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J/A+A/509/A14       Grid of solar-metallicity wind models    (Mattsson+, 2010)

Dust driven mass loss from carbon stars as a function of stellar parameters. I. A grid of solar-metallicity wind models. Mattsson L., Wahlin R., Hoefner S. <Astron. Astrophys. 509, A14 (2010)> =2010A&A...509A..14M
ADC_Keywords: Models, atmosphere ; Stars, carbon ; Stars, giant ; Mass loss Keywords: stars: AGB and post-AGB - stars: atmospheres - stars: carbon - circumstellar matter - stars: evolution - stars: mass-loss Abstract: Knowing how the mass loss of carbon-rich AGB stars depends on stellar parameters is crucial for stellar evolution modelling, as well as for the understanding of when and how circumstellar structures emerge around these stars, e.g., dust shells and so-called detached shells of expelled gas. The purpose of this paper is to explore the stellar parameter space using a numerical radiation hydrodynamic (RHD) model of carbon-star atmospheres, including a detailed description of dust formation and frequency-dependent radiative transfer, in order to determine how the mass loss of carbon stars changes with stellar parameters. Description: The file online.dat contains all the data presented in the paper. The table include input parameters and the resulting mean mass loss rate, mean velocity at the outer boundary and mean degree of dust condensation at the outer boundary. The dust-to-gas mass ratio is calculated as described in Hofner & Dorfi (1997A&A...319..648H). A FORTRAN code representing a parametric mass-loss prescription for, e.g., stellar evolution modelling, is available at where also future updates will be posted. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tables.dat 65 720 Input parameters (L*, Teff, log(C-O), Per) and the resulting average mass loss rate, average wind speed and the mean degree of dust condensation at the outer boundary
Byte-by-byte Description of file: tables.dat
Bytes Format Units Label Explanations
1- 4 F4.2 km/s dvp Piston velocity amplitude (2.00, 4.00 or 6.00) 6- 9 F4.2 solMass Mass Stellar mass (0.75, 1.00, 1.50 or 2.00) 11- 14 F4.2 [solLum] logL Log of bolometric luminosity (3.55, 3.70, 3.85, 4.00 or 4.15) 16- 19 I4 K Teff Effective temperature (2400, 2600, 2800, 3000 or 3200) 21- 24 F4.2 [-] log(C-O) Carbon excess (8.20, 8.50, 8.80 or 9.10) 25 A1 --- n_log(C-O) [*] numerical problems (1) 26- 28 I3 d Per Pulsation period (221, 295, 393, 524 or 699) 30- 37 E8.2 solMass/yr dM/dt ?=- Average mass-loss rate 38 A1 --- n_dM/dt [*] numerical problems (1) 39- 46 E8.2 km/s uout ?=- Average wind/outflow speed 47 A1 --- n_uout [*] numerical problems (1) 48- 55 E8.2 --- fc ?=- Mean degree of dust condensation 56 A1 --- n_fc [*] numerical problems (1) 57- 64 E8.2 --- Md/Mg ?=- Mean dust-to-gas mass ratio, ρdg, calculated from fc 65 A1 --- n_Md/Mg [*] numerical problems (1)
Note (1): * when no meaningful wind properties could be derived due to numerical problems.
Acknowledgements: L. Mattsson, mattsson(at)
(End) Patricia Vannier [CDS] 04-Jun-2010
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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