  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.
