  Magnetic fields likely play an important role in the formation of young
protostars. Multiscale and multiwavelength dust polarization observations can
reveal the inferred magnetic field from scales of the cloud to core to
protostar. We present continuum polarization observations of the young
protostellar triple system IRAS 16293-2422 at 89 $\mu$m using HAWC+ on SOFIA.
The inferred magnetic field is very uniform with an average field angle of
89$^\circ\pm$23$^\circ$ (E of N), which is different from the $\sim$170$^\circ$
field morphology seen at 850 $\mu$m at larger scales (> 2000 au) with JCMT
POL-2 and at 1.3 mm on smaller scales (< 300 au) with ALMA. The HAWC+ magnetic
field direction is aligned with the known E-W outflow. This alignment
difference suggests that the shorter wavelength HAWC+ data is tracing the
magnetic field associated with warmer dust likely from the outflow cavity,
whereas the longer wavelength data are tracing the bulk magnetic field from
cooler dust. Also, we show in this source the dust emission peak is strongly
affected by the observing wavelength. The dust continuum peaks closer to source
B (northern source) at shorter wavelengths and progressively moves toward the
southern A source with increasing wavelength (from 22 $\mu$m to 850 $\mu$m).
