标题： 地震学上分辨不出的红巨星振荡双星的功率密度谱形态 显示英文标题

标题： Power density spectra morphologies of seismically unresolved red-giant asteroseismic binaries

摘要： 振荡双星是由单一光变曲线中检测到的两颗振荡恒星组成的系统。这些系统通过动力学和振荡恒星参数的结合，为恒星模型提供了可靠的限制条件。预测表明，在开普勒长周期数据中可能存在大约200个振荡双星系统，并且其中大多数由两个红团簇星组成。然而，当双星分量以相似且无法区分的频率振荡时，探测这些系统变得具有挑战性。在这项研究中，我们预测了未解析的红团簇振荡双星系统的功率密度谱（PDS）形态，以提供可用于识别观测恒星的例子。我们通过组合具有相似频率范围振荡的红巨星的KASOC光变曲线，创建了5000个人工振荡双星（AAB）系统。为了量化振荡模式的复杂性，我们使用了背景归一化PDS的最大信噪比和香农熵。此外，我们还识别了每个双星分量的径向和四极模式对，并确定了它们对AABs的PDS形态的影响。我们的结果显示，大多数AAB由两个红团簇星组成。与单个分量相比，AAB的PDS通常表现出更高的熵和更低的振荡功率。我们专注于那些具有相似亮度的恒星成分的AAB，并将其分为四种不同的形态：单星状PDS、对齐、部分对齐和错位。大多数从两个分量中都能检测到振荡的AAB显示出复杂的振荡模式。因此，具有低振荡功率和高熵表征的未解析振荡双星为理解具有复杂PDS的观测恒星提供了一种潜在的解释。 显示英文摘要

摘要： Asteroseismic binaries are two oscillating stars detected in a single light curve. These systems provide robust constraints on stellar models from the combination of dynamical and asteroseismical stellar parameters. Predictions suggested that approximately 200 asteroseismic binaries may exist among the Kepler long-cadence data, and the majority of them consist of two red-clump stars. However, detecting these systems is challenging when the binary components exhibit oscillations at similar frequencies that are indistinguishable. In this study, we predict the morphologies of power density spectra (PDS) of seismically unresolved red-giant asteroseismic binaries to provide examples that can be used to identify among observed stars. We created 5,000 artificial asteroseismic binary (AAB) systems by combining the KASOC light curves of red giants with oscillations at similar frequency ranges. To quantify the complexity of the oscillation patterns, we used the maximum signal-to-noise ratio of the background-normalized PDS and Shannon entropy. Additionally, we identified the radial and quadrupole mode pairs for the individual binary components and determined their impact on the PDS morphologies of AABs. Our results reveal that the majority of AABs consist of the two red-clump stars. The PDS of AABs generally exhibits increased entropy and decreased oscillation power compared to individual components. We focused on the AABs whose stellar components have similar brightness and classified them into four distinct morphologies: single star-like PDS, aligned, partially aligned, and misaligned. Most AABs with detectable oscillations from both components show complex oscillation patterns. Therefore, unresolved asteroseismic binaries with low oscillation power and complex oscillation patterns as characterized by high entropy offer a potential explanation to understand the observed stars with complex PDS.