  Far-infrared polarized emission by means of magnetically aligned dust grains
is an excellent tracer of the magnetic fields (B-fields) in the cold phase of
the galactic outflows in starburst galaxies. We present a comprehensive study
of the B-fields in three nearby ($3.5$-$17.2$ Mpc) starbursts (M82, NGC 253,
and NGC 2146) at $5$ pc-$1.5$ kpc resolutions using publicly available
$53$-$890$ $\mu$m imaging polarimetric observations with SOFIA/HAWC+,
JCMT/POL-2, and ALMA. We find that the polarized spectral energy distributions
(SEDs) of the full galaxies are dominated by the polarized SEDs of the outflows
with dust temperatures of $T_{\rm{d,outflow}}^{\rm{PI}}\sim45$ K and emissive
index of $\beta_{\rm{outflow}}^{\rm{PI}}\sim2.3$. The disks are characterized
by low $T_{\rm{d,disk}}^{\rm{PI}}=[24,31]$ K and
$\beta_{\rm{disk}}^{\rm{PI}}\sim1$. We show that disk- and outflow-dominated
galaxies can be better distinguished by using polarized SEDs instead of total
SEDs. We compute the $53$-$850$ $\mu$m polarization spectrum of the disk and
outflow and find that dust models of the diffuse ISM can reproduce the fairly
constant polarization spectrum of the disk, $\langle P_{\rm{disk}}
\rangle=1.2\pm0.5$%. The dust models of heterogenous clouds and two temperature
components are required to explain the polarization spectrum of the outflow
($2$-$4$% at $53$ $\mu$m, $\sim1$% at $850$ $\mu$m, and a minimum within
$89$-$154$ $\mu$m). We conclude that the polarized dust grains in the outflow
arise from a dust population with higher dust temperature and emissivities than
those from the total flux. The B-fields of the outflows have maximum extensions
within $89$-$214$ $\mu$m reaching heights of $\sim4$ kpc, and flatter polarized
fluxes than total fluxes. The extension of the B-field permeating the
circumgalactic medium increases with increasing the star formation rate.
