Formation and Dynamical Evolution of the Neptune Trojans - the Influence of the Initial Solar System Architecture - Astrophysics > Earth and Planetary AstrophysicsReportar como inadecuado




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Abstract: In this work, we investigate the dynamical stability of pre-formed NeptuneTrojans under the gravitational influence of the four giant planets in compactplanetary architectures, over 10 Myr. In our modelling, the initial orbitallocations of Uranus and Neptune aN were varied to produce systems in whichthose planets moved on non-resonant orbits, or in which they lay in theirmutual 1:2, 2:3 and 3:4 mean-motion resonances MMRs. In total, 420simulations were carried out, examining 42 different architectures, with atotal of 840000 particles across all runs. In the non-resonant cases, theTrojans suffered only moderate levels of dynamical erosion, with the mostcompact systems those with aN less than or equal 18 AU losing around 50% oftheir Trojans by the end of the integrations. In the 2:3 and 3:4 MMR scenarios,however, dynamical erosion was much higher with depletion rates typicallygreater than 66% and total depletion in the most compact systems. The 1:2resonant scenarios featured disruption on levels intermediate between thenon-resonant cases and other resonant scenarios, with depletion rates of theorder of tens of percent. Overall, the great majority of plausiblepre-migration planetary architectures resulted in severe levels of depletion ofthe Neptunian Trojan clouds. In particular, if Uranus and Neptune formed neartheir mutual 2:3 or 3:4 MMR and at heliocentric distances within 18 AU asfavoured by recent studies, we found that the great majority of pre-formedTrojans would have been lost prior to Neptune-s migration. This strengthens thecase for the great bulk of the current Neptunian Trojan population having beencaptured during that migration.



Autor: P. S. Lykawka, J. Horner, B. W. Jones, T. Mukai

Fuente: https://arxiv.org/







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