  We present a new asteroseismic analysis of KIC~6048106, a \textit{Kepler}
Algol-type eclipsing binary star in a circularized orbit with
$P_\rm{orb}$=1.559361$\pm$0.000036~d. Based on a physical model for the binary
and its corresponding set of fundamental parameters, ($T_\rm{eff}=7033\pm187~K,
~M_\rm{1}=1.55\pm0.11M_{\odot}$ and
$T_\rm{eff}=4522\pm103~K,~M_\rm{2}=0.33\pm0.07M_{\odot}$, respectively for the
primary and the secondary component), we obtained the residual light curve
after removal of the full binary model, including a 290-day activity cycle for
the secondary component (Samadi Gh. et al.\,2018). In this work, we used the
method of Fourier analysis of the residual light curve in combination with
least squares optimization for the frequency analysis. We detected seven
dominant, independent gravity ($g$) modes as well as 34 low-amplitude acoustic
($p$) modes. The $g$ modes in the range $1.96-2.85$ d$^{-1}$ have a mean
spacing of $\Delta\Pi_\rm{mean}=1517.92\pm131.54$~s. Though of much lower
amplitude, additional significant frequencies were detected in the intervals
$7.49-15.2$ d$^{-1}$ and $19-22.5$ d$^{-1}$ (i.e. in the $p$ mode region), with
corresponding dominant modes $\nu_\rm{max_\rm{1}}=11.745\pm0.001$ d$^{-1}$ and
$\nu_\rm{max_\rm{2}}=20.960\pm0.002$ d$^{-1}$. From its position in the H-R
diagram, we conclude that the primary component is the source of the detected
hybrid pulsations. Consequently, the pulsation constants, Q, of the high
frequencies cover the range $0.028-0.064$~d. Furthermore, $\nu_\rm{43} $
(19.037$\pm$0.002 d$^{-1}$) might correspond to the fundamental radial mode (Q
= 0.033$\pm$0.007 d). The other frequencies in the range $19-22.5$ d$^{-1}$
could be radial or non-radial overtone modes. Moreover, the low-amplitude $p$
modes show an equidistant splitting by $f_\rm{orb}$, which we interpret as
tidal splitting following theoretical predictions.
