Fluid flow in chondritic parent bodies: Deciphering the compositions of planetesimals

Science

Volumn 286, Issue 5443, 1999, Pages 1331-1335

  Young, Edward D ^a   Ash, Richard D ^a,b   England, Philip ^a   Rumble III, Douglas ^b  

^a UNIVERSITY OF OXFORD   (United Kingdom)

^b GEOPHYSICAL LABORATORY   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

CHONDRITE; FLUID FLOW; METEORITE;

AQUEOUS SOLUTION; ARTICLE; ASTRONOMY; FLUID FLOW; MELTING POINT; PRIORITY JOURNAL; ROCK; TEMPERATURE DEPENDENCE;

EID: 0032718023     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.286.5443.1331     Document Type: Article

References (47)

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3. CV, CM, and CI refer to carbonaceous chondrites (C) with chemical similarities to the Vigarano (V), Mighei (M), and Ivuna (I) meteorites, respectively [J. T. Wasson, Meteorites: Their Record of Early Solar System History (Freeman, New York, 1985)]. CIs and CMs tend to be richer in volatile elements (such as S, Fe, K, and Na) than CVs. CIs are composed of hydrous minerals and have fractures filled with carbonate and sulfate minerals, whereas CVs are composed primarily of anhydrous minerals. CMs are intermediate, with roughly half of the minerals by weight being anhydrous.
4. A. Meibom and B. E. Clark, Meteorit. Planet. Sci. 34, 7 (1999).
5. 17O is a measure of the intercept for a mass fractionation curve and can be used to define the position of the curve on a three-isotope plot.
6. R. D. Ash, E. D. Young, D. Rumble III, G. J. MacPherson, Lunar Planet. Sci. Conf. XXX, CD-ROM (1999); E. D. Young and S. S. Russell, Science 282, 452 (1998).
7. R. D. Ash, E. D. Young, D. Rumble III, G. J. MacPherson, Lunar Planet. Sci. Conf. XXX, CD-ROM (1999); E. D. Young and S. S. Russell, Science 282, 452 (1998).
8. T. D. Swindle, M. W. Caffee, C. M. Hohenberg, Geochim. Cosmochim. Acta 52, 2215 (1988); C. J. Allègre, G. Manhès, C. Göpel, Geochim. Cosmochim. Acta 59, 1445 (1995); A. N. Krot et al., Meteorit. Planet. Sci. 34, 67 (1999).
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13. 17O for water relative to anhydrous rock [M. W. Rowe, R. N. Clayton, T. K. Mayeda, Geochim. Cosmochim. Acta 58, 5341 (1994); B. Choi, K. D. McKeegan, A. N. Krot, J. T. Wasson, Nature 392, 577 (1998)].
14. 17O for water relative to anhydrous rock [M. W. Rowe, R. N. Clayton, T. K. Mayeda, Geochim. Cosmochim. Acta 58, 5341 (1994); B. Choi, K. D. McKeegan, A. N. Krot, J. T. Wasson, Nature 392, 577 (1998)].
15. 17O for water relative to anhydrous rock [M. W. Rowe, R. N. Clayton, T. K. Mayeda, Geochim. Cosmochim. Acta 58, 5341 (1994); B. Choi, K. D. McKeegan, A. N. Krot, J. T. Wasson, Nature 392, 577 (1998)].
16. 17O for water relative to anhydrous rock [M. W. Rowe, R. N. Clayton, T. K. Mayeda, Geochim. Cosmochim. Acta 58, 5341 (1994); B. Choi, K. D. McKeegan, A. N. Krot, J. T. Wasson, Nature 392, 577 (1998)].
17. 17O for water relative to anhydrous rock [M. W. Rowe, R. N. Clayton, T. K. Mayeda, Geochim. Cosmochim. Acta 58, 5341 (1994); B. Choi, K. D. McKeegan, A. N. Krot, J. T. Wasson, Nature 392, 577 (1998)].
18. Equation 3 applies where the oxygen isotope exchange capacity of the rock has not been exhausted by protracted equilibration with flowing fluid [E. D. Young, in Reviews of Geophysics Supplement U.S. National Report to International Union of Geodesy and Geophysics 1991-1994 (American Geophysical Union, Washington, DC, 1995), p. 41]. Analytical equations that describe the effects of rock exchange capacity depletion are given by G. M. Dipple and J. M. Ferry [Geochim. Cosmochim. Acta 56, 3539 (1992)].
19. Equation 3 applies where the oxygen isotope exchange capacity of the rock has not been exhausted by protracted equilibration with flowing fluid [E. D. Young, in Reviews of Geophysics Supplement U.S. National Report to International Union of Geodesy and Geophysics 1991-1994 (American Geophysical Union, Washington, DC, 1995), p. 41]. Analytical equations that describe the effects of rock exchange capacity depletion are given by G. M. Dipple and J. M. Ferry [Geochim. Cosmochim. Acta 56, 3539 (1992)].
20. →
21. →
22. →
23. →
24. →
25. →
26. →
27. →
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29. -5. The latter is thought to characterize CAls in carbonaceous chondrites [A. K. Kennedy, J. R. Beckett, D. A. Edwards, I. D. Hutcheon, Geochim. Cosmochim. Acta 61, 1541 (1997)].
30. Interfacial liquid water at subfreezing temperatures, referred to as unfrozen water, is known to migrate through frozen terrestrial soils [M. S. Seyfried and M. D. Murdock, J. Hydrol. 202, 95 (1997)]. J. M. Rietmeijer [Nature 313, 293 (1985)] postulated that hydrous silicates could have been produced by reaction with unfrozen water on carbonaceous chondrite parent bodies. Calorimetric experiments demonstrate that carbonaceous chondrites can host unfrozen water [J. L. Gooding, Lunar Planet. Sci. Conf. XV, 228 (1984)].
31. Interfacial liquid water at subfreezing temperatures, referred to as unfrozen water, is known to migrate through frozen terrestrial soils [M. S. Seyfried and M. D. Murdock, J. Hydrol. 202, 95 (1997)]. J. M. Rietmeijer [Nature 313, 293 (1985)] postulated that hydrous silicates could have been produced by reaction with unfrozen water on carbonaceous chondrite parent bodies. Calorimetric experiments demonstrate that carbonaceous chondrites can host unfrozen water [J. L. Gooding, Lunar Planet. Sci. Conf. XV, 228 (1984)].
32. Interfacial liquid water at subfreezing temperatures, referred to as unfrozen water, is known to migrate through frozen terrestrial soils [M. S. Seyfried and M. D. Murdock, J. Hydrol. 202, 95 (1997)]. J. M. Rietmeijer [Nature 313, 293 (1985)] postulated that hydrous silicates could have been produced by reaction with unfrozen water on carbonaceous chondrite parent bodies. Calorimetric experiments demonstrate that carbonaceous chondrites can host unfrozen water [J. L. Gooding, Lunar Planet. Sci. Conf. XV, 228 (1984)].
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36. E. D. Young and S. S. Russell, Science 282, 452 (1998); S. S. Russell, L. A. Leshin, K. D. McKeegan, G. J. Macpherson, Meteorit. Planet. Sci. 32, A88 (1997); S. Sahijpal, K. D. McKeegan, A. N. Krot, D. Weber, A. A. Ulyanov, Meteorit. Planet. Sci., 34, A101 (1999).
37. E. D. Young and S. S. Russell, Science 282, 452 (1998); S. S. Russell, L. A. Leshin, K. D. McKeegan, G. J. Macpherson, Meteorit. Planet. Sci. 32, A88 (1997); S. Sahijpal, K. D. McKeegan, A. N. Krot, D. Weber, A. A. Ulyanov, Meteorit. Planet. Sci., 34, A101 (1999).
38. E. D. Young and S. S. Russell, Science 282, 452 (1998); S. S. Russell, L. A. Leshin, K. D. McKeegan, G. J. Macpherson, Meteorit. Planet. Sci. 32, A88 (1997); S. Sahijpal, K. D. McKeegan, A. N. Krot, D. Weber, A. A. Ulyanov, Meteorit. Planet. Sci., 34, A101 (1999).
39. 18O) [B. Choi, K. D. McKeegan, A. N. Krot, J. T. Wasson, Nature 392, 577 (1998); M. W. Rowe, R. N. Clayton, T. K. Mayeda, Geochim. Cosmochim. Acta 58, 5341 (1994)], which is consistent with what is expected, based on the initial equilibrium partitioning between magnetite and water on the slope 1.00 line.
40. 18O) [B. Choi, K. D. McKeegan, A. N. Krot, J. T. Wasson, Nature 392, 577 (1998); M. W. Rowe, R. N. Clayton, T. K. Mayeda, Geochim. Cosmochim. Acta 58, 5341 (1994)], which is consistent with what is expected, based on the initial equilibrium partitioning between magnetite and water on the slope 1.00 line.
41. 18O) [B. Choi, K. D. McKeegan, A. N. Krot, J. T. Wasson, Nature 392, 577 (1998); M. W. Rowe, R. N. Clayton, T. K. Mayeda, Geochim. Cosmochim. Acta 58, 5341 (1994)], which is consistent with what is expected, based on the initial equilibrium partitioning between magnetite and water on the slope 1.00 line.
42. Bulk porosities of carbonaceous chondrite groups range from 10 to 30% by volume [L. Wilson, K. Keil, S. J. Love, Meteorit. Planet. Sci. 34, 479 (1999)].
43. 17O, resulting in a somewhat poorer fit to the CM and CI data.
44. Conventional fluorination data are from R. N. Clayton and T. K. Mayeda [Earth Planet. Sci. Lett. 67, 151 (1984)] and from M. W. Rowe, R. N. Clayton, and T. K. Mayeda [Geochim. Cosmochim. Acta 58, 5341 (1994)]. Secondary ion mass spectrometry analyses of Murchison CM carbonate were reported by A. J. Brearley, J. M. Saxton, I. C. Lyon, and G. Turner [Lunar Planet. Sci. Conf. XXX, CD-ROM (1999)].
45. Conventional fluorination data are from R. N. Clayton and T. K. Mayeda [Earth Planet. Sci. Lett. 67, 151 (1984)] and from M. W. Rowe, R. N. Clayton, and T. K. Mayeda [Geochim. Cosmochim. Acta 58, 5341 (1994)]. Secondary ion mass spectrometry analyses of Murchison CM carbonate were reported by A. J. Brearley, J. M. Saxton, I. C. Lyon, and G. Turner [Lunar Planet. Sci. Conf. XXX, CD-ROM (1999)].
46. Conventional fluorination data are from R. N. Clayton and T. K. Mayeda [Earth Planet. Sci. Lett. 67, 151 (1984)] and from M. W. Rowe, R. N. Clayton, and T. K. Mayeda [Geochim. Cosmochim. Acta 58, 5341 (1994)]. Secondary ion mass spectrometry analyses of Murchison CM carbonate were reported by A. J. Brearley, J. M. Saxton, I. C. Lyon, and G. Turner [Lunar Planet. Sci. Conf. XXX, CD-ROM (1999)].
47. Supported by a grant from the Particle Physics and Astronomy Research Council (PPA/G/S/1998/00069) of the United Kingdom.