Many meteorites are full of tiny silicate spherules which are called chondrules (from Greek chondros, grain). Meteorites which contain such chondrules are called chondrites[?]. Chondrites[?] consist up to 80% of chondrules, embedded in a fine grained matrix.
Chondrites[?] represent the oldest solid material within our solar system and are believed to be the building blocks of the planetary system. Hence from the abundance of chondrules within these meteorites follow that an understanding of the formation of chondrules is important to also understand the initial development of the planetary system.
It is widely accepted that chondrules are formed by a rapid heating within minutes or less of solid precursor material to temperatures between 1500°C and 1900°C and subsequent melting, followed by a cooling within a few hours. However, the exact formation process is not known.
In particular the environmental setting, the energy source for the heating, and the precursor material are not known. The solar nebula or a protoplanetary environment are discussed as places of formation.
Proposed energy sources are:
- Impact melting
- Meteor ablation
- Hot inner nebula
- FU Orionis[?] outburst of the early sun
- Energetic outflows with bipolar shapes
- Nebular lightning
- Magnetic flares
- Accretion shocks
- Nebular shocks
In contrast, the fine graind matrix, in which the condrules are embedded after their accretion into the chondrites parent body, is assumed to have been condensed directly from the solar nebula.
Further Reading:
- Wlotzka F., Heide F. (1995) Meteorites: Messengers from Space, Springer Verlag, ISBN 0387581057
- Hewins R.H., Jones R.H., and Scott E.R.D. eds. (1996) Chondrules and the Protoplanetary Disk, Cambridge University Press, UK, ISBN 0521552885