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 _ { e } = 91 ^ { +5 } _ { -3 } km s ^ { -1 } , Z = 0.009 ^ { +0.004 } _ { -0.001 } , M = 1.64 ^ { +0.10 } _ { -0.04 } M _ { \odot } , T _ { 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 .