scholarly journals Chondrules in CK carbonaceous chondrites and thermal history of the CV-CK parent body

2016 ◽  
Vol 51 (3) ◽  
pp. 547-573 ◽  
Author(s):  
Noël Chaumard ◽  
Bertrand Devouard
Keyword(s):  
Thermal History ◽  
Parent Body ◽  
Carbonaceous Chondrites ◽  
History Of

Thermal history of the H-chondrite parent body: Implications for metamorphic grade and accretionary time-scales

2013 ◽  
Vol 119 ◽  
pp. 302-321 ◽  
Author(s):  
Marc Monnereau ◽  
Michael J. Toplis ◽  
David Baratoux ◽  
Jérémy Guignard
Keyword(s):  
Time Scales ◽  
Thermal History ◽  
Parent Body ◽  
Metamorphic Grade ◽  
History Of

scholarly journals Compositions and microstructures of CB sulfides: Implications for the thermal history of the CB chondrite parent body

2017 ◽  
Vol 52 (10) ◽  
pp. 2193-2219 ◽  
Author(s):  
Poorna Srinivasan ◽  
Rhian H. Jones ◽  
Adrian J. Brearley
Keyword(s):  
Thermal History ◽  
Parent Body ◽  
History Of

scholarly journals Constraints on the ice composition of carbonaceous chondrites from their magnetic mineralogy

2021 ◽  
Author(s):  
Sanjana Sridhar ◽  
James Bryson ◽  
Ashley King ◽  
Richard Harrison
Keyword(s):  
Size Range ◽  
Parent Body ◽  
Carbonaceous Chondrites ◽  
Magnetic Mineralogy ◽  
Aqueous Alteration ◽  
First Order ◽  
Direct Replacement ◽  
History Of ◽  
Bulk Chemical ◽  
Weathering Effects

Carbonaceous chondrites experienced varying degrees of aqueous alteration on their parent asteroids, which influenced their mineralogies, textures, and bulk chemical and isotopic compositions. Although this alteration was a crucial event in the history of these meteorites, their various alteration pathways are not well understood. One phase that formed during this alteration was magnetite, and its morphology and abundance vary between and within chondrite groups, providing a means of investigating chondrite aqueous alteration. We measured bulk magnetic properties and first-order reversal curve (FORC) diagrams of CM, CI, CO, and ungrouped C2 chondrites to identify the morphology and size range of magnetite present in these meteorites. We identify two predominant pathways of aqueous alteration among these meteorites that can be distinguished by the resultant morphology of magnetite. In WIS 91600, Tagish Lake, and CI chondrites, magnetite forms predominantly from Fe-sulfides as framboids and stacked plaquettes. In CM and CO chondrites, <0.1 μm single-domain (SD) magnetite and 0.1–5 μm vortex (V) state magnetite formed predominantly via the direct replacement of metal and Fe-sulfides. After ruling out differences in temperature, water:rock ratios, terrestrial weathering effects, and starting mineralogy, we hypothesise that the primary factor controlling the pathway of aqueous alteration was the composition of the ice accreted into each chondrite group’s parent body. Nebula condensation sequences predict that the most feasible method of appreciably evolving ice concentrations was the condensation of ammonia, which will have formed a more alkaline hydrous fluid upon melting, leading to fundamentally different conditions that may have caused the formation of different magnetite morphologies. As such, we suggest that WIS 91600, Tagish Lake, and the CI chondrites accreted past the ammonia ice line, supporting a more distal or younger accretion of their parent asteroids.

Hf–W thermochronometry: II. Accretion and thermal history of the acapulcoite–lodranite parent body

2009 ◽  
Vol 284 (1-2) ◽  
pp. 168-178 ◽  
Author(s):  
Mathieu Touboul ◽  
Thorsten Kleine ◽  
Bernard Bourdon ◽  
James A. Van Orman ◽  
Colin Maden ◽  
...  
Keyword(s):  
Thermal History ◽  
Parent Body ◽  
History Of

scholarly journals An Almahata Sitta EL3 fragment: Implications for the Unique Thermal History of Enstatite Chondrites

2021 ◽  
Author(s):  
Makoto Kimura ◽  
Michael K. Weisberg ◽  
Asako Takaki ◽  
Naoya Imae ◽  
Akira Yamaguchi
Keyword(s):  
High Temperature ◽  
Short Duration ◽  
Thermal History ◽  
Parent Body ◽  
The Other ◽  
Thermal Event ◽  
Other Hand ◽  
Typical Type ◽  
History Of ◽  
Type 3

Abstract Almahata Sitta is a polymict breccia, consisting of many kinds of clasts. Here we present our mineralogical and petrological results on an EL3 fragment, MS-177 from Almahata Sitta. This fragment shows a typical type 3 chondritic texture, consisting of well-defined chondrules often with olivine, isolated silicate minerals, and opaque nodules. Although these components are typical of EL3 chondrites, the mineral abundances and compositions are different from the other EL3s. Diopside is highly abundant. On the other hand, perryite and daubreelite were not found. The major pyroxene is orthoenstatite, and the silica phase is quartz. Fe-Ni metal has relatively high P contents. Troilite is enriched in Cr and Mn. Keilite and buseckite are present in MS-177. From the mineralogy and texture, MS-177 experienced a high-temperature event under subsolidus conditions. Shock-induced heating for a short duration might explain this high-temperature event. This is supported by shock-induced darkened feature of MS-177. We suggest that other E3 chondrites also experienced heating events under such subsolidus conditions on their parent bodies. On the other hand, the high abundance of diopside cannot be explained by a secondary thermal event and may have been a primary feature of MS-177, formed before accretion to the parent body.

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