论文标题
KIC 10975348：双模式或三模式高振幅$δ$ scuti star？
KIC 10975348: A double-mode or triple-mode high-amplitude $δ$ Scuti star?
论文作者
论文摘要
在本文中，我们使用从$ Kepler $ Mission传递的光度数据分析了KIC 10975348的光变化。与大多数研究良好的$δ$ scuti星星相比，该恒星异常微弱（$ k_ {p} $ = 18.6 mag）。短节奏数据的傅立叶分析（即Q14，Q15和Q16，跨度为220天）表明，这些变化以最强模式为主导，频率f0 = 10.231899 $ \ rm {d^{ - 1}} $，与从$ Rats-kepler $ rats-kepler $ $ rats-bekepler compatie兼容。新检测到的其他两个具有F1（= 13.4988 $ \ rm {d^{ - 1}} $）和F2（= 19.0002 $ \ rm {d^{ - 1}} $）的独立模式，并具有比F0小的数量级。我们注意到，该恒星首次被确定为高振幅$δ$ sct（HADS）恒星，幅度约为0.7 mag，而f0/f1 = 0.758的较低比率表明它可能是金属富变的恒星。频率F2可能是第三个泛音模式，这表明该目标可能是新的径向三模式恒星。我们使用1018个新确定的最大光的新确定时间进行$ O -c $分析，并得出一个埃弗米斯公式：$ t_ {max} $ = 2456170.241912（0）+0.097734（1）$ \ times $ $ $ $ e $。 $ o -o -c $图显示，KIC 10975348的脉动期似乎没有明显的变化，这与大多数HADS恒星相反。这可能的原因可能是由于当前的观测时间短。为了验证其可能的时期变化，需要从未来较长时间跨度的空间进行定期观察。
In this paper, we analyze the light variations of KIC 10975348 using photometric data delivered from $Kepler$ mission. This star is exceptionally faint ($K_{p}$ = 18.6 mag), compared to most well-studied $δ$ Scuti stars. The Fourier analysis of the short cadence data (i.e. Q14, Q15 and Q16, spanning 220 days) reveals the variations are dominated by the strongest mode with frequency F0 = 10.231899 $\rm{d^{-1}}$, which is compatible with that obtained from $RATS-Kepler$. The other two independent modes with F1 (= 13.4988 $\rm{d^{-1}}$) and F2 (= 19.0002 $\rm{d^{-1}}$) are newly detected and have amplitudes two orders of magnitude smaller than F0. We note that, for the first time, this star is identified to be a high-amplitude $δ$ Sct (HADS) star with amplitude of about 0.7 mag, and the lower ratio of F0/F1 = 0.758 suggests it might be a metal-rich variable star. The frequency F2 may be a third overtone mode, suggesting this target might be a new radial triple-mode HADS star. We perform $O - C$ analysis using 1018 newly determined times of maximum light and derive an ephemeris formula: $T_{max}$ = 2456170.241912(0)+0.097734(1) $\times$ $E$. The $O - C$ diagram shows that the pulsation period of KIC 10975348 seems to show no obvious change, which is in contrast to that of the majority of HADS stars. The possible cause of that may be due to the current short time span of observations. To verify its possible period variations, regular observation from space with a longer time span in future is needed.
