  Asteroseismology is an unique and powerful tool to detect the internal
structure of stars. CBS 114 is the sixth known pulsating DBV star. It was
observed by Handler, Metcalfe, \& Wood at South African Astronomical
Observatory over 3 weeks in 2001. Then, it was observed by Metcalfe et al. at
Bohyunsan Optical Astronomy Observatory and McDonald Observatory respectively
for 7 nights in 2004. Totally 2 triplets, 4 doublets, and 5 singlets were
identified. The frequency splitting values are very different, from 5.2 $\mu$Hz
to 11.9 $\mu$Hz, which may reflect differential rotations. We evolve grids of
white dwarf models by \texttt{MESA}. Cores, added with He/C envelopes, of those
white dwarf models are inserted into \texttt{WDEC} to evolve grids of DBV star
models. With those DBV star models, we calculate eigenperiods. Those calculated
periods are used to fit observed periods. A best-fitting model is selected. The
parameters are $T_{eff}$ = 25000 K, $M_{*}$ = 0.740 $M_{\odot}$, and
log($M_{He}/M_{*}$) = -4.5. With the massive stellar mass, the effective
temperature is close to previous spectroscopic result. In addition, kinetic
energy distributions are calculated for the best-fitting model. We find that
the observed modes with large frequency splitting values are fitted by the
calculated modes with much kinetic energy distributed in C/O core. After
preliminary analysis, we suggest that the C/O core may rotate at least 2 times
faster than the helium layer for CBS 114.
