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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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Bibliographic Details
Main Authors: Eitner, Philipp (Author) , Bergemann, Maria (Author) , Hoppe, Richard (Author) , Nordlund, Åke (Author) , Plez, Bertrand (Author) , Klevas, Jonas (Author)
Format: Article (Journal)
Language:English
Published: August 2024
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
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Summary: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.
Item Description:Online verfügbar: 2. August 2024
Gesehen am 30.06.2025
Physical Description:Online Resource
ISSN:1432-0746
DOI:10.1051/0004-6361/202348448

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