  We re-estimate the surface magnetic fields of neutron stars (NSs) in Be X-ray
binaries (BeXBs) with different models of torque, improved beyond Klus et al.
(2014). In particular, a new torque model (Dai \& Li 2006) is applied to three
models of magnetosphere radius. Unlike the previous models, the new torque
model does not lead to divergent results for any fastness parameter. The
inferred surface magnetic fields of these NSs for the two compressed
magnetosphere models are much higher than that for the uncompressed
magnetosphere model. The new torque model using the compressed-magnetosphere
radius (Shi, Zhang \& Li 2014) leads to unique solutions near spin equilibrium
in all cases, unlike other models that usually give two branches of solutions.
Although our conclusions are still affected by the simplistic assumptions about
the magnetosphere radius calculations, we show several groups of possible
surface magnetic field values with our new models when the interaction between
the magnetosphere and the infalling accretion plasma is considered. The
estimated surface magnetic fields for NSs BeXBs in the Large Magellanic Cloud,
the Small Magellanic Cloud and the Milk Way are between the quantum critical
field and the maximum "virial" value by the spin equilibrium condition.
