Other
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dda....40.0601i&link_type=abstract
American Astronomical Society, DDA meeting #40, #6.01; Bulletin of the American Astronomical Society, Vol. 41, p.898
Other
Scientific paper
Last years, new arguments in favor of the model of rarefied preplanetesimals - clumps have been found by several scientists. 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, could be more effective for rarefied preplanetesimals. For example, due to almost circular heliocentric orbits, duration of their motion inside the Hill sphere could be longer and minimum distances could be smaller than for solid bodies. Some collided rarefied preplanetesimals had a greater density at distances closer to their centers, and sometimes there could be two centers of contraction inside the rotating preplanetesimal formed as a result of a collision of two rarefied preplanetesimals. The observed separation distance can characterize the sizes of contracted preplanetesimals. In particular, binaries with close masses separated by a large distance and with any value of the eccentricity of the orbit of the secondary component relative to the primary component could be formed. Most of rarefied preasteroids could contract into solid asteroids before they collided with other preasteroids. Formation of some binaries could be caused by that the angular momentum that they obtained at the stage of rarefied preplanetesimals was greater than that could exist for solid bodies. During contraction of a rotating rarefied preplanetesimal, some material could form a cloud (that transformed into a disk) of material moving around the contracting primary. One or several satellites of the primary could be formed from this cloud. The angular momentum of a discovered trans-Neptunian or asteroidal binary is smaller than the typical angular momentum of two identical rarefied preplanetesimals having the same total mass and encountering to the Hill sphere from circular heliocentric orbits (Ipatov S.I. 2009, LPSC XL, #1021).
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