Hiding in the howardites: Unequilibrated eucrite clasts as a guide to the formation of Vesta's crust
204 howardites in the National Meteorite Collection at the Smithsonian were examined for the presence of fine‐grained eucrite clasts, with the goal of better understanding the formation of the uppermost crust of asteroid 4Vesta. Eight clasts were identified and characterized in terms of their textur...
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| Published in | Meteoritics & planetary science Vol. 51; no. 12; pp. 2387 - 2402 |
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| Main Authors | , , |
| Format | Journal Article |
| Language | English |
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Hoboken
Blackwell Publishing Ltd
01.12.2016
Wiley Subscription Services, Inc |
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| ISSN | 1086-9379 1945-5100 |
| DOI | 10.1111/maps.12730 |
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| Abstract | 204 howardites in the National Meteorite Collection at the Smithsonian were examined for the presence of fine‐grained eucrite clasts, with the goal of better understanding the formation of the uppermost crust of asteroid 4Vesta. Eight clasts were identified and characterized in terms of their textures and mineral chemistry, and their degree of thermal metamorphism was assessed. The paucity of fine‐grained eucrites, both within the unbrecciated eucrites and as clasts within the howardites, suggests that they originate from small‐scale units on the surface of Vesta, most likely derived from partial melting. Six of the eight clasts described were found to be unequilibrated, meaning that they preserve their original crystallization trends. The vast majority of eucrites are at least partially equilibrated, making these samples quite rare and important for deciphering the petrogenesis of the vestan crust. Biomodal grain populations suggest that eucrite melts often began crystallizing pyroxene and plagioclase during their ascent to the surface, where they were subject to more rapid cooling, crystallization, and later metasomatism. Pyroxene compositions from this study and prior work indicate that the products of both primitive and evolved melts were present at the vestan surface after its formation. Two howardite thin sections contained multiple eucrite composition clasts with different crystallization and thermal histories; this mm‐scale diversity reflects the complexity of the current day vestan surface that has been observed by Dawn. |
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| AbstractList | 204 howardites in the National Meteorite Collection at the Smithsonian were examined for the presence of fine-grained eucrite clasts, with the goal of better understanding the formation of the uppermost crust of asteroid 4Vesta. Eight clasts were identified and characterized in terms of their textures and mineral chemistry, and their degree of thermal metamorphism was assessed. The paucity of fine-grained eucrites, both within the unbrecciated eucrites and as clasts within the howardites, suggests that they originate from small-scale units on the surface of Vesta, most likely derived from partial melting. Six of the eight clasts described were found to be unequilibrated, meaning that they preserve their original crystallization trends. The vast majority of eucrites are at least partially equilibrated, making these samples quite rare and important for deciphering the petrogenesis of the vestan crust. Biomodal grain populations suggest that eucrite melts often began crystallizing pyroxene and plagioclase during their ascent to the surface, where they were subject to more rapid cooling, crystallization, and later metasomatism. Pyroxene compositions from this study and prior work indicate that the products of both primitive and evolved melts were present at the vestan surface after its formation. Two howardite thin sections contained multiple eucrite composition clasts with different crystallization and thermal histories; this mm-scale diversity reflects the complexity of the current day vestan surface that has been observed by Dawn. |
| Author | Corrigan, C. M. Smith, Samantha E. Mayne, Rhiannon G. |
| Author_xml | – sequence: 1 givenname: Rhiannon G. surname: Mayne fullname: Mayne, Rhiannon G. email: r.g.mayne@tcu.edu, r.g.mayne@tcu.edu organization: Monnig Meteorite Collection and Gallery, School of Geology, Energy and the Environment, Texas Christian University, TCU Box 298830, Texas, 76109, Fort Worth, USA – sequence: 2 givenname: Samantha E. surname: Smith fullname: Smith, Samantha E. organization: Monnig Meteorite Collection and Gallery, School of Geology, Energy and the Environment, Texas Christian University, TCU Box 298830, Texas, 76109, Fort Worth, USA – sequence: 3 givenname: C. M. surname: Corrigan fullname: Corrigan, C. M. organization: Department of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, 10th & Constitution NW, DC, 20560-0119, Washington, USA |
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| Notes | istex:3CA4765425CCE8C2415A66BBA2E7BFD05B6DC613 Fig S1: SEM mineral maps created by combining the individual Fe (green), Ca (blue), and Al (red) X-ray maps. Pink areas show plagioclase, pyroxene is green in its low-Ca phase and blue in high-Ca. Black areas in the map denote SiO2 (phase unknown). Scales given are 250 μm across for each map. These maps are created by mosaicing tiles collected by the SEM. There was some shadowing in the bottom left of the images that has been mostly removed during image processing, but there are remnants that remain in some of the maps.Table S1: Howardites examined in this study. Table S2: Magnification of collected SEM data. ArticleID:MAPS12730 ark:/67375/WNG-H2VJFH1H-R ObjectType-Article-1 SourceType-Scholarly Journals-1 ObjectType-Feature-2 content type line 14 content type line 23 |
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| Snippet | 204 howardites in the National Meteorite Collection at the Smithsonian were examined for the presence of fine‐grained eucrite clasts, with the goal of better... 204 howardites in the National Meteorite Collection at the Smithsonian were examined for the presence of fine-grained eucrite clasts, with the goal of better... |
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| SubjectTerms | Crusts Crystallization Eucrites Formations Howardites Pyroxenes Surface layer Texture |
| Title | Hiding in the howardites: Unequilibrated eucrite clasts as a guide to the formation of Vesta's crust |
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