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A grid of theoretical models are computed to fit the 9 oscillation modes ofIP Per detected earlier from a multi-site ground-based campaign. Fittingresults show that there are two sets of theoretical models that could reproducethe observed frequencies more or less euqally well. In view of other availablespectroscopic and photometric measurements, our best fitting stellar parametersfor IP Per are $\upsilon_{\rm e} = 91^{+5}_{-3}$ km s$^{-1}$,$Z=0.009^{+0.004}_{-0.001}$, $M = 1.64^{+0.10}_{-0.04}$ $M_{\odot}$, $T_{\rmeff} = 7766^{+348}_{-173}$ 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 hasnot yet reached the equilibrium state. At present fourteen percent of C12 havebeen turned into N14. Based on the best-fitting model, $f_{6}$ is identified asa 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.

Asteroseismology of the pre-main-sequence $\delta$ Scuti pulsator IP Persei