Physical Parameters of the Visually Close Binary Systems Hip70973 and Hip72479

Abstract

Atmospheric modelling of the components of the visually close binary systems Hip70973 and Hip72479 was used to estimate the individual physical parameters of their components. The model atmospheres were constructed using a grid of Kurucz solar metalicity blanketed models and used to compute a synthetic spectral energy distribution for each component separately, and hence for the combined system. The total observational spectral energy distributions of the systems were used as a reference for comparison with the synthetic ones. We used the feedback modified parameters and iteration method to obtain the best fit between synthetic and observational spectral energy distributions. The physical parameters of the components of the system Hip70973 were derived as T eff a ¼ 5700

Comparison of Gaia and Hipparcos parallaxes of close visual binary stars and the impact on determinations of their masses

“…The rich data of Gaia DR2 are already being implemented in solving orbits and masses of binary and multiple systems, see for example Tokovinin's work (Tokovinin 2018a(Tokovinin ,b, 2019aTokovinin et al 2019;Tokovinin 2019c). It is also very useful in determining the physical and geometrical parameters of BSs, using Al-Wardat's method, which has been used to analyse several solar-type binary and triple systems (Al-Wardat 2009;Al-Wardat & Widyan 2009;Al-Wardat 2012;Al-Wardat et al 2014cMasda et al 2016;Al-Wardat et al 2017;Masda et al 2019b), and was successfully applied to subgiant BSs like HD 25811, HD 375, HD 6009 (Al-Wardat et al 2014a,b;Al-Wardat 2014) and Hip 68170 in this work.…”

Physical and geometrical parameters of the binary system gliese 150.2

“…The total energy flux from a binary star is created from the net luminosity of the components a and b located at a distance d from the Earth [1]. So we can write:…”

Complex Analysis of the Stellar Binary HD25811: A Subgiant System

“…To calculate the individual components’ preliminary input parameters ( T eff and log g ), we followed the procedures explained in Al-Wardat (2012) using the following relations (e.g., Lang 1992; Gray 2005): where we used the bolometric corrections of Lang (1992) & Gray (2005), T ⊙ = 5777K and extinction ( A v ) given in Table 1 by NASA/ IPAC.…”

“…Combining spectrophotometry with atmospheric modelling gives a new method for the accurate determination of the physical and geometrical parameters of both components of VCBS, in addition to the estimation of their spectral types, luminosity classes, and ages. This method, first advised by Al-Wardat (2002a, 2007), was applied to several VCBS such as ADS11061, Cou1289, Cou1291, Hip11352, Hip11253, Hip70973, and Hip72479 (Al-Wardat 2002a, 2007, 2009, 2012; Al-Wardat & Widyan 2009).…”

“…This method, first advised by Al-Wardat (2002a, 2007, was applied to several VCBS such as ADS11061, Cou1289, Cou1291, Hip11352, Hip11253, Hip70973, and Hip72479 (Al-Wardat 2002a, 2007, 2009, 2012Al-Wardat & Widyan 2009).…”