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- Title
Lifetime of the Outer Solar System Nebula From Carbonaceous Chondrites.
- Authors
Borlina, Cauê S.; Weiss, Benjamin P.; Bryson, James F. J.; Armitage, Philip J.
- Abstract
The evolution and lifetime of protoplanetary disks (PPDs) play a central role in the formation and architecture of planetary systems. Astronomical observations suggest that PPDs evolve in two timescales, accreting onto the star for up to several million years (Myr) followed by gas dissipation within ≲1 Myr. Because solar nebula magnetic fields are sustained by the gas of the protoplanetary disk, we can use paleomagnetic measurements to infer the lifetime of the solar nebula. Here, we use paleomagnetic measurements of meteorites to constrain this lifetime and investigate whether the solar nebula had a two‐timescale evolution. We report on paleomagnetic measurements of bulk subsamples of two CO carbonaceous chondrites: Allan Hills A77307 and Dominion Range 08006. If magnetite in these meteorites can acquire a crystallization remanent magnetization that recorded the ambient field during aqueous alteration, our measurements suggest that the local magnetic field strength at the CO parent body location was <0.9 μT at some time between 2.7 and 5.1 Myr after the formation of calcium‐aluminum‐rich inclusions. Coupled with previous paleomagnetic studies, we conclude that the dissipation of the solar nebula in the 3–7 AU region occurred <1.5 Myr after the dissipation of the nebula in the 1–3 AU region, suggesting that protoplanetary disks go through a two‐timescale evolution in their lifetime, consistent with dissipation by photoevaporation and/or magnetohydrodynamic winds. We also discuss future directions necessary to obtain robust records of solar nebula fields using bulk chondrites, including obtaining ages from meteorites and experimental work to determine how magnetite acquires magnetization during chondrite parent body alteration. Plain Language Summary: Magnetic fields play an important role during planetary formation. That is because during the first few million years of the solar system, when only gas and dust were present, magnetic fields are coupled to the gas. Meteorites, rocks that formed during the early stages of the solar system that made their way to the Earth, could have recorded this ambient magnetic field and maintained this record for billions of years. By conducting paleomagnetic measurements of meteorites and coupling our measurements with previous work, we establish when the gas in the early solar system dissipated. Our results indicate that the gas existed for ∼3 million years and dispersed within <1.5 million years. This is consistent with mechanisms for gas dispersal that involve heating from the young Sun and magnetic‐driven winds expelling gas from the solar system. We also discuss uncertainties associated with paleomagnetic measurements and what the community can do in the future to obtain robust records of magnetic fields from the early solar system. Key Points: Paleomagnetic measurements of CO chondrites suggest solar nebula dissipation within 2.7–5.1 Myr after the formation of the solar systemThe solar nebula went through a two‐timescale evolution, consistent with dissipation through photoevaporation and/or magnetized windsWe discuss the uncertainties associated with paleomagnetic measurements of bulk chondrites and recommend future directions for the field
- Subjects
SOLAR system; CHONDRITES; SOLAR magnetic fields; ASTRONOMICAL observations; NEBULAE; REMANENCE; PROTOPLANETARY disks
- Publication
Journal of Geophysical Research. Planets, 2022, Vol 127, Issue 7, p1
- ISSN
2169-9097
- Publication type
Article
- DOI
10.1029/2021JE007139