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J/A+AS/105/29 Evolutionary sequences IV. (Fagotto+ 1994)
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Evolutionary sequences of stellar models with new radiative opacities.
IV. Z = 0.004 and Z=0.008
Fagotto F., Bressan A., Bertelli G., Chiosi C.
<Astron. Astrophys. Suppl. Ser. 105, 29 (1994)>
=1994A&AS..105...29F
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ADC_Keywords: Models, evolutionary
Keywords: stars: evolution - stars: interiors
Abstract:
We present detailed tabulations of two large grids of stellar models with
the initial chemical compositions [Y=0.240, Z=0.004] and [Y=0.250, Z=0.008],
computed with the most recent radiative opacities (OPAL) by Iglesias et al.
(1992). This paper continues the series initiated by Bressan et al. (1993)
for the grid with [Y=0.280, Z=0.020], the reference solar like abundances,
followed by Fagotto et al. (1994a) for the grids with compositions [Y=0.230,
Z=0.0004] and [Y=0.352, Z=0.05]. The tracks span a wide range of initial
masses from 0.6M_{sun}_ to 120M_{sun}_ and extend from the zero age main
sequence (ZAMS) till very advanced evolutionary phases. Specifically, low-
and intermediate-mass stars are followed till the beginning of the thermally
pulsing regime of the asymptotic giant branch phase (TP-AGB), while massive
stars are followed till the core C-ignition. The models of low- and
intermediate-mass stars are calculated at constant mass, whereas
those of massive stars are followed in presence of mass loss by stellar
wind incorporating a suitable dependence on the metallicity. 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
by dredge-up phenomena and mass loss by stellar wind. The salient features
brought by the different metallicity and helium content are briefly
outlined. In virtue of their large coverage of masses, evolutionary phases,
and chemical compositions, such grids of evolutionary tracks are basic to
studies of population synthesis. In particular they are suited to interpret
the CMDs of metal-rich globular clusters and of the typical stellar content
of the Large Magellanic Cloud.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1a.dat 155 502 Evolutionary sequences of low mass stars up to
the tip of the RGB. 0.6 < M < 1.8 for z=0.004
table1b.dat 155 437 Evolutionary sequences of low mass stars up to
the tip of the RGB. 0.6 < M < 1.8 for z=0.008
table2a.dat 155 352 Evolutionary sequences of low mass stars during
the core-helium burning and EAGB phases.
0.5 < M < 1.8 for z=0.004
table2b.dat 155 404 Evolutionary sequences of low mass stars during
the core-helium burning and the EAGB phases.
0.5 < M < 1.8 for z=0.008
table3a.dat 155 461 Evolutionary sequences of intermediate stars up
to the TPAGB or carbon-ignition.
1.9 < M < 9.0 for z=0.004
table3b.dat 155 419 Evolutionary sequences of intermediate stars up
to the TPAGB or carbon-ignition.
2.0 < M < 9.0 for z=0.008
table4a.dat 185 419 Evolutionary sequences for massive stars.
12 < M < 120 for z=0.004
table4b.dat 180 403 Evolutionary sequences for massive stars.
12 < M < 120 for z=0.008
libro.sty 77 247 Style file for table*.tex
table1.tex 114 3830 Latex version of table1(a,b)
table2.tex 114 3174 Latex version of table2(a,b)
table3.tex 114 3512 Latex version of table3(a,b)
table4.tex 123 3125 Latex version of table4(a,b)
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See also:
J/A+AS/100/647 : Evolutionary Sequences II. (Bressan+ 1993)
J/A+AS/104/365 : Evolutionary sequences. III. (Fagotto+ 1994)
J/A+AS/105/39 : Evolutionary sequences V. (Fagotto+ 1994)
Byte-by-byte Description of file: table1a.dat
Byte-by-byte Description of file: table1b.dat
Byte-by-byte Description of file: table2a.dat
Byte-by-byte Description of file: table2b.dat
Byte-by-byte Description of file: table3a.dat
Byte-by-byte Description of file: table3b.dat
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Bytes Format Units Label Explanations
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1- 6 F6.2 Sun m Initial mass
11- 21 E11.3 yr Age Age of models
25- 31 F7.3 Sun 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 Sun 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 Sun 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 Sun log(L_C) Carbon luminosity
143-148 F6.3 Sun 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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Byte-by-byte Description of file: table4a.dat
Byte-by-byte Description of file: table4b.dat
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Bytes Format Units Label Explanations
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1- 6 F6.2 Sun m Initial mass
11- 21 E11.3 yr Age Age of models
25- 31 F7.3 Sun M Current value of the mass
33- 37 F5.3 Sun log(L) Total luminosity
39- 43 F5.3 K log(Teff) Effective temperature
44- 49 F6.3 cm/s2 log(G) Surface gravity
53- 57 F5.3 K log(Tc) Central temperature
59- 63 F5.3 g/cm3 log(rho_c) Central density
65- 71 E7.2 --- COMP Central abundance of hydrogen or helium
by mass
73- 79 E7.2 --- X_C Central abundance of 12C
81- 87 E7.2 --- X_O Central abundance of 16O
89- 94 F6.4 --- Conv Fractionary mass of the convective core
(inclusive of overshoot)
96-101 F6.4 --- Q_disc Fractionary mass of the first mesh point
where the chemical composition differs
from the surface value
103-108 F6.4 Sun log(L_H) Hydrogen luminosity
109-113 F5.3 --- Q1_H Fractionary mass of the inner border of the
hydrogen rich region
115-119 F5.3 Sun log(L_He) Helium luminosity
120-126 F7.3 Sun/yr log(M_dot) Absolute value of the mass loss rate
128-134 E7.2 --- X_sur Surface abundance by mass of 1H
136-142 E7.2 --- Y_sur Surface abundance by mass of 4He
144-150 E7.2 --- XC_sur Surface abundance by mass of 12C
152-158 E7.2 --- XN_sur Surface abundance by mass of 14N
160-166 E7.2 --- XO_sur Surface abundance by mass of 16O
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(End) Patricia Bauer [CDS] 21-Jan-1994