Stellar parameters of the two binary systems: HIP 14075 and HIP 14230

Abstract

We present the stellar parameters of the individual components of the two old close binary systems HIP 14075 and HIP 14230 using synthetic photometric analysis. These parameters are accurately calculated based on the best match between the synthetic photometric results within three different photometric systems with the observed photometry of the entire system. From the synthetic photometry, we derive the masses and radii of HIP 14075 as: M A = 0.99 ± 0.19 M , R A = 0.877 ± 0.08 R for the primary and M B = 0.96 ± 0.15 M , R B = 0.821 ± 0.07 R for the secondary, and of HIP 14230 as: M A = 1.18 ± 0.22 M , R A = 1.234 ± 0.05 R for the primary and M B = 0.84 ± 0.12 M , R B = 0.820 ± 0.05 R for the secondary, both systems depend on Gaia parallaxes. Based on the positions of the components of the two systems on a theoretical Hertzsprung-Russell diagram, we find that the age of HIP 14075 is 11.5 ± 2.0 Gyr and of HIP 14230 is 3.5 ± 1.5 Gyr. Our analysis reveals that both systems are old close binary systems (≈> 4 Gyr). Finally, the positions of the components of both systems on the stellar evolutionary tracks and isochrones are discussed.

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

“…We investigated how measurements of the dynamical masses of the selected CVBSs are affected by the distances inferred from the parallax measurements in each of the catalogues discussed above. We also compared these results with masses estimated from two different indirect methods: Malkov’s photometric masses (Malkov et al 2012a,b) and Al-Wardat’s multi-parameter approach for analysing CVBSs (Al-Wardat 2002a,b, 2007; Al-Wardat et al 2014b; Al-Wardat, Widyan, & Al-thyabat 2014a; Al-Wardat et al 2016, 2017; Masda, Al-Wardat, & Pathan 2018a; Masda, Al-Wardat, & Pathan 2018c). The latter is a computationally complex method employing colours, colour indices, and magnitude differences of the system along with its parallax to build individual synthetic spectral energy distributions (SED) for each component of the system.…”

Modified Masses and Parallaxes of Close Binary Systems: HD 39438

“…It consolidates the magnitude difference measurements of speckle interferometry, combined spectral energy distributions (SEDs) of the spectrophotometric analysis with the aid of the grids of ATLAS9 models (Kurucz 1994) and radial velocity measurements (once available) to estimate the individual fundamental stellar parameters of binary systems, thereby determining the precise spectrophotometric masses of such binary systems. The method has been utilized to compare synthetic stellar photometry with observed stellar photometry to estimate the fundamental parameters of solar-type stars (Al-Wardat 2009, 2012Al-Wardat et al 2014a, 2014b, 2014c, 2016, 2017, 2021aMasda et al 2016Masda et al , 2018aMasda et al , 2018bMasda et al , 2019aMasda et al , 2019bMasda et al , 2021Widyan & Aljboor 2021;Yousef et al 2021).…”

Orbital and physical parameters of the close binary system GJ 9830 (HIP 116259)

“…It is a quantitatively analysis for the synthetic SED of a binary system which is about modifying stellar parameters such that the synthetic magnitudes fit the observed ones (Al-Wardat et al 2014b,a;Masda et al 2016;Al-Wardat et al 2017). The method, which should be followed to evaluate the stellar parameters of the binary system by using synthetic photometry throughout the analysis of the system was described in evident detials in previous paper (Masda et al 2018).…”

“…On the other hand, the physical parameters are of fundamental value in terms of testing the formation and evolution models of a binary system in addition to the orbital solution. As a result, we follow Al-Wardat's complex method (Al-Wardat 2007) which combines the results of spectrophotometry with the results of speckle interferometry to obtain the physical parameters (Al-Wardat 2012;Al-Wardat et al 2014bMasda et al 2016Masda et al , 2018. This method makes use of the entire spectral energy distributions (SEDs) of the binary systems, which are constructed with ATLAS9 atmospheric modeling (Kurucz 1994).…”

“…Two methods have been successfully applied to estimate the physical and geometrical parameters of several solar-type stars and sub-giant binary stars whether the observed spectra were available or not, such as HD 25811, HD 375, Gliese 762.1, FIN 350, COU 1511, HIP 105947 and two systems HIP 14075 and HIP 14230 (Al-Wardat et al 2014a,c, 2016, 2017Gumaan Masda et al 2018;Masda et al 2018).…”