Temperature and density profiles in the corona of main-sequence stars induced by stochastic heating in the chromosphere
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| Format: | Preprint |
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2024
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| _version_ | 1866913685785542656 |
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| author | Barbieri, Luca Casetti, Lapo Verdini, Andrea Landi, Simone |
| author_facet | Barbieri, Luca Casetti, Lapo Verdini, Andrea Landi, Simone |
| contents | All but the most massive main-sequence stars are expected to have a rarefied and hot (million-Kelvin) corona like the Sun. How such a hot corona is formed and supported has not been completely understood yet, even in the case of the Sun. Recently, Barbieri et al. (A&A 2024, J. Plasma Phys. 2024) introduced a new model of a confined plasma atmosphere and applied it to the solar case, showing that rapid, intense, intermittent and short-lived heating events in the high chromosphere can drive the coronal plasma into a stationary state with temperature and density profiles similar to those observed in the solar atmosphere. In this paper we apply the model to main-sequence stars, showing that it predicts the presence of a solar-like hot and rarefied corona for all such stars, regardless of their mass. However, the model is not applicable as such to the most massive main-sequence stars, because the latter lack the convective layer generating the magnetic field loop structures supporting a stationary corona, whose existence is assumed by the model. We also discuss the role of stellar mass in determining the shape of the temperature and density profiles. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2411_07868 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Temperature and density profiles in the corona of main-sequence stars induced by stochastic heating in the chromosphere Barbieri, Luca Casetti, Lapo Verdini, Andrea Landi, Simone Solar and Stellar Astrophysics All but the most massive main-sequence stars are expected to have a rarefied and hot (million-Kelvin) corona like the Sun. How such a hot corona is formed and supported has not been completely understood yet, even in the case of the Sun. Recently, Barbieri et al. (A&A 2024, J. Plasma Phys. 2024) introduced a new model of a confined plasma atmosphere and applied it to the solar case, showing that rapid, intense, intermittent and short-lived heating events in the high chromosphere can drive the coronal plasma into a stationary state with temperature and density profiles similar to those observed in the solar atmosphere. In this paper we apply the model to main-sequence stars, showing that it predicts the presence of a solar-like hot and rarefied corona for all such stars, regardless of their mass. However, the model is not applicable as such to the most massive main-sequence stars, because the latter lack the convective layer generating the magnetic field loop structures supporting a stationary corona, whose existence is assumed by the model. We also discuss the role of stellar mass in determining the shape of the temperature and density profiles. |
| title | Temperature and density profiles in the corona of main-sequence stars induced by stochastic heating in the chromosphere |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2411.07868 |