论文标题
KIC 1573174的频率分析：散发出关于HADS恒星性质的灯光
Frequency analysis of KIC 1573174 : shedding light on the nature of HADS stars
论文作者
论文摘要
我们建议KIC 1573174是四型$δ$Δ$ scuti星，在HADS（高振幅Delta Scuti Star）组和平均低振幅脉动器之间具有脉动振幅。该恒星中检测到的径向模式为开发限制的黑星技术提供了独特的机会。从开普勒任务中对光曲线进行了详细的频率分析。光曲线的变化以最强模式为主导，频率为f0 = 7.3975 $ \ rm {d^{ - 1}} $，如傅里叶分析长节奏数据（Q1-Q17，跨越1460天）所示，表明目标是$δ$ sacti sacti star。其他三个独立模式，具有F1 = 9.4397 D $^{ - 1} $，F2 = 12.1225 D $^{ - 1} $和F3 = 14.3577 D $^{ - 1} $的比率为$ P_ {1} $ / $ P_ {0} $ p_ {0} $ p_ {0} $ p_ {$ p_ {$ p_} $ / $ p_ {3} $ / $ p_ {0} $估计为0.783、0.610和0.515，这表明KIC 1573174是四倍模式$δ$Δ$ scuti star。通过研究相调制的研究，已使用另一种方法来确定$ O-C $。获得周期$（1/p）〜DP/DT $的变化，导致$ -1.14 \ times 10^{ - 6}〜\ text {yr}^{ - 1} $和$ -4.48 \ times 10^{ - 6}〜\ text { - 6}〜\ text {yr} {yr}^{yr}^{ - 1} $ for f0和f0和f0和f0和f0和f0和f0 and f0和f0 and f0和f0 and f0 and f0 and f0 and f0 and f0 and f0 and f0和f1基于频率参数（即F0，F1，F2和F3），通过采用恒星进化代码MESA进行了一系列理论模型。观察到的$ f_ {1}/f_ {2} $的比率大于模型的比率，这可能是由恒星旋转引起的。我们建议将来高分辨率的光谱观测是进一步限制模型的高度期望。
We propose that KIC 1573174 is a quadruple-mode $δ$ Scuti star with pulsation amplitudes between those of the HADS (high-amplitude Delta Scuti star) group and average low-amplitude pulsators. The radial modes detected in this star provide a unique opportunity to exploit asteroseismic techniques up to their limits. Detailed frequency analysis is given for the light curve from the Kepler mission. The variation of the light curve is dominated by the strongest mode with a frequency of F0 = 7.3975 $\rm{d^{-1}}$, as shown by Fourier analysis of long cadence data (Q1-Q17, spanning 1460 days), indicating that the target is a $δ$ Scuti star. The other three independent modes with F1 = 9.4397 d$^{-1}$, F2 = 12.1225 d$^{-1}$ and F3 = 14.3577 d$^{-1}$, have ratios of $P_{1}$ / $P_{0}$, $P_{2}$ / $P_{0}$ and $P_{3}$ / $P_{0}$ estimated as 0.783, 0.610 and 0.515, which indicate that KIC 1573174 is a quadruple-mode $δ$ Scuti star. A different approach has been used to determine the $O-C$ through the study of phase modulation. The change of period $(1/P)~dP/dt$ is obtained resulting in $-1.14 \times 10^{-6}~\text{yr}^{-1}$ and $-4.48 \times 10^{-6}~\text{yr}^{-1}$ for F0 and F1 respectively. Based on frequency parameters (i.e., F0, F1, F2, and F3), a series of theoretical models were conducted by employing the stellar evolution code MESA. The ratio of observed $f_{1}/f_{2}$ is larger than that of the model, which may be caused by the rotation of the star. We suggest high-resolution spectral observation is highly desired in the future to further constrain models.
