  With the observations from \textit{Rossi X-ray Timing Explorer}, we search
and study the X-ray bursts of accreting millisecond X-ray pulsar
SAX~J1748.9-2021 during its 2010 outburst. We find 13 X-ray bursts, including
12 standard type-\uppercase\expandafter{\romannumeral1} X-ray bursts and an
irregular X-ray burst which lacks cooling tail. During the outburst, the
persistent emission occurred at $\sim$(1-5)$\%\rm {\dot{M}_{Edd}}$. We use a
combination model of a blackbody (BB), a powerlaw, and a line component to fit
the persistent emission spectra. Another BB is added into the combination model
to account for the emission of the X-ray bursts due to the thermonuclear
burning on the surface of the neutron star. Finally, we modify the combination
model with a multiplicative factor $f_{\rm a}$, plus a BB to fit the spectra
during the X-ray bursts. It is found that the $f_{\rm a}$ is inversely
correlated with the burst flux in some cases. Our analysis suggests that the
ignition depth of the irregular X-ray burst is obviously smaller than those of
the type-\uppercase\expandafter{\romannumeral1} X-ray bursts. We argue that the
detected type-\uppercase\expandafter{\romannumeral1} X-ray bursts originate
from helium-rich or pure-helium environment, while the irregular X-ray burst
originates from the thermonuclear flash in a shallow ocean.
