Hostname: page-component-586b7cd67f-t7fkt Total loading time: 0 Render date: 2024-11-26T09:30:32.291Z Has data issue: false hasContentIssue false

Microstructures and Microanalysis in ALH84001: Minerals or Martians?

Published online by Cambridge University Press:  02 July 2020

Ralph P. Harvey
Affiliation:
Department of Geological Sciences, Case Western Reserve University, ClevelandOH44106-7216
John Bradley
Affiliation:
MVA Inc., 5500 Oakbrook Parkway #200, Norcross, GA30093; School of Materials Science and Engineering, Georgia Institute of Technology, Atlanta, GA30332-0245
Harry Y. McSween Jr.
Affiliation:
Department of Geological Sciences, University of Tennessee, KnoxvilleTN37996-1410
Get access

Extract

The martian meteorite ALH84001 leapt into the spotlight in late 1996 when a NASA-led research team suggested that it contained evidence of biotic activity on ancient Mars. ALH84001 is unique among the martian meteorites- a cumulate rock made up predominantly of orthopyroxene, with interstitial maskelynite (feldspar turned into a diaplectic glass by shock), apatite, chromite and sulfides. Highly brecciated fracture zones cut through the rock, presumably a result of impacts, and within these zones is a variable amount of secondary carbonate. This carbonate, the most extensive secondary mineral found in any martian meteorite, formed during significant interaction between martian crust and volatiles, and represents a unique access point toward understanding the environment of ancient Mars. However, the conditions under which this carbonate formed are less clear. While claims for evidence of biotic activity are predicated on carbonate formation at low (<100°C) temperatures under water-rich conditions, other research suggests much less hospitable conditions, with little water present and formation temperatures approaching 700°C.

Type
Microscopy of Ceramics and Minerals
Copyright
Copyright © Microscopy Society of America

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

References:

1.McKay, D.S. et al., Science 273 (1996) 924 .CrossRefGoogle Scholar
2.Harvey, R. P. and McSween, H.Y. Jr., Nature, 382, (1996) 49.CrossRefGoogle Scholar
3.Scott, E. R. D. et al., Nature 387 (1997) 377.CrossRefGoogle Scholar
4.Harvey, R. P. and McSween, H.Y. JrMeteoritics 29, (1994) 472.Google Scholar
5.Romanek, C. S. et al., Nature 372 (1994) 655.CrossRefGoogle Scholar
6.Leshin, L. A. et al., Geochimica et Cosmochimica Acta, (1998) (in press).Google Scholar
7.Bradley, J. P. et a\.,Geochimica et Cosmochimica Acta 60, (1996) 5149.CrossRefGoogle Scholar
8.Bradley, J. P. et al., Meteoritics and Planetary Science (1998) (in press).Google Scholar
9.Thomas-Keprta, K. et al., Abstracts Lunar and Planetary Science Conference 28 (1997) 1433.Google Scholar
10.Bradley, J. P. et al., Nature 390, (1997) 454.CrossRefGoogle Scholar
11. This work was funded by NASA's Ancient Martian Meteorite Program (to RPH).Google Scholar