论文标题
SZ Lyn使用多频段高时间分辨率光度法从地面和空间中
Asteroseismology of sz lyn using multi-band high time resolution photometry from ground and space
论文作者
论文摘要
我们报告了SZ Lyncis的高时间分辨率地面和基于空间的光度观测的分析，SZ Lyncis是二元星的分析，其成分之一是高振幅$δ$ scuti。 UBVR光度观测是从阿布山红外天文台和费尔伯恩天文台获得的。 WASP项目的档案观察结果也包括在内。此外，苔丝项目的连续高质量光曲线被广泛用于分析。苔丝的良好分辨光曲线揭示了23个具有四种独立模式的频率，13个主脉冲频率的谐波为8.296943 $ \ pm $ 0.000002 D $^{ - 1} $及其组合。频率8.296 d $^{ - 1} $通过振幅比方法标识为基本径向模式，并使用估计的脉动常数。频率14.535 d $^{ - 1} $，32.620 d $^{ - 1} $和4.584 d $^{ - 1} $是针对SZ lyn的新发现的。在这三个，14.535 d $^{ - 1} $和32.620 d $^{ - 1} $中，被识别为非降低下阶p-modes和4.584 d $^{ - 1} $，可能是$δ$ scuti scuti s scuti scuti scuti s g-mode的指示。由于频率确定和模式识别，通过使用观察到的频率的恒星脉动模型的优化对SZ LYN的物理参数进行了修订。理论模型对应于7500 k $ \ le $ t $ _ {\ rm eff} $ $ $ \ le $ 7800 k，log（g）= 3.81 $ \ pm $ 0.06。使用进化序列估计，SZ Lyn的质量接近1.7--2.0 m $ _ \ odot $。周期密度关系估计平均密度$ρ$ 0.1054 $ \ pm $ 0.0016 g cm $^{ - 3} $
We report the analysis of high temporal resolution ground and space based photometric observations of SZ Lyncis, a binary star one of whose components is a high amplitude $δ$ Scuti. UBVR photometric observations were obtained from Mt. Abu Infrared Observatory and Fairborn Observatory; archival observations from the WASP project were also included. Furthermore, the continuous, high quality light curve from the TESS project was extensively used for the analysis. The well resolved light curve from TESS reveals the presence of 23 frequencies with four independent modes, 13 harmonics of the main pulsation frequency of 8.296943$\pm$0.000002 d$^{-1}$ and their combinations. The frequency 8.296 d$^{-1}$ is identified as the fundamental radial mode by amplitude ratio method and using the estimated pulsation constant. The frequencies 14.535 d$^{-1}$, 32.620 d$^{-1}$ and 4.584 d$^{-1}$ are newly discovered for SZ Lyn. Out of these three, 14.535 d$^{-1}$ and 32.620 d$^{-1}$ are identified as non-radial lower order p-modes and 4.584 d$^{-1}$ could be an indication of a g-mode in a $δ$ Scuti star. As a result of frequency determination and mode identification, the physical parameters of SZ Lyn were revised by optimizations of stellar pulsation models with the observed frequencies. The theoretical models correspond to 7500 K $\le $T$_{\rm eff}$ $\le$ 7800 K, log(g)=3.81$\pm$0.06. The mass of SZ Lyn was estimated to be close to 1.7--2.0 M$_\odot$ using evolutionary sequences. The period-density relation estimates a mean density $ρ$ of 0.1054$\pm$0.0016 g cm$^{-3}$
