Along with the complete set of physical and geometrical parameters, we present the habitability and stability of the proposed planets around the young stellar system HD 21841. Our study utilizes an orbital analysis of the system, employing Tokovinin’s Method and incorporating 12 new speckle interferometric measurements that collectively span approximately 90° of the orbit. Additionally, we employ Al-Wardat’s method for analyzing stellar systems and variable stars, in conjunction with Gaia DR3 astrometry and spectral data, to provide a comprehensive spectrophotometric assessment of the components. This method utilizes Kurucz’s model stellar atmospheres and available photometric data to develop synthetic spectral energy distributions (SEDs) for each component and subsequently the entire system. We can identify the physical parameters and the optimal solution by comparing the synthetic SED of the entire system with the observational data from Gaia. The analysis successfully determined the stellar parameters of the system for the first time, revealing the following: Teff. = 5945 ± 80 K, R = 1.018 ± 0.05 R⊙,  for the primary component and Teff. = 5700 ± 80 K, R = 0.975 ± 0.06 R⊙,  for the secondary component. Both components are found to have solar metallicity and are approximately 1 billion years old. The combined spectrophotometric and dynamical analysis resulted in precise stellar masses and a new dynamical parallax of πdyn = 23.756 ± 0.001 mas, consistent with the Gaia DR3 value (π = 24.31 ± 0.19). In addition to studying the habitability and stability of the exoplanets within the system, we explored the processes of its formation and evolution. 

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