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 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 1997A&A...319..648H).
A FORTRAN code representing a parametric mass-loss prescription for,
e.g., stellar evolution modelling, is available at
http://coolstars.astro.uu.se
where also future updates will be posted.
File Summary:
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FileName Lrecl Records Explanations
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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
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Byte-by-byte Description of file: tables.dat
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Bytes Format Units Label Explanations
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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,
ρd/ρg, calculated from fc
65 A1 --- n_Md/Mg [*] numerical problems (1)
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Note (1): * when no meaningful wind properties could be derived due to
numerical problems.
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Acknowledgements:
L. Mattsson, mattsson(at)fysast.uu.se
(End) Patricia Vannier [CDS] 04-Jun-2010