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Major components of chondrites are chondrules and matrix. Measurements of thevolatile abundance in Semarkona chondrules suggest that chondrules formed in adense clump that had a higher solid density than the gas density in the solarnebula. We investigate collisions between chondrules and matrix in the surfaceregion of dense clumps using fluffy aggregate growth models. Our simulationsshow that the collisional growth of aggregates composed of chondrules andmatrix takes place in the clumps well before they experience gravitationalcollapse. The internal structure of chondrite parent bodies (CPBs) can bethereby determined by aggregate growth. We find that the aggregate growthgenerates two scales within CPBs. The first scale is involved with the smallscale distribution of chondrules and determined by the early growth stage,where chondrules accrete aggregates composed of matrix grains. This accretioncan reproduce the thickness of the matrix layer around chondrules found inchondrites. The other scale is related to the large scale distribution ofchondrules. Its properties (e.g., the abundance of chondrules and the overallsize) depend on the gas motion within the clump, which is parameterized in thiswork. Our work thus suggests that the internal structure of CPBs may provideimportant clues about their formation conditions and mechanisms.

Aggregate Growth and Internal structures of Chondrite Parent Bodies Forming from Dense Clumps