Calculation of molecular line intensity in stellar atmospheres
| Autor: | Beatriz Barbuy, Júlio Trevisan, A. A. de Almeida |
|---|---|
| Rok vydání: | 2018 |
| Předmět: |
Physics
010504 meteorology & atmospheric sciences Molecular line Stellar atmosphere FOS: Physical sciences Astronomy and Astrophysics Context (language use) Astrophysics medicine.disease_cause 01 natural sciences Spectral line Stars Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science 0103 physical sciences Code (cryptography) medicine ATMOSFERAS ESTELARES 010303 astronomy & astrophysics Intensity (heat transfer) Ultraviolet Solar and Stellar Astrophysics (astro-ph.SR) 0105 earth and related environmental sciences |
| Zdroj: | Repositório Institucional da USP (Biblioteca Digital da Produção Intelectual) Universidade de São Paulo (USP) instacron:USP |
| DOI: | 10.48550/arxiv.1812.02414 |
| Popis: | Molecular line intensity calculations are not a straightforward task. We present a description of the basics for including molecular linesin synthetic spectra, and of the input data needed. We aim both at describing ways in which molecular lines are computed in the context of photospheres of F-G-K stars, and to present a new online available version of our code for spectrum synthesis of cool stars. We apply calculations to molecular bands in the ultraviolet, visible and near-infrared main features, and comparisons with spectra of reference stars are shown. We provide user-friendly tools for the free use of the code PFANT. The code is available at http://trevisanj.github.io/PFANT. Comment: Publications of the Astronomical Society of Australia, in press |
| Databáze: | OpenAIRE |
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