Physical and orbital properties of the stellar system HIP 43766

Abstract

In this paper, we present the analysis of the stellar binary system HIP 43766 to determine its properties. We rely on dynamical modeling and atmospheric modeling with recent data to determine the orbital solution and the physical properties of the system. There is a consistency between observed and synthetic photometry obtained using atmospheric modeling. The calculated dynamical mass sum of the system ranged between 1.691 and 2.609 solar masses, while it ranges between 2.0 and 2.1 as estimated utilizing atmospheric modeling. This could be due to inaccuracy in estimating the orbit, which could be modified with future observations with more relative positional measurements. The parameters of the system and the position of the components on the evolutionary tracks show that the system consists of F5 and G5 subgiant stars, mostly formed by fragmentation. A dynamical mass sum is predicted for the system.

Speckle-interferometric Study of Close Visual Binary System HIP 11253 (HD 14874) using Gaia (DR2 and EDR3)

“…In this paper, we use two methods. The first one is Al-Wardatʼs method for analyzing binary and multiple stellar systems (BMSSs), which was introduced by Al-Wardat (2002), and has been used to analyze many CVBSs and BMSSs (Al-Wardat & Widyan 2009;Al-Wardat 2012;Masda et al 2019;Widyan & Aljboor 2021;Al-Tawalbeh et al 2021;Al-Wardat et al 2021;Abu-Dhaim et al 2022). The main idea of Al-Wardatʼs method is to build entire spectral energy distributions (SEDs) of BMSSs using the model atmospheres like those of (ATLAS9) (Kurucz 1994), by implementing the available observational measurements like magnitude difference and color indices.…”

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).…”

“…On the one hand, synthetic stellar photometry is mainly utilized to obtain the fundamental stellar parameters more precisely through comparing their results with the observed ones (Al-Wardat et al 2014a, 2014b, 2021aMasda et al 2018aMasda et al , 2018bMasda et al , 2019aMasda et al , 2019bMasda et al , 2021Widyan & Aljboor 2021). Synthetic photometry is synthetic analysis of the results of the spectroscopic analysis (synthetic SED) of the binary system.…”