发表机构
Çanakkale Onsekiz Mart University（恰纳卡莱18马尔大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过分析17个oEA系统，结合双星建模、O-C分析和TESS测光，发现质量转移指标与$\delta$ Scuti脉动周期存在弱到中等正相关，表明质量转移可能作为次要因素影响脉动特性。
AI 中文摘要
我们探讨了17个振荡食双星Algol型系统中，正在进行的质量转移与$\delta$ Scuti主星脉动特性之间的潜在关联。为此，我们结合了双星建模、更新的O-C分析以及基于TESS测光数据的频率表征。为确保同质性，各组分的$T_{\rm eff}$均采用一致的SED拟合方法推导。通过双星解和O-C图，我们确定了质量转移指标（Q、dP/dt和dM/dt），并检验了它们与主导脉动周期和振幅的关系。对于全样本，结果显示弱到中等的正趋势，其中logdP/dt与logPpuls之间的关系最强，而涉及dM/dt和脉动振幅的关系较弱且统计上不显著。在排除两个显著异常值R CMa和BW Del后，logPpuls与质量转移指标之间的相关性在统计上变得更加显著，包括在保守和非保守假设下与dP/dt、Q和dM/dt的关系。这些关系可能反映了质量转移对吸积主星结构和轨道构型的间接影响，可能减少潮汐约束并允许脉动周期向更长方向移动。然而，较大的离散性和有限的样本量表明这些关系仍受到较差的约束。我们的结果表明，脉动特性主要由内在恒星参数和已确立的Porb-Ppuls关系主导，而正在进行的质量转移可能作为次要因素起作用。尽管当前样本不允许就质量转移的作用得出确切结论，但本研究为基于更大样本和改进约束的未来研究提供了同质的观测框架。
英文摘要
We explored potential associations between ongoing mass transfer and the pulsation properties of $δ$ Scuti primaries in a sample of 17 oscillating eclipsing Algol systems. For this purpose, we combined binary modelling, updated O-C analyses, and frequency characterization based on TESS photometry. To ensure homogeneity, the $T_{\rm eff}$ of the components were derived using a consistent SED fitting approach. From the binary solutions and O-C diagrams, we determined the mass transfer indicators (Q, dP/dt, and dM/dt) and examined their relations with the dominant pulsation period and amplitude. For the full sample, the results indicate weak to moderate positive trends, with the strongest relation found between logdP/dt and logPpuls, while the relations involving dM/dt and pulsation amplitudes are weaker and statistically insignificant. After excluding the two prominent outliers, R CMa and BW Del, the correlations between logPpuls and the mass transfer indicators become statistically more significant, including relations with dP/dt, Q, and dM/dt under both conservative and non-conservative assumptions. These relationships may reflect the indirect effects of mass transfer on the structure of the accreting primary and on the orbital configuration, potentially reducing tidal constraints and allowing shifts toward longer pulsation periods. However, the large dispersion and limited sample size indicate that these relationships remain poorly constrained. Our results suggest that pulsation properties are primarily governed by intrinsic stellar parameters and the well established Porb-Ppuls relation, while ongoing mass transfer may contribute as a secondary factor. Although the present sample does not allow firm conclusions regarding the role of mass transfer, this study provides a homogeneous observational framework for future investigations based on larger samples and improved constraints.
CommentsAccepted for publication in Publications of the Astronomical Society of Japan (PASJ)
