2025RAA....25b5011M

We present the essential stellar parameters of the close visual triple system HD 2893 using Al-Wardat's method for analyzing binary and multiple star systems in conjunction with Kurucz's model atmospheres. This method accurately computes the spectrophotometric stellar masses through a combined synthetic spectral energy distribution approach that compares the results with observed data. The vigorous approach uses spectroscopic, photometric, and dynamical analysis to yield precise results. The method implements Gaia DR3 measurements and other measurements like those of Hipparcos and 2MASS All-Sky Catalog as a guide for the best fit between the synthetic spectra and observed photometry. The analysis gives precise spectrophotometric stellar masses for the system being ${{ \mathcal M }}_{{\rm{Sph}}}^{{\rm{A}}}\,=\,$$1.20\pm 0.07\,{{ \mathcal M }}_{\odot }$, ${{ \mathcal M }}_{{\rm{Sph}}}^{{\rm{B}}}\,=\,$$1.09\pm 0.06\,{{ \mathcal M }}_{\odot }$, and ${{ \mathcal M }}_{{\rm{Sph}}}^{{\rm{C}}}\,=\,$$0.46\pm 0.01\,{{ \mathcal M }}_{\odot }$. It shows that the three components are main sequence stars with an estimated age of around 1.0 Gyr. When integrated with the dynamical analysis, a new dynamical parallax for the system is obtained, π_dyn = 13.8528 ± 0.20 mas. Additionally, the discussion covers the formation and evolution of the triple system.