论文标题
在苔丝观察到的Eclipsing二进制文件中检测$δ$ Scuti脉动器
Detection of $δ$ Scuti pulsators in the eclipsing binaries observed by TESS
论文作者
论文摘要
基于1-50个扇区的2分钟的节奏苔丝数据，我们报告了在6431欧元的$Δ$ scuti-Type脉动的系统提取的结果，其轨道周期短于13天，轨道周期短。在这些系统中，总共发现了242个脉动器数量，其中包括143个新发现。我们根据H-R图和主导脉动周期之间的关系$ P _ {\ rm dom} $，轨道周期$ p _ {\ rm orb} $与有效温度$ t _ {\ rm eff} $检查了它们的脉动属性。结果，216个目标可能是$δ$ scuti恒星（123颗），11个可能是$γ$ doradus-doradus- $δ$Δ$ scuti杂交恒星（8个新），5 $β$ cephei stars（4 new），4 $ $Δ$Δ$δ$Δ$Δ$Δ$ scuti-cuti-cuti-cuti-γ$ doradus hybrid stars（3 new），可能是新星，3个新星（3新），3个新星（3新）（3新）还有一个新的未分类之星。至于6个新的$δ$ scuti脉动脉动器，用$ p _ {\ rm orb} $ <$ <$ 0.65天，我们发现其中3个显着超过了$ p _ {\ rm dom} $/$ p _ {\ rm orb orb orb orb ym比将。这可能表明$ p _ {\ rm dom} $和$ p _ {\ rm orb} $对它们不相关。最后，我们从统计学上分析了216 $δ$ scuti恒星的主要脉动周期，以黯然失色。这些恒星集中在225美元左右的Hz左右，高频区域的恒星比例明显高于单恒星，这可能归因于传质过程。
Based on 2-minute cadence TESS data from sectors 1-50, we report the results of the systematic extraction of $δ$ Scuti-type pulsations in the 6431 eclipsing binaries with orbital periods shorter than 13 days. A total number of 242 pulsators were found in those systems, including 143 new discoveries. We examined their pulsation properties based on the H-R diagram and the relationships between the dominant pulsation period $P_{\rm dom}$, orbital period $P_{\rm orb}$, and effective temperature $T_{\rm eff}$. As a consequence, 216 targets are likely $δ$ Scuti stars (123 new), 11 likely $γ$ Doradus-$δ$ Scuti hybrid stars (8 new), 5 likely $β$ Cephei stars (4 new), 4 likely $δ$ Scuti-$γ$ Doradus hybrid stars (3 new), 3 likely Maia stars (3 new), 2 likely pulsating red giants (1 new), and a new unclassified star. As for the 6 new $δ$ Scuti pulsators in eclipsing binaries with $P_{\rm orb}$ $<$ 0.65 days, we found that 3 of them significantly exceed the upper limits of the $P_{\rm dom}$/$P_{\rm orb}$ ratio. This may indicate that $P_{\rm dom}$ and $P_{\rm orb}$ are uncorrelated for them. Finally, we statistically analyzed the dominant pulsation periods of the 216 $δ$ Scuti stars in eclipsing binaries. Those stars concentrate around 225 $μ$Hz and the proportion of stars in the high-frequency region is significantly higher than that of single stars, which could be ascribed to the mass transfer process.
