M3DIS - a grid of 3D radiation-hydrodynamics stellar atmosphere models for stellar surveys: I. Procedure, validation, and the sun
Context: Large-scale stellar surveys, such as SDSS-V, 4MOST, WEAVE, and PLATO, require accurate atmospheric models and synthetic spectra of stars for accurate analyses of fundamental stellar parameters and chemical abundances. Aims: The primary goal of our work is to develop a new approach to solve...
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| Main Authors: | , , , , , |
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| Format: | Article (Journal) |
| Language: | English |
| Published: |
August 2024
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| In: |
Astronomy and astrophysics
Year: 2024, Volume: 688, Pages: 1-20 |
| ISSN: | 1432-0746 |
| DOI: | 10.1051/0004-6361/202348448 |
| Online Access: | Verlag, kostenfrei, Volltext: https://doi.org/10.1051/0004-6361/202348448 Verlag, kostenfrei, Volltext: https://www.aanda.org/articles/aa/abs/2024/08/aa48448-23/aa48448-23.html 
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| Author Notes: | Philipp Eitner, Maria Bergemann, Richard Hoppe, Åke Nordlund, Bertrand Plez, and Jonas Klevas |
MARC
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| 520 | |a Context: Large-scale stellar surveys, such as SDSS-V, 4MOST, WEAVE, and PLATO, require accurate atmospheric models and synthetic spectra of stars for accurate analyses of fundamental stellar parameters and chemical abundances. Aims: The primary goal of our work is to develop a new approach to solve radiation-hydrodynamics (RHD) and generate model stellar spectra in a self-consistent and highly efficient framework. Methods: We build upon the Copenhagen legacy RHD code, the MULTI3D non-local thermodynamic equilibrium (NLTE) code, and the DISPATCH high-performance framework. The new approach allows us to calculate 3D RHD models of stellar atmospheres on timescales of a few thousand CPU hours and to perform subsequent spectrum synthesis in local thermodynamic equilibrium (LTE) or NLTE for the desired physical conditions within the parameter space of FGK-type stars. Results: We compare the 3D RHD solar model with other available models and validate its performance against solar observations, including the centre-to-limb variation of intensities and key solar diagnostic lines of H and Fe. We show that the performance of the new code allows to overcome the main bottleneck in 3D NLTE spectroscopy and enables calculations of multi-dimensional grids of synthetic stellar observables for comparison with modern astronomical observations. | ||
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