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

Abstract

We present the complete set of physical and geometrical parameters of the visual close binary system GJ\,9830 for the first time by using Al-Wardat's complex method. This method combines magnitude difference from speckle interferometry, synthetic spectral energy distributions of the binary components which are constructed depending on grids of Kurucz blanketed models (Atlas9), along with the orbital solution by using Tokovinin's dynamical method to estimate the parameters of the individual components. The analysis of the system by using synthetic photometry resulted in the following set of parameters: $T_{eff.}=6220\pm 100$ \,K, $\log \mathrm{g}=4.30\pm 0.12$, $R=1.10\pm 0.08R_{\odot }$ for the primary component and $T_{eff.}=4870\pm 100$\,K, $\log \mathrm{g}=4.60\pm 0.11$, $R=0.709\pm 0.07R_{\odot }$ for the secondary component. The recently published dynamical parallax from \textit{Gaia} space mission was used to calculate the total mass of the binary system as $1.75\pm 0.06{\mathcal{M}}_{\odot }$ which coincides with those estimated by using Al-Wardat's method as ${\mathcal{M}}^A=1.18\pm 0.10{\mathcal{M}}_{\odot }$, ${\mathcal{M}}^B=0.75\pm 0.08{\mathcal{M}}_{\odot }$. The analysis of the system reveals that both components belong to main sequence stars with an age around $1.4\pm 0.50$\,Gyr. The evolutionary tracks and isochrones of the system's components are discussed, and the fragmentation process is suggested as the most likely process for the formation of the system.

13 page, 5 figures

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Cited by in corpus (3)

• Comparison of Gaia and Hipparcos parallaxes of close visual binary stars and the impact on determinations of their masses
• The stellar system HIP 101227: is it a binary, a triple or a quadruple system?
• A Comprehensive Study of the Physical and Geometrical Characteristics of the Close Visual Binary System HIP 45571