  A grid of theoretical models are computed to fit the 9 oscillation modes of
IP Per detected earlier from a multi-site ground-based campaign. Fitting
results show that there are two sets of theoretical models that could reproduce
the observed frequencies more or less euqally well. In view of other available
spectroscopic and photometric measurements, our best fitting stellar parameters
for IP Per are $\upsilon_{\rm e} = 91^{+5}_{-3}$ km s$^{-1}$,
$Z=0.009^{+0.004}_{-0.001}$, $M = 1.64^{+0.10}_{-0.04}$ $M_{\odot}$, $T_{\rm
eff} = 7766^{+348}_{-173}$ K, $\log L/L_{\odot} = 1.125^{+0.094}_{-0.046}$,
$\log g = 4.041^{+0.008}_{-0.003}$ dex, $R = 2.022^{+0.042}_{-0.018}$
$R_{\odot}$, $\tau_{0} = 8711^{+68}_{-35}$ s, age = $7.39^{+0.76}_{-0.46}$ Myr.
Meanwhile, IP Per is found to be a pre-main sequence star where CN cycle has
not yet reached the equilibrium state. At present fourteen percent of C12 have
been turned into N14. Based on the best-fitting model, $f_{6}$ is identified as
a radial mode, $f_{1}$ and $f_{2}$ as two dipole modes, and $f_{3}$, $f_{4}$,
$f_{5}$, $f_{7}$, $f_{8}$, and $f_{9}$ as six quadrupole modes.

Solar and Stellar Astrophysics