Synthetic photometry for carbon-rich giants. IV. An extensive grid of dynamic atmosphere and wind models

TL;DR

This paper presents an extensive grid of dynamic atmosphere and wind models for carbon-rich AGB stars, providing synthetic spectra and photometry to improve understanding of their evolution, spectral properties, and contribution to galactic chemical enrichment.

Contribution

It introduces a comprehensive set of 540 dynamic models with detailed spectra and photometry, covering a range of stellar parameters and pulsation amplitudes, and compares them with observations.

Findings

Good agreement in mass-loss rates vs. (J-K) colours

Models reproduce K magnitudes vs. (J-K) colours well

Some discrepancies due to input parameters and model assumptions

Abstract

The evolution and spectral properties of stars on the AGB are significantly affected by mass loss through dusty stellar winds. Dynamic atmosphere and wind models are an essential tool for studying these evolved stars, both individually and as members of stellar populations, to understand their contribution to the integrated light and chemical evolution of galaxies. This paper is part of a series testing state-of-the-art atmosphere and wind models of carbon stars against observations, and making them available for use in various theoretical and observational studies. We have computed low-resolution spectra and photometry (in the wavelength range 0.35-25 mu) for a grid of 540 dynamic models with stellar parameters typical of solar-metallicity C-rich AGB stars and with a range of pulsation amplitudes. The models cover the dynamic atmosphere and dusty outflow (if present), assuming spherical symmetry, and taking opacities of gas-phase species and dust grains consistently into account. To characterize the time-dependent dynamic and photometric behaviour of the models in a concise way we defined a number of classes for models with and without winds. Comparisons with observed data in general show a quite good agreement for example regarding mass-loss rates vs. (J-K) colours or K magnitudes vs. (J-K) colours. Some exceptions from the good overall agreement, however, are found and attributed to the range of input parameters (e.g. relatively high carbon excesses) or intrinsic model assumptions (e.g. small particle limit for grain opacities). While current results indicate that some changes in model assumptions and parameter ranges should be made in the future to bring certain synthetic observables into better agreement with observations, it seems unlikely that these pending improvements will significantly affect the mass-loss rates of the models.