J/A+AS/106/275 Theoretical isochrones (Bertelli+ 1994)
Theoretical isochrones from models with new radiative opacities
Bertelli G., Bressan A., Chiosi C., Fagotto F., Nasi E,
<Astron. Astrophys. Suppl. Ser. 106, 275 (1994)>
=1994A+AS..106..275B 1994A+AS..106..275B (SIMBAD/NED Reference)
ADC_Keywords: Models, evolutionary; HR diagrams
Keywords: stars: evolution, interiors, fundamental parameters, HR diagram
Abstract:
In this paper we present large grids of theoretical isochrones for the
initial chemical compositions [Z=0.0004, Y=0.23], [Z=0.004, Y=0.24],
[Z=0.008, Y=0.25], [Z=0.02, Y=0.28], and [Z= 0.05, Y=0.352] and ages
in the range 4Myr to 16Gyr. These isochrones are derived from stellar
models computed with the most recent radiative opacities by Iglesias
et al. (1992). In addition to this we present another set with
chemical composition [Z=0.001, Y=0.23] based on models calculated with
the radiative opacities by Huebner et al. (1977). All the stellar
models are followed from the zero age main sequence (ZAMS) to the
central carbon ignition for massive stars or to the beginning of the
thermally pulsing regime of the asymptotic giant branch phase (TP-AGB)
for low and intermediate mass stars.
For each isochrone, we give the current mass, effective temperatures,
bolometric and visual magnitudes, (U-B), (B-V), (V-R), (V-I), (V-J),
(V-H), and (V-K) colors, and the luminosity function for the case of
the Salpeter law. In addition to this, integrated magnitudes and
colors at several characteristic points are also presented together
with the mass of the remnant star when appropriate. The main
characteristic that makes this set of isochrones very valuable is
based on their extension in mass and chemical composition, besides the
calculation of late stages of evolution, beyond the red giant tip till
the white dwarf stage after the planetary nebula phase.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1 106 6369 Model for z=0.0004, Y=0.23
table2 106 5954 Model for z=0.0010, Y=0.23
table3 106 6634 Model for z=0.0040, Y=0.24
table4 106 6709 Model for z=0.0080, Y=0.25
table5 106 6608 Model for z=0.0200, Y=0.28
table6 106 6474 Model for z=0.0500, Y=0.352
z0004.pst 80 8637 Postscript files of table1 ready to print
z001.pst 80 8038 Postscript files of table2 ready to print
z004.pst 80 8844 Postscript files of table3 ready to print
z008.pst 80 8955 Postscript files of table4 ready to print
z02.pst 80 8865 Postscript files of table5 ready to print
z05.pst 80 8625 Postscript files of table6 ready to print
--------------------------------------------------------------------------------
Byte-per-byte Description of file: table*
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
3- 8 F6.3 [yr] log(Age) Logarithm of the age
11- 17 F7.4 solMass M Current mass (1)
20- 24 F5.3 [K] log(Teff) Logarithm of effective temperature
26- 31 F6.2 mag Mbol Bolometric magnitude
33- 38 F6.2 mag V Absolute visual magnitude
41- 45 F5.2 mag (U-B) (U-B) color index
48- 52 F5.2 mag (B-V) (B-V) color index
55- 59 F5.2 mag (V-R) (V-R) color index
62- 66 F5.2 mag (V-I) (V-I) color index
69- 73 F5.2 mag (V-J) (V-J) color index
76- 80 F5.2 mag (V-H) (V-H) color index
83- 87 F5.2 mag (V-K) (V-K) color index
89- 99 F11.8 --- FLUM Luminosity function for the case of the
Salpeter law
102-106 F5.2 solMass Mwind Real value of the mass after mass loss by
stellar wind for massive stars (2)
--------------------------------------------------------------------------------
Note (1):
The current mass is usually increasing along the isochrone, but in the
transition from the tip of the RGB to the ZAHB and from the tip of the
AGB to the P-AGB phase. The mass is decreased in these transitions
according to the effects of mass loss during the RGB phase, and the
TP-AGB phase as described in section 3.
Note (2):
For massive stars the actual value of the mass is not given by the
current mass along the isochrone, but it is derived taking into
account mass loss by stellar wind as pointed out in section 2.2
of the text.
Of course, for low and intermediate mass stars Mwind is not printed in
the postscript files, and its value is defined as zero in table* files.
Only in the youngest isochrones, when massive stars are involved and
mass loss by stellar wind is taken into account, the value of Mwind
represents the actual mass associated to the corresponding luminosity
and effective temperature.
--------------------------------------------------------------------------------
References:
Iglesias, C.A., Rogers, F.J., Wilson B.G. =1992ApJ...397..717I 1992ApJ...397..717I
Huebner, W.F., Merts, A.L., Magee, N.H., Argo, M.F., 1977,
Los Alamos Sci. Lab. Rep. LA-6760-M
(End) Patricia Bauer [CDS] 21-Mar-1994