Predicting photospheric UV emission from stellar evolutionary models
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arXiv
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| Auteurs principaux: | , , , |
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| Format: | Preprint |
| Publié: |
2024
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| _version_ | 1866912073487745024 |
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| author | Wang, Song Li, Xue Han, Henggeng Liu, Jifeng |
| author_facet | Wang, Song Li, Xue Han, Henggeng Liu, Jifeng |
| contents | Stellar ultraviolet (UV) emission serves as a crucial indicator for estimating magnetic activity and evaluating the habitability of exoplanets orbiting stars. In this paper, we present a straightforward method to derive stellar photospheric UV emission for F to M main-sequence stars. By using PARSEC models, we establish relations between near-UV (NUV) and far-UV (FUV) magnitudes from the Galaxy Evolution Explorer (GALEX), NUV magnitudes from the China Space Station Telescope, and stellar effective temperatures and Gaia BP$-$RP color for different metallicities. Together with the observed sample, we find that for NUV emission, the photospheric contribution to the observed flux is less than 20% for M stars, around 10% to 70% for G stars, and ranges from 30% to 85% for G and F stars. For FUV emission, the photospheric contribution is less than $10^{-6}$ for M stars, below $10^{-4}$ for K stars, around $10^{-4}$ to 10% for G stars, and between 6% and 50% for F stars. Our work enables the simple and effective determination of stellar excess UV emission and the exploration of magnetic activity. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2410_11611 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Predicting photospheric UV emission from stellar evolutionary models Wang, Song Li, Xue Han, Henggeng Liu, Jifeng Solar and Stellar Astrophysics Earth and Planetary Astrophysics Astrophysics of Galaxies Stellar ultraviolet (UV) emission serves as a crucial indicator for estimating magnetic activity and evaluating the habitability of exoplanets orbiting stars. In this paper, we present a straightforward method to derive stellar photospheric UV emission for F to M main-sequence stars. By using PARSEC models, we establish relations between near-UV (NUV) and far-UV (FUV) magnitudes from the Galaxy Evolution Explorer (GALEX), NUV magnitudes from the China Space Station Telescope, and stellar effective temperatures and Gaia BP$-$RP color for different metallicities. Together with the observed sample, we find that for NUV emission, the photospheric contribution to the observed flux is less than 20% for M stars, around 10% to 70% for G stars, and ranges from 30% to 85% for G and F stars. For FUV emission, the photospheric contribution is less than $10^{-6}$ for M stars, below $10^{-4}$ for K stars, around $10^{-4}$ to 10% for G stars, and between 6% and 50% for F stars. Our work enables the simple and effective determination of stellar excess UV emission and the exploration of magnetic activity. |
| title | Predicting photospheric UV emission from stellar evolutionary models |
| topic | Solar and Stellar Astrophysics Earth and Planetary Astrophysics Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2410.11611 |