Mineralogical characterization of primitive, type-3 lithologies in Rumuruti chondrites

被引:32
作者
Bischoff, A
机构
[1] Inst Planetol, D-48149 Munster, Germany
[2] Interdisciplinary Ctr Electron Microscopy & Micro, D-48149 Munster, Germany
来源
METEORITICS & PLANETARY SCIENCE | 2000年 / 35卷 / 04期
关键词
D O I
10.1111/j.1945-5100.2000.tb01453.x
中图分类号
P3 [地球物理学]; P59 [地球化学];
学科分类号
0708 ; 070902 ;
摘要
Rumuruti (R) chondrites constitute a new, well-established chondrite group different from the carbonaceous, ordinary, and enstatite chondrites. Many of these samples are gas-rich regolith breccias showing the typical light-dark structure and consist of abundant fragments of various parent-body lithologies embedded in a fine-grained olivine-rich matrix. Unequilibrated type-3 lithologies among these fragments have frequently been mentioned in various publications. In this study, detailed mineralogical data on seven primitive fragments from the R-chondrites Dar al Gani 013 and Hughes 030 are presented. The fragments range from similar to 300 mu m in size up to several millimeters. Generally, the main characteristics can be summarized as follows: (1) Unequilibrated type-3 fragments have a well-preserved chondritic texture with a chondrule-to-matrix ratio of similar to 1:1. Chondrules and chondrule fragments are embedded in a fine-grained olivine-rich matrix. Thus, the texture is quite similar to that of type-3 carbonaceous chondrites. (2) In all cases, matrix olivines in type-3 fragments have a significantly higher Fa content (44-57 mol%) than olivines in other (equilibrated) lithologies (38-40 mol% Fa). (3) Olivines and pyroxenes occurring within chondrules or as fragments are highly variable in composition (Fa(0-65) and Fs(0-33), respectively) and, generally, more magnesian than those found in equilibrated R chondrites. Agglomerated material of the R-chondrite parent body (or bodies) was highly unequilibrated. It is suggested that the material that accreted to form the parent body consisted of chondrules and chondrule fragments, mainly having Mg-rich silicate constituents, and Fe-rich highly oxidized fine-grained materials. The dominating phase of this fine-grained material may have been Fa-rich olivine from the beginning. The brecciated whole rocks, the R-chondrite regolith breccias, were not significantly reheated subsequent to brecciation or during lithification, as indicated by negligible degree of equilibration between matrix components and Mg-rich olivines and pyroxenes in primitive type-3 fragments.
引用
收藏
页码:699 / 706
页数:8
相关论文
共 29 条
[11]  
Gibbons R.V., 1975, P LUN SIC C, V6th, P3143
[12]   The Meteoritical Bulletin, No. 83, 1999 July [J].
Grossman, JN .
METEORITICS & PLANETARY SCIENCE, 1999, 34 :A169-A186
[13]  
GROSSMAN JN, 1998, METEORITES EARLY SOL, P619
[14]  
JACKEL A, 1996, LUNAR PLANET SCI, V27, P595
[15]   The compositional classification of chondrites .7. The R chondrite group [J].
Kallemeyn, GW ;
Rubin, AE ;
Wasson, JT .
GEOCHIMICA ET COSMOCHIMICA ACTA, 1996, 60 (12) :2243-2256
[16]   FROM REGOLITH TO ROCK BY SHOCK [J].
KIEFFER, SW .
MOON, 1975, 13 (1-3) :301-320
[17]   PETROGRAPHIC VARIATIONS AMONG CARBONACEOUS CHONDRITES OF VIGARANO TYPE [J].
MCSWEEN, HY .
GEOCHIMICA ET COSMOCHIMICA ACTA, 1977, 41 (12) :1777-1790
[18]   PECORA-ESCARPMENT-91002 - A MEMBER OF THE NEW RUMURUTI (R) CHONDRITE GROUP [J].
RUBIN, AE ;
KALLEMEYN, GW .
METEORITICS, 1994, 29 (02) :255-263
[19]   CARLISLE LAKES AND ALLAN HILLS 85151 - MEMBERS OF A NEW CHONDRITE GROUPLET [J].
RUBIN, AE ;
KALLEMEYN, GW .
GEOCHIMICA ET COSMOCHIMICA ACTA, 1989, 53 (11) :3035-3044
[20]  
SCHAAL RB, 1980, P LUNAR PLANET SCI C, P1679