On the origin of fluorine-poor apatite in chondrite parent bodies
-
Francis M. McCubbin
, Jonathan A. Lewis
, Poorna Srinivasan
Abstract
We conducted a petrologic study of apatite within one LL chondrite, six R chondrites, and six CK chondrites. These data were combined with previously published apatite data from a broader range of chondrite meteorites to determine that chondrites host either chlorapatite or hydroxylapatite with ≤33 mol% F in the apatite X-site (unless affected by partial melting by impacts, which can cause F-enrichment of residual apatite). These data indicate that either fluorapatite was not a primary condensate from the solar nebula or that it did not survive lower temperature nebular processes and/or parent body processes. Bulk-rock Cl and F data from chondrites were used to determine that the solar system has a Cl/F ratio of 10.5 ± 1.0 (3σ). The Cl/F ratios of apatite from chondrites are broadly reflective of the solar system Cl/F value, indicating that apatite in chondrites is fluorine poor because the solar system has about an order of magnitude more Cl than F. The Cl/F ratio of the solar system was combined with known apatite-melt partitioning relationships for F and Cl to predict the range of apatite compositions that would form from a melt with a chondritic Cl/F ratio. This range of apatite compositions allowed for the development of a crude model to use apatite X-site compositions from achondrites (and chondrite melt rocks) to determine whether they derive from a volatile-depleted and/or differentiated source, albeit with important caveats that are detailed in the manuscript. This study further highlights the utility of apatite as a mineralogical tool to understand the origin of volatiles (including H2O) and the diversity of their associated geological processes throughout the history of our solar system, including at its nascent stage.
Funding statement: F.M.M., J.W.B., and L.P.K. were supported by NASA’s Planetary Science Research Program during this work. J.A.L. and J. J.B. were supported by the NASA Postdoctoral Program during this work. J.J.B. also recognizes support from start-up funds from the University of Arizona. S.M.E. acknowledges support from NASA Solar System Workings grant 80NSSC19K0752. B.A.A. was supported by a grant from the NASA Emerging Worlds Program awarded to F.M.M. T.C.P acknowledges support from the JETS contract at NASA Johnson Space Center.
Acknowledgments
We are grateful to the Meteorite Working Group, now the Antarctic Meteorite Review Panel of the Astromaterials Allocation Review Board, for carefully evaluating our sample requests, and we thank the curatorial staff at NASA Johnson Space Center for allocation of the Antarctic meteorites used in this study. The U. S. Antarctic meteorite samples are recovered by the Antarctic Search for Meteorites (ANSMET) program which has been funded by NSF and NASA and characterized and curated by the Department of Mineral Sciences of the Smithsonian Institution and Astromaterials Acquisition and Curation Office at NASA Johnson Space Center, respectively. We also thank Carl Agee of the Institute of Meteoritics at the University of New Mexico in Albuquerque, New Mexico, U. S.A. for the allocation of Parnallee, Karoonda, and NWA 8186, and we thank Lindsay Keller at NASA JSC for allowing us to use sections of Maralinga. F.M.M. wishes to thank Jim Webster for inspiring and encouraging him to work on apatite, both experimentally and in natural samples, during his formative years as a Ph.D. student at Stony Brook University. Jim was a dear friend, colleague, and mentor, and he is deeply missed. We are grateful to Daniel Harlov for the editorial handling of this manuscript and to Craig Walton and an anonymous reviewer for providing constructive and helpful comments that improved the overall quality of this work.
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