Few Comments on the Relation Between the Initial Proto-planetary Disc Model and the Oort Cloud Formation

Details Few Comments on the Relation Between the Initial Proto-planetary Disc Model and the Oort Cloud Formation Few Comments on the Relation Between the Initial Proto-planetary Disc Model and the Oort Cloud Formation

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009em%26p..105..367p&link_type=abstract

Earth, Moon, and Planets, Volume 105, Issue 2-4, pp. 367-371

Physics

Comets: General, Oort Cloud, Solar System: Formation

Scientific paper

A fraction of small bodies from the once existing proto-planetary disc was ejected, by the giant planets, to large heliocentric distances and start to build the comet Oort cloud. Considering four models of initial proto-planetary disc, we attempt to roughly map a dependence between the initial disc’s structure and some properties of the Oort cloud. We find that it is difficult to construct the proto-planetary disc if (i) the amount of heavy chemical elements in Jupiter and Saturn is as high as currently accepted and (ii) the total mass of the minimum-mass solar nebula is assumed to be lower than ≈0.05 M_{odot}. The behaviour of the Oort cloud formation does not crucially depend on the initial disc model. Some differences in its structure are obvious: since the cloud is known to be filled mainly by Uranus and Neptune, the efficiency of its formation is higher when the initial amount of particles in the Uranus-Neptune region is relatively higher. A significantly large number of Jupiter Trojans in our simulation appears, however, only in the case of the initially non-gapped disc, with the particles situated also close to the Jupiter’s orbit.

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