Volatiles are depleted in the CI chondrites and, in part, are not observable in the solar photosphere due to the high first excited atomic state of gases, resulting in the absence of characteristic absorption lines. Fractionation due to intense stellar winds early in solar history. Assuming that the sun lost a substantial fraction of its original mass during an early T-Tauri stage, the overall fractionation of the remaining material in the sun could be significant. A low level of ionization and separation of the bulk material from originally embedded magnetic fields would produce a fractionation of gas ions from solids and ions from neutral atoms and molecules. This mechanism may have been active in the interstellar cloud long before ignition of the sun, since magnetohydrodynamic processes are thought to play a crucial role in causing local inhomogeneities leading to stellar formation.
Today only solids spiral toward the sun.
The mass flux is insignificant relative to the mass of the solar convection zone, and it is not clear whether the atoms in the incoming particles are accreted to the sun or vaporized and swept out with the solar wind. However, this mechanism could have been significant in the early solar system when unaccreted materials were abundant and the solar surface temperature much lower. This would lead to enrichment of solids relative to gases in the photosphere. Enhancement of volatiles in the sun as the result of early large-scale planetesimal formation in the outer solar system. This would only affect H and He.