Paleomagnetic evidence for a disk substructure in the early solar system

TL;DR

Paleomagnetic measurements of meteorite chondrules reveal a significant magnetic field in the early solar nebula's outer regions, indicating a major disk substructure likely caused by a magnetized disk wind, shedding light on early solar system dynamics.

Contribution

This study provides direct paleomagnetic evidence for a disk substructure in the early solar system, a novel insight into nebular magnetic fields and disk evolution.

Findings

Detected a 101 ± 48 μT magnetic field in the outer solar nebula.

Found a 5 to 150 times higher magnetic field in outer vs. inner solar system.

Suggests substantial mass loss from the disk due to a magnetized wind.

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.