VI/118 Stellar Models until He burning (Claret+ 1995-1998)
Stellar Models until He burning, Papers 1-4
Claret A., Gimenez A.
<Astron. Astrophys. Suppl. Ser. 109, 441 (1995);
Astron. Astrophys. Suppl. Ser. 114, 549 (1995);
Astron. Astrophys. Suppl. Ser. 125, 439 (1997);
Astron. Astrophys. Suppl. Ser. 133, 123 (1998)>
=1995A&AS..109..441C 1995A&AS..109..441C
=1995A&AS..114..549C 1995A&AS..114..549C
=1997A&AS..125..439C 1997A&AS..125..439C
=1998A&AS..133..123C 1998A&AS..133..123C
ADC_Keywords: Models, evolutionary
Keywords: stars: binaries: general - evolution - interiors -
fundamental parameters - abundance
Description:
Grids of stellar evolutionary models published in the 4 papers
referenced below are merged here. OPAL opacities with LS coupling and
Grevesse composition were adopted, and Alexander's tables were used
for lower temperatures. The models adopt a core overshooting with
αov=0.20, and mixing length parameter l/Hp=1.52 that seems
to represent well double-lined eclipsing binary stars. Mass loss
during the main sequence and in the red giant phase were taken into
account. The nuclear network treats 14 isotopes and optionally the
lithium burning to study its depletion in less massive models during
pre main sequence evolution.
The initial parameters of the models are summarized in the file
"grids.dat", with metal contents of Z=0.02 (solar), 0.01, 0.03 and
0.004 (Magellanic Clouds), with a wide range of initial hydrogen
content around the solar composition. The mass range covered goes
from 1 (0.6 for the solar composition) up to 40M☉ and the more
massive models were followed until helium burning.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
grid.dat 21 290 Summary of initial parameters
models.dat 108 8673 Evolutionary models
--------------------------------------------------------------------------------
See also:
J/A+A/424/919 : Stellar models grids. Z=0.02, M=0.8 to 125 (Claret, 2004)
J/A+A/440/647 : New grids of stellar models. II. (Claret, 2005)
Byte-by-byte Description of file: grid.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 F5.3 --- X [0.55/0.8] X initial composition (H)
7- 11 F5.3 --- Z [0.004,0.03] Z initial composition
13- 19 F7.4 [solMass] logM ]-0.23/1.6] Initial mass of the model
21 I1 --- Ov [0/1] without (0) or with (1) overshooting
--------------------------------------------------------------------------------
Byte-by-byte Description of file: models.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 I1 --- Pap [1,4] Paper number (1)
3- 7 F5.3 --- X [0.55/0.8] X initial composition (H)
9- 13 F5.3 --- Z [0.004,0.03] Z initial composition
15- 21 F7.4 [solMass] logM ]-0.23/1.6] Initial mass of the model
23 I1 --- Ov [0/1] without (0) or with (1) overshooting
25- 36 E12.6 yr Age Age of models
39- 45 F7.4 [solLum] log(L) Total luminosity
48- 54 F7.4 [cm/s2] log(g) Surface gravity
58- 63 F6.4 [K] log(Teff) Effective temperature
66- 72 F7.4 --- log(k2) Apsidal motion constant (j=2, see paper)
75- 81 F7.4 --- log(k3) Apsidal motion constant (j=3, see paper)
84- 90 F7.4 --- log(k4) Apsidal motion constant (j=4, see paper)
92-101 E10.4 --- alpha alpha = -Ep / (GM2/R)
103-108 F6.4 ---- beta Fractional gyration radius
--------------------------------------------------------------------------------
Note (1): the numbers correspond to the following papers:
1 = Claret A. (1995A&AS..109..441C 1995A&AS..109..441C)
2 = Claret A., Gimenez A. (1995A&AS..114..549C 1995A&AS..114..549C)
3 = Claret A. (1997A&AS..125..439C 1997A&AS..125..439C)
4 = Claret A., Gimenez A. (1998A&AS..133..123C 1998A&AS..133..123C)
--------------------------------------------------------------------------------
History:
Prepared as a merging of the papers 1-4 referenced above.
(End) Francois Ochsenbein [CDS] 15-Sep-2005