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J/A+AS/105/39 Evolutionary sequences V. (Fagotto+ 1994)
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Evolutionary sequences of stellar models with very high metallicity.
V. Z = 0.10
Fagotto F., Bressan A., Bertelli G., Chiosi C.
<Astron. Astrophys. Suppl. Ser. 105, 39 (1994)>
=1994A&AS..105...39F (SIMBAD/NED RefCode)
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ADC_Keywords: Models, evolutionary ;Abundances
Keywords: stars: evolution - stars: interiors
Abstract:
We present detailed tabulations of a large grid of stellar models with
initial chemical compositions [Y=0.475, Z=0.1] computed with the radiative
opacities by Huebner et al. (1977) and convective overshoot. This choice
of the opacity is due to the high metallicity in use, because the Livermore
Library of radiative opacities (Iglesias et al. 1992) did not contain
tabulations for Z=0.1. The tracks span the range of initial masses from
0.6M_{sun}_ to 9M_{sun}_ and extend from the zero age main sequence (ZAMS)
till very advanced evolutionary phases. Specifically, low- and
intermediate-mass stars are followed either till the white dwarf (WD) or
late stages of the early asymptotic giant branch (AGB) phase, depending on
the mass of the star and on details of the evolutionary behaviour discussed
in the text. Massive stars are calculated till core C-ignition. The critical
masses separating low- from intermediate-, and intermediate-mass from
massive stars are M_HeF_=1.3M_{sun}_ andM_up_=4M_{sun}_, respectively. All
the models are calculated at constant mass. The results for all the models
are given in extensive tables which summarize also the lifetimes of the
various phases and the variations of the surface abundances limited to the
first dredge-up. The stellar models presented here are particularly suited
to interpret the CMDs of very metal-rich clusters and the stellar content of
elliptical galaxies. However we warn the reader that, because of the opacity,
these models are not fully homogeneous with the others of the same series by
Bressan et al. (1993) and Fagotto et al. (1994a,b) that are calculated with
the Livermore opacity.
Related Data: Other tables of the series are available as
J/A+AS/100/647 (II: Z = 0.02)
J/A+AS/104/365 (III: Z = 0.0004 and Z = 0.05)
J/A+AS/105/29 (IV: Z = 0.004 and Z = 0.008)
J/A+AS/105/39 (V: Z = 0.10)
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1 161 396 Evolutionary sequences of low mass stars up to
the tip of the RGB, 0.6<M<1.3,
Z=0.10, Y=0.475, Overshoot
table2 160 552 Evolutionary sequences of low mass stars during
the core helium-burning and EAGB phases
0.45<M<1.3, Z=0.10, Y=0.475
table3 161 449 Evolutionary sequences of intermediate stars
up to the TPAGB or carbon-ignition
1.4<M<9.0, Z=0.10, Y=0.475, Overshoot
libro.sty 77 247 Style file to process tables.tex
table1.tex 114 1426 LaTex version of table1
table2.tex 115 2026 LaTex version of table2
table3.tex 114 1657 LaTex version of table3
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Byte-by-byte Description of file: table1, table2, table3
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Bytes Format Units Label Explanations
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1- 6 F6.2 solMass m Initial mass
11- 21 E11.3 yr Age Age of models
25- 31 F7.3 [solLum] log(L) Total luminosity
33- 37 F5.3 [K] log(Teff) Effective temperature
38- 43 F6.3 [cm/s2] log(G) Surface gravity
45- 49 F5.3 [K] log(Tc) Central temperature
53- 57 F5.3 [g/cm3] log(rho_c) Central density
59- 63 F5.3 --- COMP Central abundance (by mass) of hydrogen
or helium
65- 71 E7.2 --- X_C Central abundance of 12C
73- 79 E7.2 --- X_O Central abundance of 16O
81- 86 F6.4 --- Conv Fractionary mass of the convective core
(inclusive of overshoot)
88- 93 F6.4 --- Q_disc Fractionary mass of the first mesh point
where the chemical composition differs
from the surface value
95-100 F6.3 [solLum] log(L_H) Hydrogen luminosity
102-107 F6.4 --- Q1_H Fractionary mass of the inner border of the
hydrogen rich region
109-114 F6.4 --- Q2_H Fractionary mass of the outer border of the
H-burning region. The boundary is taken
where the nuclear energy generation rate
becomes greater than a suitable value
115-120 F6.3 [solLum] log(L_He) Helium luminosity
122-127 F6.4 --- Q1_He Fractionary mass of the inner border of the
He-burning region (when greater than zero
He-burning is in a shell). The boundary is
taken where the nuclear energy generation
rate becomes greater than a suitable value
129-134 F6.4 --- Q2_He Fractionary mass of the upper border of the
He-burning region. The boundary is taken
as above.
136-140 F5.3 [solLum] log(L_C) Carbon luminosity
143-148 F6.3 [solLum] log(L_nu) Neutrinos luminosity (absolute value)
150-155 F6.4 --- Q_Tmax Fractionary mass of the point where the
temperature attains the maximum value
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History:
* 22-Oct-1997: table2 completed with missing models of masses
from 0.7 to 1.3
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(End) Patricia Bauer [CDS] 20-Jan-1994