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J/A+AS/104/365 Evolutionary sequences. III. (Fagotto+ 1994)
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Evolutionary sequences of stellar models with new radiative opacities.
III. Z = 0.0004 and Z=0.05
Fagotto F., Bressan A., Bertelli G., Chiosi C.
<Astron. Astrophys. Suppl. Ser. 104, 365 (1994)>
=1994A&AS..104..365F (SIMBAD/NED References)
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ADC_Keywords: Models, evolutionary; HR diagrams; Abundances
Keywords: stars: evolution - stars: interiors -
stars: Hetzsprung-Russell diagram - stars: abundances
Abstract:
We present detailed tabulations of two large grids of stellar models with
the extreme initial chemical composition [Z=0.0004, Y=0.230], and [Z=0.050,
Y=0.352]. The models are computed with the most recent radiative opacities
(OPAL) by Iglesias et al. (1992) and with the inclusion of overshoot from
convective cores and envelopes according to the formalism by Bressan et al.
(1981) and Alongi et al. (1991), respectively, and the revision made by
Bressan et al. (1993a). These calculations represent the continuation of the
series initiated with the paper by Bressan et al. (1993a) for the grid with
[Z=0.020, Y=0.280] (the reference solar like abundance). The tracks are
calculated for a wide range of initial masses from 0.6 M_{sun}_ to 120
M_{sun} _ and extend from the ZAMS till very advanced evolutionary phases.
Specifically, low and intermediate mass stars are followed to the beginning
of the 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 winds incorporating a suitable dependence on the metallicity.
The results of all the models are given in extensive tables which summarize
also the lifetimes of the various phases and the variations of 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, with particular attention to the anomalous behaviour
of the low mass, high metallicity stars in core He-burning and later phases.
Such grids of evolutionary tracks are well indicated for studies of
population synthesis in virtue of their large coverage of masses,
evolutionary phases, and chemical composition. The high metallicity set is
particularly suited to interpret the stellar content of bulges and
elliptical galaxies.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1a 156 531 Evolutionary sequences of low mass stars up to
the tip of the RGB. 0.6 < M < 1.7 for z=0.0004
table1b 155 560 Evolutionary sequences of low mass stars up to
the tip of the RGB. 0.6 < M < 1.7 for z=0.05
table2a 155 422 Evolutionary sequences of low mass stars during
the core helium-burning and EAGB phases.
0.5 < M < 1.7 for z=0.0004
table2b 155 537 Evolutionary sequences of low mass stars during
the core helium-burning and EAGB phases.
0.5 < M < 1.7 for z=0.05
table3a 155 507 Evolutionary sequences of intermediate stars up
to the TPAGB or carbon-ignition.
1.8 < M < 9.0 for z=0.0004
table3b 155 408 Evolutionary sequences of intermediate stars up
to the TPAGB or carbon-ignition.
1.8 < M < 9.0 for z=0.05
table4a 166 392 Evolutionary sequences for massive stars.
12 < M < 120 for z=0.0004
table4b 166 324 Evolutionary sequences for massive stars.
12 < M < 120 for z=0.05
tabz0004.tex 123 7304 LaTex version of the tables for z=0.0004
tabz05.tex 123 7377 LaTex version of the tables for z=0.05
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Byte-by-byte Description of file: table1a
Byte-by-byte Description of file: table1b
Byte-by-byte Description of file: table2a
Byte-by-byte Description of file: table2b
Byte-by-byte Description of file: table3a
Byte-by-byte Description of file: table3b
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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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Byte-by-byte Description of file: table4a
Byte-by-byte Description of file: table4b
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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 solMass M Current value of the mass
33- 37 F5.3 [solLum] 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 [solLum] 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 [solLum] log(L_He) Helium luminosity
120-126 F7.3 [solMass/yr] log(M_dot) Absolute value of the mass loss rate
128-134 E7.2 --- X_sur Surface abundance (by mass) of 1 H
136-142 E7.2 --- Y_sur Surface abundance (by mass) of 4 He
144-150 E7.2 --- XC_sur Surface abundance (by mass) of 12 C
152-158 E7.2 --- XN_sur Surface abundance (by mass) of 14 N
160-166 E7.2 --- XO_sur Surface abundance (by mass) of 16 O
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(End) Patricia Bauer [CDS] 13-Dec-1993