  We analyzed the deconvolved surface brightness profiles of 247 massive and
angularly large disk galaxies at $1\leq z\leq 3$ to study high-redshift disk
breaks, using F356W-band images from the Cosmic Evolution Early Release Science
survey (CEERS). We found that 12.6% of these galaxies exhibit type I
(exponential) profiles, 56.7% exhibit type II (down-bending) profiles, and
34.8% exhibit type III (up-bending) profiles. Moreover, we showed that galaxies
that are more massive, centrally concentrated, or redder, tend to show fewer
type II and more type III breaks. These fractions and the detected dependencies
on galaxy properties are in good agreement with those observed in the Local
Universe. In particular, the ratio of the type II disk break radius to the bar
radius in barred galaxies typically peaks at a value of 2.25, perhaps due to
bar-induced radial migration. However, the timescale for secular evolution may
be too lengthy to explain the observed breaks at such high redshifts. Instead,
violent disk instabilities may be responsible, where spiral arms and clumps
torque fling out the material, leading to the formation of outer exponential
disks. Our results provide further evidence for the assertion that the Hubble
Sequence was already in place during these early periods.
