An achondrite is a stony meteorite that does not contain chondrules. It consists of material similar to terrestrial basalts or plutonic rocks and has been differentiated and reprocessed to a lesser or greater degree due to melting and recrystallization on or within meteorite parent bodies. As a result, achondrites have distinct textures and mineralogies indicative of igneous processes.
|— Type —|
Achondrites account for about 8% of meteorites overall, and the majority (about two-thirds) of them are HED meteorites, possibly originating from the crust of asteroid 4 Vesta. Other types include Martian, Lunar, and several types thought to originate from as-yet unidentified asteroids. These groups have been determined on the basis of e.g. the Fe/Mn chemical ratio and the 17O/18O oxygen isotope ratios, thought to be characteristic "fingerprints" for each parent body.
Achondrites are classified into the following groups:
Primitive achondrites edit
Primitive achondrites, also called PAC group, are so-called because their chemical composition is primitive in the sense that it is similar to the composition of chondrites, but their texture is igneous, indicative of melting processes. To this group belong:
- Acapulcoites (after the meteorite Acapulco, Mexico)
- Lodranites (after the meteorite Lodran)
- Winonaites (after the meteorite Winona)
- Ureilites (after the meteorite Novy Ureii, Russia)
- Brachinites (after the meteorite Brachina)
Asteroidal achondrites edit
Asteroidal achondrites, also called evolved achondrites, are so-called because they have been differentiated on a parent body. This means that their mineralogical and chemical composition was changed by melting and crystallization processes. They are divided into several groups:
- HED meteorites (Vesta). They may have originated on the asteroid 4 Vesta, because their reflection spectra are very similar. They are named after the initial letters of the three subgroups:
Lunar meteorites edit
Martian meteorite edit
See also edit
- Etymology: from the prefix a- (privative a) and the word chondrite.
- Recommended classifications: Eucrite-pmict
- Achondrite, Encyclopædia Britannica
- Sahijpal, S.; Soni, P.; Gagan, G. (2007). "Numerical simulations of the differentiation of accreting planetesimals with 26Al and 60Fe as the heat sources". Meteoritics & Planetary Science. 42 (9): 1529–1548. Bibcode:2007M&PS...42.1529S. doi:10.1111/j.1945-5100.2007.tb00589.x.
- Gupta, G.; Sahijpal, S. (2010). "Differentiation of Vesta and the parent bodies of other achondrites". J. Geophys. Res. Planets. 115 (E8). Bibcode:2010JGRE..115.8001G. doi:10.1029/2009JE003525. S2CID 129905814.
- Mason, B. (1962). Meteorites. New York: John Wiley.
- Mittlefehldt, David W.; McCoy, Timothy J.; Goodrich, Cyrena Anne; Kracher, Alfred (1998). "Non-chondritic Meteorites from Asteroidal Bodies". Reviews in Mineralogy and Geochemistry. 36 (1): 4.1–4.195.
- O. Richard Norton. The Cambridge encyclopedia of meteorites. UK, Cambridge University Press, 2002. ISBN 0-521-62143-7.
- Drake, M. J. (2001). "The eucrite/Vesta story". Meteoritics and Planetary Science. 36 (4): 501–513. Bibcode:2001M&PS...36..501D. doi:10.1111/j.1945-5100.2001.tb01892.x. S2CID 128394153.
- Treiman, A. H. (2000). "The SNC meteorites are from Mars". Planetary and Space Science. 48 (12–14): 1213–1230. Bibcode:2000P&SS...48.1213T. doi:10.1016/S0032-0633(00)00105-7.
- Achondrite Images from Meteorites Australia