial distance much smaller than Beagué et al. (2007). This shows that the limiting mass of larger body created is not dependent only on the satellite-planet mass ratio.
Cabo Winter Othon
Izidoro André
Tsuchida Masayoshi
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