  The accretion-powered X-ray pulsar 4U 1626--67 is one of the few highly
magnetized pulsars that accretes through Roche-lobe overflow from a low-mass
companion. The characteristics of its broadband spectrum are similar to those
of X-ray pulsars hosted in a high-mass X-ray binary systems, with a broad
resonant cyclotron scattering feature (CRSF) at $\sim$37 keV. In this work, we
examine the pulse-resolved and the pulse-averaged broadband spectrum using data
from NuSTAR and Swift. We use the Becker & Wolff model of bulk+thermal
Comptonization to infer key physical parameters of the accretion column flow
and a broadband model for the disk reflected spectrum. In the softer X-ray
band, we need to add a soft black-body component with $kT_{\rm bb}$ $\sim$0.5
keV, whose characteristics indicate a possible origin from the neutron star
surface. Residuals suggest that the shape of the cyclotron line could be more
satisfactorily fitted using a narrow core and broader wings and, at higher
energies, a second harmonic could be present at $\sim$61 keV.
