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The frequency ratios $r_{01}$ and $r_{10}$ of KIC 11081729 decrease firstlyand then increase with the increase in frequency. For different spectroscopicconstraints, all models with overshooting parameter $\delta_{\mathrm{ov}}$ lessthan 1.7 can not reproduce the distributions of the ratios. However, thedistributions of the ratios can be directly reproduced by models with$\delta_{\mathrm{ov}}$ in the range of about $1.7-1.8$. The estimations of massand age of the star can be affected by spectroscopic results, but thedetermination of the $\delta_{\mathrm{ov}}$ is not dependent on thespectroscopic results. A large overshooting of convective core may exist in KIC11081729. The characteristics of $r_{01}$ and $r_{10}$ of KIC 11081729 mayresult from the effects of the large overshooting of convective core. Thedistributions of $r_{01}$ and $r_{10}$ of different stars with a convectivecore can be reproduced by the function $B(\nu_{n,1})$. If the value of thecritical frequency $\nu_{0}$ is larger than the value of frequency of maximumoscillation power $\nu_{max}$, a star may have a small convective core and$\delta_{\rm ov}$. But if the value of $\nu_{0}$ is less than that of$\nu_{max}$, the star may have a large convective core and$\delta_{\mathrm{ov}}$. The function aids in determining the presence ofconvective core and the size of the convective core including overshootingregion from observed frequencies. The determination is not dependent on thecalculation of stellar models.

A Large Convective-Core Overshoot in \textit{Kepler} Target KIC 11081729