Asteroseismology of the Pre-main-sequence δ Scuti Pulsator IP Persei

A grid of theoretical models are computed to fit the nine 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 equally as well. In view of other available spectroscopic and photometric measurements, our best-fitting stellar parameters for IP Per are u(e) = 91(-3)(+5) km s(-1), Z = 0.009(-0.001)(+0.004), M = 1.64(-0.04)(+0.10) M-circle dot,M- T-eff = 7766(-173)(+348) K, log L/L-circle dot = 1.125(-0.046)(+0.094), log g = 4.041(-0.003)(+0.008) dex, R = 2.022(-0.018)(+0.042) R-circle dot, T-0 = 8711(-35)(+68) s, and age = 7.39(-0.46)(+0.76) Myr. Meanwhile, IP Per is found to be a pre-main-sequence star where the CN cycle has not yet reached the equilibrium state. At present, 14% 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.