title: Physics and chemistry of the solar nebula.
abstract: The solar system is thought to have begun in a flattened disk of gas and dust referred to traditionally as the solar nebula. Such a construct seems to be a natural product of the collapse of dense parts of giant molecular clouds, the vast star-forming regions that pepper the Milky Way and other galaxies. Gravitational, magnetic and thermal forces within the solar nebula forced a gradual evolution of mass toward the center (where the sun formed) and angular momentum (borne by a small fraction of the mass) toward the outer more distant regions of the disk. This evolution was accompanied by heating and a strong temperature contrast from the hot, inner regions to the cold, more remote parts of the disk. The resulting chemistry in the disk determined the initial distribution of organic matter in the planets; most of the reduced carbon species, in condensed form, were located beyond the asteroid belt (the 'outer' solar system). The Earth could have received much of its inventory of pre-biological material from comets and other icy fragments of the process of planetary formation in the outer solar system.
authors.affiliation: Lunar and Planetary Laboratory, University of Arizona, Tucson 85721, USA.
authors.forename: J I
authors.initials: JI
authors.lastname: Lunine
mesh_terms: D001256:Astronomy / Q000379:methods; D055598:Chemical Phenomena; D002621:Chemistry; D003080:Cold Temperature; D019443:Cosmic Dust; D005740:Gases; D008962:Models, Theoretical; D055585:Physical Phenomena; D010825:Physics; D016082:Solar System
chemical_list: D019443:Cosmic Dust; D005740:Gases