  The H II region N88a in the Small Magellanic Cloud (SMC) is a spherical
region of $1.5~\mathrm{pc}$ diameter, with high concentration of gas and dust,
and at least four massive stars within it. Previous studies suggest that the
four known sources may be insufficient to ionize the region and explain the
nebular emission. In this contribution we analyze the ionizing photon
production of the four known sources within the H II region. We compared the
available photometry in the literature with the spectral energy distribution
calculated for the ``Potsdam Wolf-Rayet'' (PoWR) models of massive stars for a
wide range of dust extinction coefficient (Av). In particular, we selected
models of OB-type atmospheres with SMC metallicity and compared the ionizing
photon flux prediction with previous estimates based on the nebular emission of
the H {\sc ii} region. We found that the Av values that best reproduce the
photometry of each source vary from 0.82 to 3.84, increasing toward the dust
band that runs through the nebula. In addition, all four sources are compatible
with O-type stars with $\mathrm{T_{eff}} > 40 ~\mathrm{kK}$ and intrinsic
ratios $\mathrm{F(LyC)/F(UV)}>1$. Lastly, the total ionizing photon rate
predicted by the hottest models is $\mathrm{log(Q_H)} > 49.6 ~\mathrm{ph\
s}^{-1}$, which suggests that the stars could maintain the ionization state of
the nebula.
