Study of Eclipsing Binary Physical Parameters. Case: CV Boo Aliyya Nur Rahma (a*), Mahasena Putra (a,b), Muhamad Irfan Hakim (a,b), Aprilia (a,b), Yayan Sugianto (a,b)
(a) Astronomy Study Program, Faculty of Mathematics and Natural Science, Institut Teknologi Bandung, Indonesia
* aliyyanurr[at]gmail.com
(b) Bosscha Observatory, Faculty of Mathematics and Natural Science, Institut Teknologi Bandung, Indonesia
Abstract
Eclipsing binary is a binary system in which the components are seen eclipsing each other from the Earth. Photometric and spectroscopic observation of eclipsing binaries show variation of their brightness (light curve) and radial velocity (velocity curve). Light and radial velocity curve analysis provide physical and geometrical parameters of the binary systems and their components, which is very important in stellar evolution studies, especially in the era of multi-wavelength surveys. These parameters are determined by solving inverse problem, i.e. finding the best-fitting model to the observational curves. Modern numerical models includes detailed physics of stellar atmosphere, geometry, and dynamics of the binary system. One of such models is PHOEBE (PHysics Of Eclipsing BinariEs) 2.3, which offers sophisticated methods to solve the inverse problem. It is solved by computing model curves from initial (estimated) parameters, optimizing them numerically, and sampling the optimized models. We studied CV Boo, a detached eclipsing binary with a period of 0.874 days, using PHOEBE 2.3. Light curve and radial velocity curves were obtained from the literature. Our best solution of the inverse problem in this study are \(q=0.9872\substack{+0.0005 \\ -0.0005}\), \(T{\textrm{s}}/T_{\textrm{r}}=0.9682\substack{+0.0010 \\ -0.0015}\), \((R{\textrm{p}}+R_{\textrm{s}})/a=0.5000 \substack{+0.0010\\-0.0013}\), \(\omega=85.36\substack{+0.13\\-0.13}\) deg, \(e=0.0101\substack{+0.0004\\-0.0003}\), \(i=91.891\substack{+0.073\\-0.07}\) deg. We discuss the steps in finding the solution and the results in this paper.
