J/A+AS/126/39 Models of circumstellar dust shells (Steffen+ 1997)
Hydrodynamical models and synthetic spectra of circumstellar dust shells
around AGB stars. I. Stationary solutions.
Steffen M., Szczerba R., Men'shchikov A., Schoenberner D.
<Astron. Astrophys. Suppl. Ser. 126, 39 (1997)>
=1997A&AS..126...39S 1997A&AS..126...39S (SIMBAD/NED BibCode)
ADC_Keywords: Models, evolutionary
Keywords: stars: AGB and post-AGB - circumstellar matter - stars: mass loss -
dust, extinction - hydrodynamics - radiative transfer -
Description:
Main properties of the steady state hydrodynamical models of
circumstellar gas/dust shells around late type giants, computed for
different stellar parameters (mass, luminosity, effective temperature)
and dust composition (astronomical silicates, graphite, or amorphous
carbon, with properties given in Tab.1 and Fig.1). Each table lists
the results as a function of the adopted mass loss rate for fixed
stellar parameters and dust properties. Tables 2 - 11 are related to
Figures 2 - 11: Each of the figures shows the velocity structure and
the resulting spectral energy distribution for a subset of models
listed in the respective table.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tables 72 108 Models results (table2-11)
tables.tex 106 393 LaTeX version of the tables
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Byte-by-byte Description of file: tables
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Bytes Format Units Label Explanations
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1- 2 A2 --- Model Model name (1)
3 A1 --- n_Model [mn] Note on Model (2)
5- 8 E4.0 solMass/yr MassLoss ? Mass loss rate
10- 16 F7.4 10+14cm r1 ? Dust condensation radius
18 A1 --- l_r1/r* [~] Limit flag on r1/r*
19- 23 F5.2 --- r1/r* ? r1 in stellar radii
25 A1 --- l_ue [~] Limit flag on ue
26- 30 F5.2 km/s ue ? Terminal gas outflow velocity
32- 35 F4.2 --- ue/vesc(r1) ? ue in units of escape velocity at r1
37- 40 F4.2 --- (w-u)/ue ? Terminal drift velocity in units of ue
42 A1 --- l_tauV [~] Limit flag on tauV
43- 50 F8.4 --- tauV ? Total optical depth at lambda 0.55 mum
52- 58 F7.4 --- tau10 ? Total optical depth at lambda 10 mum
60- 65 F6.4 --- tauF ? Flux-averaged total optical depth (Eq.25)
67- 72 F6.4 --- Beta ? MassLoss*ue*c/L (3)
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Note (1): the models are:
C1 to C6 models: M= 1, L=1E4, Teff=3000, Astr. silicates, u1=2 km/s (Table2)
D1 to D5 models: M= 4, L=5E4, Teff=2500, Astr. silicates, u1=2 km/s (Table3)
E1 to E5 models: M=10, L=4E5, Teff=2500, Astr. silicates, u1=4 km/s (Table4)
F1 to F4 models: M=30, L=1E4, Teff=2500, Astr. silicates, u1=4 km/s (Table5)
G1 to G6 models: M= 1, L=1E4, Teff=2000, Graphite, u1=2 km/s (Table6)
H1 to H6 models: M= 3, L=5E4, Teff=2000, Graphite, u1=2 km/s (Table7)
I1 to I5 models: M= 5, L=5E4, Teff=2000, Graphite, u1=2 km/s (Table8)
J1 to J6 models: M= 1, L=1E4, Teff=2000, Amorphous carbon, u1=2 km/s(Table9)
K1 to K6 models: M= 3, L=5E4, Teff=2000, Amorphous carbon, u1=2 km/s(Table10)
L1 to L5 models: M= 5, L=5E4, Teff=2000, Amorphous carbon, u1=2 km/s(Table11)
Where M is Mstar (M☉), L is Lstar (L☉) , and
u1 is the initial velocity (gas and dust) at the inner boundary r1.
Note (2): For each mass loss rate, the second row (n_Model = n)
lists the corresponding results from a model calculation ignoring gas
pressure.
Missing data indicate that no steady state solution was found.
Note (3): Beta = Mdot*ue*c/L =
Ratio of momentum flux in the outflow to stellar photon momentum flux
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Acknowledgements: Matthias Steffen
(End) Matthias Steffen [Ast. Inst. Potsdam], Patricia Bauer [CDS] 26-Feb-1997