New Constraints on the Origin of Surface Brightness Profile Breaks of
  Disk Galaxies from MaNGA
  In an effort to probe the origin of surface brightness profile (SBP) breaks
widely observed in nearby disk galaxies, we carry out a comparative study of
stellar population profiles of 635 disk galaxies selected from the MaNGA
spectroscopic survey. We classify our galaxies into single exponential (TI),
down-bending (TII) and up-bending (TIII) SBP types, and derive their spin
parameters and radial profiles of age/metallicity-sensitive spectral features.
Most TII (TIII) galaxies have down-bending (up-bending) star formation rate
(SFR) radial profiles, implying that abrupt radial changes of SFR intensities
contribute to the formation of both TII and TIII breaks. Nevertheless, a
comparison between our galaxies and simulations suggests that stellar migration
plays a significant role in weakening down-bending $\Sigma_{\star}$ profile
breaks. While there is a correlation between the break strengths of SBPs and
age/metallicity-sensitive spectral features for TII galaxies, no such
correlation is found for TIII galaxies, indicating that stellar migration may
not play a major role in shaping TIII breaks, as is evidenced by a good
correspondence between break strengths of $\Sigma_{\star}$ and surface
brightness profiles of TIII galaxies. We do not find evidence for galaxy spin
being a relevant parameter for forming different SBP types, nor do we find
significant differences between the asymmetries of galaxies with different SBP
types, suggesting that environmental disturbances or satellite accretion in the
recent past do not significantly influence the break formation. By dividing our
sample into early and late morphological types, we find that galaxies with
different SBP types follow nearly the same tight stellar mass-$R_{25}$
relation, which makes the hypothesis that stellar migration alone can transform
SBP types from TII to TI and then to TIII highly unlikely.
