A METHOD FOR DETERMINING THE PHYSICAL PARAMETERS OF HOT SUPERGIANTS BASED ON SPECTRAL ENERGY DISTRIBUTION ANALYSIS
This study determines the physical parameters of B- and A-type hot supergiants through the construction and analysis of their spectral energy distributions (SEDs). These luminous stars are in the late stages of stellar evolution and are important for understanding stellar structure and the chemical...
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| Main Authors: | , , , , , |
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| Format: | Article |
| Language: | English |
| Published: |
Al-Farabi Kazakh National University
2025-06-01
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| Series: | Physical Sciences and Technology |
| Online Access: | https://phst.kaznu.kz/index.php/journal/article/view/523 |
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| Summary: | This study determines the physical parameters of B- and A-type hot supergiants through the construction and analysis of their spectral energy distributions (SEDs). These luminous stars are in the late stages of stellar evolution and are important for understanding stellar structure and the chemical evolution of galaxies. Despite the existence of earlier studies, many supergiants remain insufficiently characterized due to the complexity of observations.
We refined the effective temperature Teff, surface gravity (log g), and interstellar extinction Av for a sample of 16 supergiants using multiwavelength photometry spanning from the ultraviolet to the infrared. A dedicated software package written in Fortran was used to convert observed magnitudes into physical fluxes and compare them with synthetic photometry derived from Castelli & Kurucz model atmospheres. The optimal parameter set for each star was obtained by minimizing the deviations between the observed and model SEDs, iterating over Av values.
The resulting parameters show good agreement with those published in the literature, confirming the reliability of our approach. In several cases, deviations in the infrared suggested the presence of circumstellar dust, underscoring the value of SED analysis for identifying secondary features. This work contributes to a more accurate characterization of hot supergiants and illustrates the broader applicability of SED-based techniques in stellar astrophysics.
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| ISSN: | 2409-6121 2522-1361 |