An improved model for the upper atmosphere of Epsilon Eridani
The photochemistry and composition of the atmosphere of a planet orbiting a star in its habitable zone is critically influenced by the near and far UV radiation emitted by the host star. In particular, the extreme UV and X-rays photons can drive atmospheric mass loss. At the present some regions of...
Guardado en:
| Autores principales: | , |
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| Formato: | Articulo |
| Lenguaje: | Inglés |
| Publicado: |
2021
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| Materias: | |
| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/166632 |
| Aporte de: |
| Sumario: | The photochemistry and composition of the atmosphere of a planet orbiting a star in its habitable zone is critically influenced by the near and far UV radiation emitted by the host star. In particular, the extreme UV and X-rays photons can drive atmospheric mass loss. At the present some regions of the UV spectra are unobservable due to interstellar absorption, and for the characterization of the UV radiation environment around a planet, a reliable atmospheric stellar model for the host star is needed. In this work we present an initial stellar model for the upper atmosphere of the dK2V star, Epsilon Eridani. Here we extend our previous photosphere-chromosphere model that accurately reproduced the visible continuum and several important spectral features observed at CASLEO. In order to build the upper part of our model corresponding to the transition region and corona, data from HST and XMM obtained as part of the MUSCLES (Measurements of the Ultraviolet Spectral Characteristics of Low-mass Exoplanetary Systems) survey are going to be used. For this work, we started the development of the model using the data from HST only. The use of this new model, that takes in account the complete stellar atmosphere from the photosphere to the corona, allows us to obtain a reliable calculation of the radiation received by the planet. |
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