Primordial light noble gases in the solar system

The isotopic signature of planetary helium (He-3/He-4 = (1.4 +/- 0.4) x 10(-4)) differs from that of solar helium (He-3/He-4 = (4.2 +/- 0.25) X 10(-4)), which was formed through deuterium fusion at the stage of Sun transition into the main sequence (t similar to 10(7) y). On the basis of this observation, it was concluded that the accretion of the protoplanetary cloud occurred at earlier stages. It was shown that the planetary gases were the primary constituents of the protoplanetary cloud. This conclusion was drawn from the following He-3/He-4 values. (1) Calculations of the compositions of shells of the massive supernova, whose explosion resulted in the formation of the solar system, show a value of 0.8 x 10(-4) for the H-envelope and 1.4 x 10(-4) for the complete ejection of the supernova. (2) SiC grains condensing in the solar wind of the presupernova show <2.6 x 10(-4). (3) Diamonds formed at the explosion of the supernova (less than or equal to1.5-1.7) x 10(-4). (4) Main planetary gas (Q phase), 1.6 x 10(-4) (5) The A-type gases of C chondrites average at (1.25 +/- 0.76) x 10(-4). (6) Jupiter's atmosphere (1.1 +/- 0.2) x 10(-4). (7) The protosolar cloud that gave rise to the proto-Sun, 1.42 x 10(-4). (8) It was assumed that gas-rich meteorites may contain the He-D component (He-3/He-4 = (1.5 +/- 1) x 10(-4)) of the primitive solar wind emitted by the Sun before it reached the main sequence. During the main sequence (greater than or equal to4.5 x 10(9) y), He-3/He-4 increased monotonously in the outer convection zone of the Sun due to the reaction d(n, gamma)H-3(beta (+), nu)He-3, which resulted in He-3/He-4 = (4.2 +/-0.25) x 10(-4) in the modern solar wind measured by the Apollo spacecraft. After the gas has dissipated from the inner layers of the protoplanetary cloud disk, the solar wind irradiated the surface of small fragments formed by the catastrophic fragmentation of large bodies with their subsequent gravitation-driven reaccumulation into meteorite parent bodies, which often contain solar gases. We present data on the element and isotopic compositions, energy characteristics, and abundances of solar gases and various types of planetary gases: Q gases, components Ne-A, Ne-E, and subsolar gases. The most feasible models of their origin are discussed.