2019ApJ...887..253C

We computed a grid of theoretical models to fit the δ Scuti frequencies of CoRoT 100866999 detected earlier from the CoRoT time serials. The pulsating primary star is determined to be a main-sequence star with a rotation period of 4.1_–0.5^+0.6 days, rotating slower than the orbital motion. The fundamental parameters of the primary star are determined to be M=1.71_–0.04^+0.13M_☉, Z=0.012_–0.000^+0.004, f_ov=0.02_–0.02^+0.00, T_eff=8024_–297⁺²⁴⁹ K, L=11.898_–1.847^+2.156L_☉, logg=4.166_–0.002^+0.013, R=1.787_–0.016^+0.040R_☉, and X_c=0.488_–0.020^+0.011, matching those obtained from the eclipsing light-curve analysis. Based on the model fittings, p₁ and p₅ are suggested to be two dipole modes, and p₃, p₄, p₆, and p₇ are suggested to be four quadrupole modes. In particular, p₄ and p₇ are identified as two components of one quintuplet. Based on the best-fitting model, we find that p₁ is a g mode and the other nonradial modes have pronounced mixed characters, which give strong constraints on the convective core. Finally, the relative size of the convective core of CoRoT 100866999 is determined to R_conv/R=0.0931_–0.0013^+0.0003.