Title: DUETS: Setting expectations for asteroseismic binaries and binary products with synthetic populations Show Chinese title

Title: DUETS：利用合成种群为振荡双星和双星产物设定期望

Abstract: Asteroseismology gives us the opportunity to better characterize binaries and their products, and shed light on their role in Galactic populations. We estimate occurrence rates, mass distributions, and evolutionary states of asteroseismic binaries, exhibiting solar-like oscillations from both components, and of products of binary interactions with detectable solar-like oscillations. Additionally, we explore the effects of mass accretion or loss on apparent age-metallicity relations. Using the TRILEGAL code, we simulate Kepler's field of view adopting the Eggleton and Moe & Di Stefano distributions of initial binary parameters, and run an additional simulation with non-interacting binaries for comparison. We find that asteroseismic binaries require an initial mass ratio close to one, and even small mass transfer events can prevent the detection of oscillations from both components. The fraction of asteroseismic binaries for red giant stars with detectable oscillations ranges from 0.5\% for non-interacting binaries to a minimum of 0.06% when taking interactions into account. Moreover, asteroseismic binaries composed of two red clump stars are not expected at separations $\leq 500~\text{R}_\odot$ due to the interplay of stellar evolution and binary interactions. Finally, we estimate that at least ~1% of the Kepler red giants with detectable oscillations have undergone significant mass accretion or loss, potentially affecting Galactic age-metallicity relations, although there is a strong dependence on the assumed initial binary parameters. Comparing predicted and observed asteroseismic binaries, as well as over- and under-massive stars, offers a way to constrain key binary evolution assumptions, and to reduce uncertainties in mass-transfer modeling. Show Chinese abstract

Abstract: 星震学为我们提供了更好地表征双星及其产物的机会，并揭示它们在银河系种群中的作用。 我们估计了具有太阳型振荡的星震双星的发生率、质量分布和演化状态，以及具有可探测太阳型振荡的双星相互作用产物。 此外，我们还研究了质量吸积或损失对表面年龄-金属丰度关系的影响。 使用TRILEGAL代码，我们采用Eggleton和Moe & Di Stefano提出的初始双星参数分布模拟开普勒视场，并运行了另一组非相互作用双星的模拟以供比较。 我们发现，星震双星需要一个接近1的初始质量比，即使是最小的质量转移事件也可能阻止从两个成分中检测到振荡。 对于具有可探测振荡的红巨星，星震双星的比例从非相互作用双星的0.5\%下降到考虑相互作用时的最低值0.06%。 此外，由两颗红团星组成的星震双星在分离距离为$\leq 500~\text{R}_\odot$时不会形成，这是由于恒星演化与双星相互作用之间的相互作用。 最后，我们估计至少有~1%的开普勒红巨星经历了显著的质量吸积或损失，这可能影响银河系的年龄-金属丰度关系，尽管这取决于假设的初始双星参数。 通过比较预测和观测到的星震双星以及超质量和亚质量恒星，可以约束关键的双星演化假设，并减少质量转移建模中的不确定性。