  Polarization of starlight and thermal dust emission caused by aligned dust
grains is a valuable tool to characterize magnetic fields (B-fields) and
constrain dust properties. However, the physics of grain alignment is not fully
understood. To test the popular paradigm of radiative torque (RAT) theory,
including RAT alignment (RAT-A) and disruption (RAT-D), we use dust
polarization data observed by {\it Planck} and SOFIA/HAWC+ toward two filaments
with contrasting physical conditions: Musca, a quiet filament, and OMC-1, a
highly dynamic filament due to feedback. We analyze various relations of the
observed polarization fraction, $P$, with gas column density, $\NHt$, dust
temperature, $\Td$, and polarization angle dispersion function, $\S$. We found
that $P$ decreases with increasing $\S$ and increasing $\NHt$, as expected from
RAT-A. On the other hand, the $P-\Td$ relation is more complicated; it is a
linear correlation at low $\Td$ but turns into an anti-correlation when $\Td$
reaches a certain high value. Next, we compute the polarization fraction on a
pixel-by-pixel with B-fields in the plane of the sky using the DustPOL code
based on RAT, incorporate the depolarization effect by B-field tangling using
$\S$, and compare the realistic polarization model with observations of Musca
and OMC-1. For Musca with well-ordered B-fields, our numerical model reproduces
the decline of $P$ toward the filament spine (aka. polarization hole), having
high $\NHt$ and low $\Td$, indicating the loss of grain alignment efficiency
due to RAT-A. For OMC-1, with stronger B-field variations and higher $\Td$, our
model can reproduce the observed $P-\Td$ and $P-N(\rm H_{2})$ relations only if
the depolarization effect resulting from B-field tangling and RAT-D effect are
taken into account. Our results provide more robust observational evidence for
the RAT paradigm, particularly the recently discovered RAT-D.
