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Extraterrestrial He in Sediments: From Recorder of Asteroid Collisions to Timekeeper of Global Environmental Changes

  • David McGee
  • Sujoy Mukhopadhyay
Chapter
Part of the Advances in Isotope Geochemistry book series (ADISOTOPE)

Abstract

Most 3He in deep-sea sediments is derived from fine-grained extraterrestrial matter known as interplanetary dust particles (IDPs). These particles, typically <50 μm in diameter, are sufficiently small to retain solar wind-implanted He with high 3He/4He ratios during atmospheric entry heating. This extraterrestrial 3He (3HeET) is retained in sediments for geologically long durations, having been detected in sedimentary rocks as old as 480 Ma. As a tracer of fine-grained extraterrestrial material, 3HeET offers unique insights into solar system events associated with increased IDP fluxes, including asteroid break-up events and comet showers. Studies have used 3HeET to identify IDP flux changes associated with a Miocene asteroid break-up event and a likely comet shower in the Eocene. During much of the Cenozoic, 3HeET fluxes have remained relatively constant over million-year timescales, enabling 3HeET to be used as a constant flux proxy for calculating sedimentary mass accumulation rates and constraining sedimentary age models. We review studies employing 3HeET-based accumulation rates to estimate the duration of carbonate dissolution events associated with the K/Pg boundary and Paleocene-Eocene Thermal Maximum. Additionally, 3HeET has been used to quantify sub-orbital variability in fluxes of paleoproductivity proxies and windblown dust. In order to better interpret existing records and guide the application of 3HeET in novel settings, future work requires constraining the carrier phase(s) of 3HeET responsible for long-term retention in sediments, better characterizing the He isotopic composition of the terrigenous end-member, and understanding why observed extraterrestrial 3He fluxes do not match the predicted variability of IDP accretion rate over orbital timescales.

Keywords

Solar Wind Accretion Rate Late Eocene Asteroid Belt Ferromanganese Crust 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

Notes

Acknowledgement

The authors would like to thank Ken Farley for reviewing this chapter.

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Authors and Affiliations

  1. 1.Department of Earth, Atmospheric and Planetary SciencesMassachusetts Institute of TechnologyCambridgeUSA
  2. 2.Department of Earth and Planetary SciencesHarvard UniversityCambridgeUSA

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