Paleomagnetic evidence for a disk substructure in the early solar system

Abstract

Astronomical observations and isotopic measurements of meteorites suggest that substructures are common in protoplanetary disks and may even have existed in the solar nebula. Here, we conduct paleomagnetic measurements of chondrules in CO carbonaceous chondrites to investigate the existence and nature of these disk sub-structures. We show that the paleomagnetism of chondrules in CO carbonaceous chondrites indicates the presence of a 101 $\pm$ 48 $\mu$T field in the solar nebula in the outer solar system ($\sim$3 to 7 AU from the Sun). The high intensity of this field relative to that inferred from inner solar system ($\lesssim$3 AU) meteorites indicates a factor of $\sim$5 to 150 mismatch in nebular accretion between the two reservoirs. This suggests substantial mass loss from the disk associated with a major disk substructure, possibly due to a magnetized disk wind.

arXiv comment16 pages, 3 figures, published in Science Advances

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Cited by in corpus (4)

• Three-dimensional Global Simulations of Type-II Planet-disk Interaction with a Magnetized Disk Wind: I. Magnetic Flux Concentration and Gap Properties
• Lifetime of the Outer Solar System Nebula From Carbonaceous Chondrites
• Magnetic disk winds in protoplanetary disks: Description of the model and impact on global disk evolution
• Unlocking planetesimal magnetic field histories: a refined, versatile model for thermal evolution and dynamo generation