Computer Science
Scientific paper
Apr 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009eguga..1110080i&link_type=abstract
"EGU General Assembly 2009, held 19-24 April, 2009 in Vienna, Austria http://meetings.copernicus.org/egu2009, p.10080"
Computer Science
Scientific paper
Last years, new arguments in favor of the model of rarefied preplanetesimals - clumps have been found. There are several hypotheses of formation of binaries for a model of solid objects (see references in [1]). Ipatov [2] supposed that a considerable fraction of trans-Neptunian binaries could be formed at the stage of compression of rarefied preplanetesimals moved in almost circular orbits. For circular heliocentric orbits, two objects that entered inside the Hill sphere could move there for a longer time than those entered the sphere from eccentric heliocentric orbits. The diameters of preplanetesimals were greater than the diameters of solid planetesimals of the same masses. Therefore the models of binary formation due to the gravitational interactions or collisions of future binary components with an object (or objects) that were inside their Hill sphere, which were considered by several authors for solid objects, are more effective for rarefied preplanetesimals. Formulas for the angular momentum of two collided rarefied preplanetesimals - Hill spheres (with radii r1 and r2 and masses m1 and m2) moved in circular heliocentric orbits are presented in [3]. At a difference in their semimajor axes a equaled to Î °•(r1 + r2), the tangential velocity of collision is v? = kÎ °•(G•MS)1•2•(r1 + r2)•a-3•2 and the angular momentum Ks = kÎ °•(G•MS)1•2•(r1 + r2)2•m1•m2•(m1 + m2)-1•a-3•2, where Gis the gravitational constant, and MS is the mass of the Sun. At ra=(r1 + r2)/a«Î ° and ra«1, one can obtain kÎ ° ?(1-1.5•Î °2). The mean value of |kÎ °| equals to 0.6. It is equal to 2/3 for mean positive values of kÎ ° and to 0.24 for mean negative values of kÎ °. The resulting momentum is positive at 0< Î °
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