  The Galactic diffuse X-ray emission (GDXE) is believed to arise from
unresolved populations of numerous low-luminosity X-ray binary systems that
trace stellar mass distribution of the Milky Way. Many dedicated studies
carried out over the last decade suggest that a dominant contributor to GDXE is
a population of accreting white dwarfs (WDs). The question arises about
relative contribution of different subclasses of accreting WD population,
namely non-magnetic WD binaries, magnetic intermediate polars (IPs) and polars,
in different regions of the Galaxy: the Galactic center, bulge, and ridge.
Recent low-energy (E$<10$ keV) studies indicate that non-magnetic WD binaries,
in particular quiescent dwarf novae, provide a major contribution to the
diffuse hard X-ray emission of the Galactic bulge. From the other side,
previous high energy (E$>10$ keV) X-ray measurements of the bulge and ridge
imply a dominant population of magnetic CVs, in particular intermediate polars.
In this work we use side aperture of the NuSTAR to probe the diffuse continuum
of the inner $\sim1-3^{\circ}$ of the Galactic bulge, which allows us to
constrain possible mixture of soft and hard populations components of the
spectrum. We found that GDXE spectrum is well-described by a single-temperature
thermal plasma with $kT \approx 8$ keV, which supports that the bulge is
dominated by quiescent dwarf novae with no evidence of a significant
intermediate polar population in the hard X-ray band. We also compare this
result with previous NuSTAR measurements of the inner 10 pc and inner 100 pc of
the Galactic center.
