发表机构
University of Nigeria, Nsukka; Çanakkale Onsekiz Mart University; Villanova University; Royal Observatory of Belgium; Nicolaus Copernicus Astronomical Centre, Polish Academy of Sciences（尼日利亚恩苏卡大学; 恰纳卡莱十月马特大学; 维拉诺瓦大学; 比利时皇家天文台; 波兰科学院尼古拉·哥白尼天文学中心）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过光谱和测光分析十三个含$\beta$ Cep脉动星的食双星，测定其轨道与恒星参数，并探讨自转、圆化及同步化特性，为理解大质量脉动恒星演化提供关键约束。
AI 中文摘要
食双星为恒星性质和演化提供了精确约束，使得那些包含$\beta$ Cep脉动星的双星系统对于表征大质量脉动恒星尤为珍贵。本文对十三个具有大质量主成分的食双星进行了光谱和测光分析，以推导其轨道和恒星参数，并推断它们可能的演化状态。这些系统使用SALT HRS、HERMES、CHIRON以及斯卡尔纳特普莱索天文台（SPO）的一台摄谱仪进行了光谱观测，并使用TESS进行了测光观测。确定了视向速度和大气参数，对双星系统进行了建模，并使用适当的建模工具推导了其绝对参数。还研究了系统的自转特性、轨道圆化和同步化，并讨论了样本的一般性质。样本包含一个慢自转体、两个已圆化且同步化的快自转系统，以及五个圆轨道和五个偏心轨道且具有非同步快自转的系统。这些系统主要是具有暗伴星的SB1或SB2型，导致动力学质量估计精度为$5$--$12\\%$，半径估计精度为$1.5$--$3.9\\%$。次成分似乎跨越了从低质量到中等质量系统的广泛质量谱。系统的偏心率与投影自转速度（$v \sin i$）表现出一定趋势，尽管它们之间没有普遍的相关性。此外，即使对于已圆化的短周期密近双星系统，也可能存在没有共转或同步化的圆化现象。
英文摘要
Eclipsing binaries provide precise constraints on stellar properties and evolution, making those hosting $β$ Cep pulsators particularly valuable for characterising massive pulsating stars. In this paper, thirteen eclipsing binaries with massive primary components are spectroscopically and photometrically analysed to derive the orbital and stellar parameters, and infer their possible evolutionary status. The systems were spectroscopically observed using SALT HRS, HERMES, CHIRON and a spectrograph at Skalnate Pleso Observatory (SPO), and photometrically observed using TESS. Radial velocities and atmospheric parameters are determined, binary systems are modelled, and their absolute parameters are derived using appropriate modelling tools. The rotational properties, circularisation, and synchronisation of the systems are also investigated, and the general properties of the sample are discussed. The sample shows one slow rotator, two circularised and synchronised fast rotating systems, as well as five circular and five eccentric systems with asynchronous fast rotation. The systems are predominantly SB1 or SB2 with faint companions, resulting in dynamical mass estimates at $5$ -- $12\%$ precision and radius estimates at $1.5$ -- $3.9\%$ precision. The secondary components appear to cut across a wide mass spectrum ranging from low-mass to intermediate mass systems. The eccentricity of the systems shows certain trends with the projected rotational velocity ($v \sin i$) although there is no universal correlation between them. Also, there could be circularisation without co-rotation or synchronisation even for circularised short-period close binary systems.
Comments20 pages and 12 figures. Accepted for publication in Astronomy & Astrophysics
