Meteorites usually derive from primitive materials that condensed and accreted from the gas-and dust-containing presolar disk. Most of them were altered by postaccretionary processes, but some survived essentially integrity. These primitive chondrites are recognizable usually from isotopic abundance characteristics. Based on mineral-petrologic characteristics and their origin we can classify known meteorites into a much smaller number of types. The authors summarized evolved process from nebula to meteorite in early solar system.  Some new insights based on these data are that the early solar system experienced a variety of nucleosynthetic input, the dynamic entity with transient heating events, and the system of plantesimals and planets evolved more rapidly than previously expected.