Metallic microstructures in slowly-cooled iron-rich meteorites reflect the
thermal and magnetic histories of their parent planetesimals. Of particular
interest is the cloudy zone, a nanoscale intergrowth of Ni-rich islands within
a Ni-poor matrix that forms below 350{\deg}C by spinodal decomposition. The
sizes of the islands have long been recognized as reflecting the
low-temperature cooling rates of meteorite parent bodies. However, a model
capable of providing quantitative cooling rate estimates from island sizes has
been lacking. Moreover, these islands are also capable of preserving a record
of the ambient magnetic field as they grew, but some of the key physical
parameters required for recovering reliable paleointensity estimates from
magnetic measurements of these islands have been poorly constrained. To address
both of these issues, we present a numerical model of the structural and
compositional evolution of the cloudy zone as a function of cooling rate and
local composition. Our model produces island sizes that are consistent with
present-day measured sizes. This model enables a substantial improvement in the
calibration of paleointensity estimates and associated uncertainties. In
particular, we can now accurately quantify the statistical uncertainty
associated with the finite number of islands and the uncertainty on their size
at the time of the record. We use this new understanding to revisit
paleointensities from previous pioneering paleomagnetic studies of cloudy
zones. We show that these could have been overestimated but nevertheless still
require substantial magnetic fields to have been present on their parent
bodies. Our model also allows us to estimate absolute cooling rates for
meteorites that cooled slower than 10000{\deg}C My-1. We demonstrate how these
cooling rate estimates can uniquely constrain the low-temperature thermal
history of meteorite parent bodies.Comment: Manuscript resubmitted after revision