Detailed TESS-Based Light Curve Modeling and Fundamental Parameter Estimation of 27 W UMa-Type Contact Binaries
LUX, Observatoire de Paris, CNRS, PSL（巴黎天文台，法国国家科学研究中心，巴黎文理研究大学）；Astronomy Department of the Raderon AI Lab.（拉德罗恩人工智能实验室天文学系）；Yazd Branch of the National Organization for Development of Exceptional Talents (SAMPAD)（伊朗特殊天赋人才开发组织亚兹德分校）；Yazd Desert Night Sky Astronomy Institute（亚兹德沙漠夜空天文研究所）
Atila Poro, Ahmad Sarostad, Mohammad Davoudi, Mahsa Marami, Motaharehalsadat Mohtaram, Mohammadparsa Sharififard, Diana Zadkhosh, Aida Rakian, Alireza Shiri Ahm… 展开作者
We performed a comprehensive analysis of 27 short period contact binary systems for which no light curve analysis had previously been reported. Photometric time-series data from the TESS mission were used in this analysis. The observational results were validated using additional TESS sectors, along with complementary photometric observations from the ASAS-SN survey. The photometric light curves of the 27 contact binary systems were analyzed with the BSN application. Model solutions were obtained through iterative fitting followed by MCMC-based refinement to derive reliable system parameters, and starspot configurations were incorporated for seven targets exhibiting O'Connell effect asymmetries. The absolute parameters of the target systems were derived using the empirical parameter relationship between orbital period and semi-major axis. Based on the results of the light curve solutions and the estimated absolute parameters, five of the analyzed systems are identified as A-subtype, while the remaining targets belong to the W-subtype. We analyzed a sample of 484 W UMa contact binaries to identify the physical and orbital parameters that most effectively distinguish A-subtype from W-subtype systems using t-statistics. Three targets exhibited extremely low mass ratios, and their orbital analysis confirmed that they are dynamically stable. The evolutionary states of the systems were examined, showing that lower-mass companions are generally more evolved, while more massive components remain less evolved. The positions of the systems and their stellar components were compared across four diagrams derived from empirical parameter relationship studies, showing good agreement with the linear fits.
Photometric investigation and orbital period analyses of the W UMa binaries FP Lyn, FV CVn and V354 UMa
给出了FP Lyn、FV CVn和V354 UMa的新光变曲线和光度解。发现这三个系统都是W型浅接触双星。此外，很明显，FP Lyn和V354 UMa的光变曲线是不对称的。因此，在主星FP Lyn上增加了一个热点，而在副星V354 UMa上增加了一个暗点。与此同时，我们在FP Lyn的光度解决方案中添加了第三盏灯，以获得最终结果。对于FP Lyn，获得的质量比和填充因子为$q=1.153$和$f=13.4\%$，对于FV CVn，获得的质量比和填充因子为$q=1.075$和$f=4.6\%$，对于V354 UMa，获得的质量比和填充因子为$q=3.623$和$f=10.7\%$。对这三个系统轨道周期的研究表明，它们的轨道周期是变化的。发现FP Lyn和V 354 Uma分别存在着长期增长的组分，其增长率分别为$dp/dt=4.19\times10^{-7}$ d yr $^{-1}$和$dp/dt=7.70\times10^{-7}$ d yr $^{-1}$，这可能是由质量较小的组分向质量较大的组分的守恒质量转移引起的。此外，还发现了FV CVn的一些可变成分，即频率为$dp/dt=-1.13\times10^{-6}$ d yr $^{-1}$，伴随着振幅和周期分别为0.0069天和10.65年的周期振荡。长期下降的最可能的解释是角动量损失。而附加分量的存在是对周期性变化的最合…
On the origin of W UMa type Contact binaries - a new method for computation of initial masses
WUMa型二进制有两个定义特征。它们是（i）两个成分的有效温度非常相似，（ii）次级（目前质量较轻）成分相对于其当前质量而言过于明亮。我们认为后者是一个指示其质量之前的质量转移事件。对于这些恒星，我们定义了一个质量差（$δM$），这个质量差是由光度确定的质量和由拟合双星轨道确定的当前质量之间的差。我们比较了观测值的质量差与恒星模型的质量损失。我们发现观测到的W UMa型双星的初始次级质量范围为1.3-2.6 M $_{\odot}$。我们发现，A-和W-亚型接触双星有不同的范围内的初始次级质量。初始质量高于$1.8 \pm 0.1$ M $_{\odot}$的二元系统成为A-亚型，而初始质量低于此的系统成为W-亚型。只有6%的系统违反了这一行为。我们还使用以下初始质量比的倒数的约束条件获得了原色的初始质量：$0 < 1/q_i < 1$。除了两个系统外，我们发现原色的初始质量范围为0.2-1.5 M $_{\odot}$。最后，在比较我们的模型观察到的系统，我们发现的证据表明，传质过程是不保守的。我们发现，只有34%的质量从次级转移到初级。其余部分从系统中丢失。
Searching for Contact Binaries with LAMOST and TESS
Xinjiang Astronomical Observatory, Chinese Academy of Sciences（中国科学院新疆天文台）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文学与空间科学学院）；Department of Astronomy, Xiamen University（厦门大学天文学系）；College of Physics and Information Engineering, Quanzhou Normal University（泉州师范学院物理与信息工程学院）
BSN-VI: Multiband Light Curve Modeling of Four W UMa-Type Contact Binaries I. Revisiting Energy Transfer Mechanisms and Luminosity Behavior
BSN Project（BSN项目）；Independent researcher（独立研究者）；LUX, Observatoire de Paris, CNRS, PSL（巴黎天文台，法国国家科学研究中心，巴黎文理研究大学）；Department of Astronomy, Raderon AI Lab（天文学系，拉德伦人工智能实验室）；Instituto de Astronomía, UNAM（墨西哥国立自治大学天文学研究所）；European Southern Observatory（欧洲南方天文台）；Department of Astronomy and Space Science, Faculty of Science, Erciyes University（埃尔吉耶斯大学理学院天文学与空间科学系）；Erciyes University, Astronomy and Space Science Observatory Application and Research Center（埃尔吉耶斯大学天文与空间科学观测应用与研究中心）；Department of Physics, Faculty of Arts and Sciences, Çanakkale Onsekiz Mart University（恰纳卡莱18三月大学文理学院物理系）；Astrophysics Research Center and Observatory, Çanakkale Onsekiz Mart University（恰纳卡莱18三月大学天体物理学研究中心和天文台）；Variable Stars South (VSS), Congarinni Observatory（南变星组织（VSS），康加里尼天文台）
BSN-VIII: Detailed Photometric Modeling of Ten W UMa Contact Binaries and a Revised Empirical Period-Mass Relationship
Observatoire de Paris, CNRS, PSL（巴黎天文台）；Raderon AI Lab.（雷顿人工智能实验室）；University of Texas at Dallas（德克萨斯大学达拉斯分校）；Shandong University（山东大学）；Société Astronomique de France（法国天文学会）
The Phenomenological Classification of TESS Eclipsing Binaries
Shandong University（山东大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；University of the Chinese Academy of Sciences（中国科学院大学）
A Photometric Study of Four Recently Discovered Contact Binaries: 1SWASP J064501.21+342154.9, 1SWASP J155822.10-025604.8, 1SWASP J212808.86+151622.0 and UCAC4 436-062932
Temperature and Distance Dependence of Tidal Circularization in Close Binaries: A Catalog of Eclipsing Binaries in the Southern Hemisphere Observed by the TESS Satellite
