We report the identification of the bright (V${\sim}13.3$ mag) star FY Sct as a long period detached eclipsing binary using a combined ASAS-SN and ASAS light curve spanning 2000-2018. The orbital period is P${\sim}2.57$ years and the primary eclipse lasts ${\sim}73$ days. The eclipse profile is suggestive of a disk eclipsing binary rather than a stellar component. We also detect ${\sim}0.4$ mag pulsations with a period of P${\sim78}$ d. The next eclipse begins on September, 28, 2018. Further photometric and spectroscopic observations are encouraged, particularly when the system is in eclipse.
Twin binaries were identified among the eclipsing binaries with $δ$>--30$^\circ$ listed in the ASAS catalog. In addition to the known twin binaries in the literature, 68 new systems have been identified, photometric and spectroscopic observations were done. Color, spectral type, temperature, ratio of radii and masses of the components have been derived and presented. Including 12 twin binary systems that exist in both ASAS and the catalogue of absolute parameters of detached eclipsing binary stars, a total of 80 twin detached binary systems have been statistically studied. A comparison of the …
We use ASAS V-band and ASAS-SN g-band observations to model the long-period detached eclipsing binary ASASSN-21co. ASAS observations show an eclipse of depth V ~ 0.6 mag in April of 2009. ASAS-SN g-band observations from March of 2021 show an eclipse of similar duration and depth, suggesting an orbital period of 11.9 years. We combine the g-band observations with additional BVRI photometry taken during the eclipse to model the eclipse using PHOEBE. We find that the system is best described by two M giants with a ratio of secondary radius to primary radius of ~0.61. Optical spectra taken during…
The photometric and spectroscopic data for three double-lined detached eclipsing binaries were collected from the photometric and spectral surveys. The light and radial velocity curves of each binary system were simultaneously analyzed by using Wilson-Devinney (WD) code, and the absolute physical and orbital parameters of these binaries were derived. The masses of both components of ASASSN-V J063123.82+192341.9 were found to be $M_1 = 1.088 \pm 0.016$ and $M_2 = 0.883 \pm 0.016\ M_{\odot}$; and those of ASAS J011416+0426.4 were determined to be $M_1 = 0.934 \pm 0.046$ and $M_2 = 0.754 \pm 0.04…
Detached eclipsing binaries are a fundamental tool for measuring the physical parameters of stars that are effectively evolving in isolation. Starting from more than 40,000 eclipsing binary candidates identified by the All-Sky Automated Survey for Supernovae (ASAS-SN), we use PHOEBE to determine the sum of the fractional radii, the ratio of effective temperatures, the inclinations, and the eccentricities for 35,464 systems. We visually inspect all the light curve models to verify the model fits and examine the TESS light curves, when available, to select systems with evidence for additional ph…
Detached eclipsing binaries are the primary tool used to measure precise masses and radii of stars. In our previous paper estimating the parameters of more than 30,000 detached eclipsing binaries, we identified 766 eclipsing binaries with additional features in their All-Sky Automated Survey for Supernovae (ASAS-SN) and Transiting Exoplanet Survey Satellite (TESS) light curves. Here, we characterize these "extra-physics" systems, identifying eclipsing binaries with spotted stars, pulsating components, and candidate triple/quadruple systems. We use the Gaia, ATLAS, ZTF, and ASAS-SN variable sta…
Orbital and physical parameters of eclipsing binaries from the ASAS catalogue - V. Investigation of subgiants and giants: the case of ASAS J010538-8003.7, ASAS J182510-2435.5, and V1980 Sgr
We report long-termed UBVRIRcIc photometry of the highly eccentric 12.04 day detached eclipsing binary V490 Sct (V =13.1, B9.5+A0, e = 0.40), which we use to determine its relative and absolute parameters. The absolute masses, radii, and temperatures are Ma = 2.33+/-0.1 Msun, Ra = 1.91+/-0.04 Rsun, and Ta = 9960+/-60 K for the primary and Mb = 2.24+/-0.1 Msun, Rb = 1.86+/-0.04 Rsun, and Tb = 9700+/-80 K for the secondary. The system displays a slow periastron advance that is dominated by general relativity (GR). Our measurement, dw/dt = 0.86 deg/century, is 32% less then the expected rate, dw/…
Eclipsing systems are essential objects for understanding the properties of stars and stellar systems. Eclipsing systems with pulsating components are furthermore advantageous because they provide accurate constraints on the component properties, as well as a complementary method for pulsation mode determination, crucial for precise asteroseismology. The outcome of space missions aiming at delivering high-accuracy light curves for many thousands of stars in search of planetary systems has also generated new insights in the field of variable stars and revived the interest of binary systems in g…
Orbital and physical parameters of eclipsing binaries from the ASAS catalogue -- II. Two spotted M < 1 M$_\odot$ systems at different evolutionary stages
目标。我们提出了我们的详细的光谱和光度分析的结果，以前未知的< 1 M{_ \sun }分离食双星：ASAS J 045304 -0700.4和ASAS J 082552 -1622.8。方法.利用Keck-I望远镜上的高分辨率Echelle光谱仪（HIRES），我们获得了两个物体的光谱，覆盖了系统轨道的大部分。我们还获得了V和I波段测光与1.0米伊丽莎白望远镜的南非天文台（SAAO）。用PHOEBE和JKTEBOP程序计算了系统的轨道参数和物理参数。我们调查了这两个双星的演化状态与几套广泛使用的等时线。结果我们的模拟表明：（1）ASAS J 045304 -0700.4是一个古老的、贫金属的、活跃的系统，其组分质量为M1 = 0.8452 \pm 0.0056 M $_\odot$，M2 = 0.8390 \pm 0.0056 M $_\odot$，R1 = 0.848 \pm 0.005 R $_\odot$，R2 = 0.833 \pm 0.005 R $_\odot$，这使它处于主序星演化的末端--这是一个很少观察到的恒星演化阶段。(2)ASAS J 082552 -1622.8是一种富含金属，活动双星，成分质量为M1 = 0.703 \pm 0.003 M $_\odot$，M2 = 0.687 \pm 0.003 M $_\odot$和R1的半径= 0.694（+0.0…
We present a classification of the light curve morphologies of eclipsing binary systems observed by ASAS-SN based on their light curve images. The data of 16500 eclipsing systems having three different classes (detached Algol type, $β$ Lyr type, and W UMa type) are collected to construct their light curves. A deep learning algorithm containing the convolutional neural networks is employed on the images to achieve a satisfying classification. A code called ASEBCLASS is written in Python language, and it uses the TensorFlow platform through Keras API to employ the mathematical libraries in the t…
Orbital and physical parameters of eclipsing binaries from the ASAS catalogue -- I. A sample of systems with components' masses between 1 and 2 M$_\odot$
我们从\emph{All Sky Automated Survey}（ASAS）数据库中获得的18个样本的绝对物理和轨道参数的测光和我们自己的径向速度测量的基础上。径向速度（RV）的计算使用的光谱，我们收集了3.9米的英澳望远镜和\emph{University College London Echelle Spectrograph}和1.9米的SAAO拉德克利夫望远镜和它的\emph{Grating Instrument for Radiation Analysis with a Fibre Fed Echelle}。为了获得尽可能精确的RV，大多数系统都使用AAT/UCLES的碘池进行观察和/或使用二维互相关技术（TODCOR）进行分析。使用合成模板光谱作为参考，用TODCOR测量RV。然而，对于两个对象，我们使用我们自己的方法的层析分离的二进制光谱提供观察到的模板光谱的RV测量，并提高RV精度甚至更多。对于这些二进制之一，AI苯丙氨酸，我们能够获得的轨道解的RV $rms$为62和24 m s $^{-1}$的小学和中学分别。对于该系统，$M \sin^3{i}$的精密度为0.08%。为了进行分析，我们使用了ASAS数据库中可用的光度法。利用PHOEBE和JKTEBOP程序将RV曲线和光变曲线结合起来，得到了系统的绝对物理参数。有了精确的RV，我们在几种情况下能够在质量上达到…
We present results of the analysis of light and radial velocity (RV) curves of eight detached eclipsing binaries observed by the All-Sky Automated Survey, which we have followed up with high-resolution spectroscopy, and were later observed by the $Kepler$ satellite as part of the $K2$ mission. The RV measurements came from spectra obtained with OAO-188/HIDES, MPG-2.2m/FEROS, SMARTS 1.5m/CHIRON, Euler/CORALIE, ESO-3.6m/HARPS, and OHP-1.93/ELODIE instruments. The $K2$ time-series photometry was analyzed with the JKTEBOP code, with out-of-eclipse modulations of different origin taken into account…
Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue - VII. V1200 Centauri: a bright triple in the Hyades moving group
通过对\textit{All Sky Automated Survey}（ASAS）和SuperWASP数据库的光谱观测和光变曲线的分析，给出了V1200~Centauri（ASAS~J135218-3837.3）的轨道和物理参数。利用互相关技术\textsc{todcor}，从OUC 50厘米望远镜和PUCHEROS摄谱仪以及1.2米欧拉望远镜和CORALIE摄谱仪获得的高分辨率光谱中计算了径向速度。我们发现系统的绝对参数为$M_1= 1.394\pm 0.030$ M $_\odot$，$M_2= 0.866\pm 0.015$ M $_\odot$，$R_1= 1.39\pm 0.15$ R $_\odot$，$R_2= 1.10\pm 0.25$ R $_\odot$ .我们研究了双星的演化状态和运动学，我们的结果表明V1200~Centauri可能是毕宿星移动群的成员，但大部分膨胀的次级半径可能表明该系统可能更年轻，大约3000万年。我们还发现，食对是由另一个恒星质量的物体在351天的轨道上运行的，这对于等级三元组来说是不寻常的短。这使得V1200 Cen成为测试多颗恒星形成模型的潜在目标。
Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue - X. Three high-contrast systems with secondaries detected with IR spectroscopy
We present new photometric and spectroscopic observations and analyses for the eclipsing binary systems V1241 Tau and GQ Dra. Our photometric light and radial velocity curves analyses combining with the TESS light curves show that both are conventional semi-detached binary systems. Their absolute parameters are also derived. We present the $O-C$ analyses of the systems and we propose the most possible orbital period modulating mechanisms. Furthermore, Fourier analyses are applied to the photometric residual data of the systems to check for the pulsational behavior of the components. We conclud…
IM Per is a triple star system whose eclipsing pair masses and radii are accurate to within 1 \%. The TESS light curve of the program target exhibits partial eclipses and multiple oscillations with mmag-level amplitudes. It is found that the oscillations affect eclipse timing measurements. Binary modeling of the high-quality TESS data indicates that the eclipsing components of the triple system are twin dwarfs with parameters of $M_2$/$M_1$ = 0.995, $R_2$/$R_1$ = 0.901, and $Δ$($T_{\rm eff,1}$--$T_{\rm eff,2}$) = 12 K in an eccentric ($e$ = 0.049), detached configuration. The third light of $l…
Orbital period and multi-color light curves' investigation of OW Leo are presented for the first time. The orbital period of OW Leo is corrected from $P = 0.325545$ days to $P = 0.32554052$ days in our work, and the observational data from the All-Sky Automated Survey for SuperNovae (ASAS-SN) are used to test the newly determined orbital period. Then, the phased light curves are calculated with the new period and the Wilson-Devinney program is applied to model the light curves, which reveal that OW Leo is a W-subtype shallow contact binary system ($q = 3.05$, $f = 12.8\,\%$). The absolute phys…
Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue - VI. AK Fornacis - a rare, bright K-type eclipsing binary
我们提出了一个明亮的（V=9.14），附近（d=31秒差距），晚型分离食二进制AK天炉座的光度和光谱分析相结合的结果。这个P=3.981 d的系统以前没有被认为是双线光谱双星，这是这个独特目标的第一个完整的物理模型。利用FEROS、CORALIE和HARPS摄谱仪，我们收集了一些高分辨率的光谱，以计算双星两个组成部分的径向速度。测量是用我们自己的解缠程序和TODCOR技术完成的，后来又与ASAS和SuperWASP档案中的光度法相结合。我们还使用Spectroscopy Made Easy（SME）软件包对组分光谱进行了大气分析。我们的分析表明，AK For由两个活跃的冷矮星组成，质量分别为$M_1=0.6958 \pm 0.0010$和$M_2=0.6355 \pm 0.0007$ M $_\odot$，半径分别为$R_1=0.687 \pm 0.020$和$R_2=0.609 \pm 0.016$ R $_\odot$，金属丰度略低于太阳。两个组件的参数都很好地再现了模型。AK For是已知的K型或M型食双星中最亮的系统。它的轨道周期是最长的之一，旋转速度是最低的之一，这使我们能够获得非常精确的径向速度测量。物理参数的精度，我们得到的地方AK的二进制文件中最好的质量测量在文献中。它还填补了我们对0.5-0.8 M $_\odot$范围内的恒星以及短周期和长周期系统的知识空白。所…
