Precise Physical Parameters, Habitability, and Orbital Stability of Sun-like SB2 Systems: HD 130669, HD 184467, HD 191854, and HD 214222

TL;DR

This study addresses precise physical and orbital characterization of four Sun-like SB2 systems by fusing visual and spectroscopic data with Al-Wardat's atmospheric modeling. The approach yields refined masses and orbital parallaxes, resolves parallax discrepancies, and provides atmospheric parameters by fitting synthetic SEDs to observations, placing components on evolutionary tracks. The authors also assess dynamical stability and dynamically informed habitable zones, finding no circumbinary HZs but potential circumstellar zones in several systems, with HD 191854 showing the most favorable conditions for habitability. The results support the viability of targeted planet searches around Sun-like binaries and demonstrate a robust, multi-technique workflow that can be extended with Gaia DR4 data to improve sample statistics and habitability assessments in binary environments. The methodology, validated against Gaia/Hipparcos data, has practical implications for planning planet searches and modeling planetary stability in multi-star systems.

Abstract

This work analyzes four Sun-like double-lined spectroscopic binary (SB2) systems by combining visual and spectroscopic observational data with Al-Wardat's atmospheric modeling method to accurately determine their fundamental parameters. For each system, we determine stellar masses, orbital parallaxes, effective temperatures, spectral types, semimajor axes, and eccentricities with high precision, resolving discrepancies between astrometric and spectroscopic measurements. Moreover, we assess the potential for stable planetary orbits in these systems. We also calculate habitable zones around these binaries based on the orbital evolution of planetary orbits. These systems may represent promising targets for future extrasolar planet searches around Sun-like stars due to their robust physical and orbital parameters that can be used to determine planetary habitability and stability.

Figures (14)

• Figure 1: Synthetic spectral energy distribution (SED) of the binary system HD 130669 constructed using Al-Wardat’s complex method and Kurucz’s ATLAS9 model atmospheres. The total flux (black), flux of component A (blue), and flux of component B (orange) are shown. Overplotted are observed photometric fluxes from 2MASS (J, H), Gaia (BP, RP), and Johnson photometry (B, V) with their respective magnitudes. This comparison validates the consistency between the synthetic model and observed data across a wide wavelength range ($3,500-18,000 \mathring{A}$).
• Figure 2: Synthetic spectral energy distribution (SED) of the binary system HD 184467 constructed using Al-Wardat’s complex method and Kurucz’s ATLAS9 model atmospheres. The total flux (black), flux of component A (blue), and flux of component B (orange) are shown. Overplotted are observed photometric fluxes from 2MASS (J, H), Gaia (BP, RP), and Johnson photometry (B, V) with their respective magnitudes. This comparison validates the consistency between the synthetic model and observed data across a wide wavelength range ($3,500-18,000 \mathring{A}$).
• Figure 3: Synthetic spectral energy distribution (SED) of the binary system HD 191854 constructed using Al-Wardat’s complex method and Kurucz’s ATLAS9 model atmospheres. The total flux (black), flux of component A (blue), and flux of component B (orange) are shown. Overplotted are observed photometric fluxes from 2MASS (J, H), Gaia (BP, RP), and Johnson photometry (B, V) with their respective magnitudes. This comparison validates the consistency between the synthetic model and observed data across a wide wavelength range ($3,500-18,000 \mathring{A}$).
• Figure 4: Synthetic spectral energy distribution (SED) of the binary system HD 21422 constructed using Al-Wardat’s complex method and Kurucz’s ATLAS9 model atmospheres. The total flux (black), flux of component A (blue), and flux of component B (orange) are shown. Overplotted are observed photometric fluxes from 2MASS (J, H), Gaia (BP, RP), and Johnson photometry (B, V) with their respective magnitudes. This comparison validates the consistency between the synthetic model and observed data across a wide wavelength range ($3,500-18,000 \mathring{A}$).
• Figure 5: H–R diagrams for the binary systems HD 130669, HD 184467, HD 191854, and HD 214222. The positions of the individual stellar components (A and B) are plotted with their respective uncertainties. Evolutionary tracks corresponding to different stellar masses are shown by black lines, while the system's best-fitting isochrone (age) is indicated by a red dotted line. The Zero-Age Main Sequence (ZAMS) is depicted as a thick solid black line. These diagrams were constructed using the evolutionary models to determine the masses and ages of the components based on their effective temperatures and luminosities.