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Published June 23, 2020 | Supplemental Material + Published
Journal Article Open

Massive formation of early diagenetic dolomite in the Ediacaran ocean: Constraints on the "dolomite problem"

Abstract

Paleozoic and Precambrian sedimentary successions frequently contain massive dolomicrite [CaMg(CO₃)₂] units despite kinetic inhibitions to nucleation and precipitation of dolomite at Earth surface temperatures (<60 °C). This paradoxical observation is known as the "dolomite problem." Accordingly, the genesis of these dolostones is usually attributed to burial–hydrothermal dolomitization of primary limestones (CaCO₃) at temperatures of >100 °C, thus raising doubt about the validity of these deposits as archives of Earth surface environments. We present a high-resolution, >63-My-long clumped-isotope temperature (T_(Δ47)) record of shallow-marine dolomicrites from two drillcores of the Ediacaran (635 to 541 Ma) Doushantuo Formation in South China. Our T∆47 record indicates that a majority (87%) of these dolostones formed at temperatures of <100 °C. When considering the regional thermal history, modeling of the influence of solid-state reordering on our T_(Δ47) record further suggests that most of the studied dolostones formed at temperatures of <60 °C, providing direct evidence of a low-temperature origin of these dolostones. Furthermore, calculated δ¹⁸O values of diagenetic fluids, rare earth element plus yttrium compositions, and petrographic observations of these dolostones are consistent with an early diagenetic origin in a rock-buffered environment. We thus propose that a precursor precipitate from seawater was subsequently dolomitized during early diagenesis in a near-surface setting to produce the large volume of dolostones in the Doushantuo Formation. Our findings suggest that the preponderance of dolomite in Paleozoic and Precambrian deposits likely reflects oceanic conditions specific to those eras and that dolostones can be faithful recorders of environmental conditions in the early oceans.

Additional Information

© 2020 National Academy of Sciences. Published under the PNAS license. Edited by Mark Thiemens, University of California San Diego, La Jolla, CA, and approved May 8, 2020 (received for review September 25, 2019). PNAS first published June 8, 2020. We thank Uri Ryb, Maoyan Zhu, Xuan Qiu, Changqun Cao, Xinjun Wang, Hongbin Zhang, Meng Cheng, Keyi Cheng, Qingsong Liu, Jinjiang Pan, Wei Shi, and the Tripati Research Group for laboratory assistance and/or helpful discussions. This study was supported by the National Natural Science Foundation of China (NSFC) (Grants 41825019, 41821001, 41573099), NSFC–Research Councils United Kingdom_National Environment Research Council Program (Grant 41661134048), the National Key R&D Program of China (Grant 2016YFA0601100), Strategic Priority Research Program of Chinese Academy of Sciences (Grant XDB26000000), 111 Project of China (Grant BP0820004), China University of Geosciences–Wuhan (Grant CUGCJ1710), the Department of Energy through Basic Energy Sciences (Grant DE-FG02-13ER16402), and an award from "Laboratoire Excellence" LabexMER (Grant ANR-10-LABX-19), co-funded by a grant from the French government under the program Investissements d'Avenir. The National Aeronautics and Space Administration Astrobiology Institute under Cooperative Agreement NNA15BB03A issued through the Science Mission Directorate also provided funds (T.W.L.). Author contributions: C.L. designed research; B.C., I.F., A.T., M.K.L., I.M., Z.A., Z.S., J.T., and J.H. performed research; B.C., C.L., D.L., I.F., A.T., M.K.L., I.M., G.L., S.X., J.H., and A.I. analyzed data; and B.C., C.L., D.L., T.J.A., T.W.L. and A.I. wrote the paper with assistance from all authors. The authors declare no competing interest. This article is a PNAS Direct Submission. This article contains supporting information online at https://www.pnas.org/lookup/suppl/doi:10.1073/pnas.1916673117/-/DCSupplemental.

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Additional details

Created:
August 22, 2023
Modified:
October 20, 2023