J/A+A/424/919 Stellar models grids. Z=0.02, M=0.8 to 125 (Claret, 2004)
New grids of stellar models including tidal-evolution constants up to carbon
burning. I. From 0.8 to 125M☉ at Z=0.02.
Claret A.
<Astron. Astrophys. 424, 919 (2004)>
=2004A&A...424..919C 2004A&A...424..919C
ADC_Keywords: Models, evolutionary
Keywords: binaries: close - stars: evolution - stars: interiors -
stars: fundamental parameters - stars: abundances - stars: rotation
Abstract:
We present new stellar models based on updated physics (opacities,
expanded nuclear network and mass loss rates). We compute stellar
models suitable for the mean solar neighborhood, i.e. for Z=0.02 and
X=0.70. The covered mass range is from 0.8 up to 125M☉ and the
models are followed until the exhaustion of carbon in the core, for
the more massive ones. In addition, the effective temperatures of the
more massive models are corrected for the effects of stellar winds,
while models with lower effective temperatures are computed using a
special treatment of the equation of state (CEFF). Convective core
overshooting is assumed to be moderate and is modelled with
alphaov=0.20. Besides the classical ingredients of stellar models,
we also provide the internal structure constants needed to investigate
apsidal motion and tidal evolution in close binaries. The latter
constants are made public for the first time. According to the current
theories of tidal evolution, the time scales for synchronization and
circularization for cool stars depend -- apart from the mass, radius
and effective temperature -- on the depth of the convective envelope
xbf and on the radius of gyration β. For stars with higher
effective temperatures, these dependencies are mainly incorporated in
the tidal torque constant E2. All these parameters are steep
functions of mass and time, and thus require a special numerical
treatment. The new mass loss formalism produces more mass concentrated
configurations than previously, especially for more massive and more
evolved stellar models. As the present grid is designed mainly for the
study of double-lined eclipsing binaries, the gravity-darkening
exponents necessary to calculate the surface brightness distribution
in rotationally and/or tidally distorted stars are computed following
the method described recently by Claret (1998, Cat. J/A+AS/133/123),
and made available for each point of every evolutionary track.
Description:
The influence of the recent measurement of the nuclear reaction
14N(P,GAMMA)15O will be analysed and added to the present
calculations.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
grid.dat 37 30 Summary of parameters
tables.dat 644 60744 All models with Z=0.02, X=0.70, M=0.8 to 125M☉
x70z02/* . 31 Original tables (30) and explanations (README)
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See also:
J/A+A/424/919 : New grids of stellar models - I. (Claret, 2004)
J/A+A/440/647 : New grids of stellar models - II. (Claret, 2005)
J/A+A/467/1389 : New grids of stellar models - IV. (Claret, 2007)
J/A+AS/109/441 : Stellar models until He burning - I. (Claret, 1995)
J/A+AS/114/549 : Stellar models until He burning - II. (Claret+, 1995)
J/A+AS/125/439 : Stellar models until He burning - III. (Claret+, 1997)
J/A+AS/133/123 : Stellar models until He burning - IV. (Claret+ 1998)
Byte-by-byte Description of file: grid.dat
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Bytes Format Units Label Explanations
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1- 5 F5.3 --- X [0.70] X initial X composition
7- 11 F5.3 --- Z [0.02] Z initial composition
13- 19 F7.4 [solMass] logM Initial mass
21 I1 --- Ov [0/1] 1 = with Overshooting
23- 37 A15 --- FileName Original filename with result
(in subdirectory)
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Byte-by-byte Description of file: tables.dat
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Bytes Format Units Label Explanations
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1- 7 F7.4 [solMass] logM Initial mass
9- 12 F4.2 --- X [0.70] X initial X composition (H)
14- 17 F4.2 --- Z [0.02] Z initial composition
19 I1 --- Ov [0/1] Overshooting (1)
21- 32 D12.6 yr Age Age of the models
34- 43 F10.6 [solLum] log(L) Log (Total luminosity)
45- 54 F10.6 [cm/s2] log(g) Log (Surface gravity)
56- 65 F10.6 [K] log(Teff) Log (Effective temperature)
67- 76 F10.6 solMass Mass Actual mass of the model
78- 87 F10.6 [solMass/yr] logdM/dt Log (mass loss rate)
89- 98 F10.6 [g/cm3] logDc Log (central density)
100-109 F10.6 [K] logTc Log (central temperature)
111-120 F10.6 --- Qc Core mass (fraction)
122-131 E10.4 --- Xc H central abundance (mass fraction)
133-142 E10.4 --- Xs H surface abundance (mass fraction)
145-154 E10.4 --- Yc 4He central abundance (mass fraction)
156-165 E10.4 --- Ys 4He surface abundance (mass fraction)
167-176 E10.4 --- C12c 12C central abundance (mass fraction)
178-187 E10.4 --- C12s 12C surface abundance (mass fraction)
189-198 E10.4 --- C13c 13C central abundance (mass fraction)
200-209 E10.4 --- C13s 13C surface abundance (mass fraction)
211-220 E10.4 --- N14c 14N central abundance (mass fraction)
222-231 E10.4 --- N14s 14N surface abundance (mass fraction)
233-242 E10.4 --- O16c 16O central abundance (mass fraction)
244-253 E10.4 --- O16s 16O surface abundance (mass fraction)
255-265 E11.4 --- O17c 17O central abundance (mass fraction)
267-277 E11.4 --- O17s 17O surface abundance (mass fraction)
280-289 E10.4 --- O18c 18O central abundance (mass fraction)
291-300 E10.4 --- O18s 18O surface abundance (mass fraction)
302-311 E10.4 --- Ne20c 20Ne central abundance (mass fraction)
313-322 E10.4 --- Ne20s 20Ne surface abundance (mass fraction)
324-333 E10.4 --- Ne22c 22Ne central abundance (mass fraction)
335-344 E10.4 --- Ne22s 22Ne surface abundance (mass fraction)
346-355 E10.4 --- Mg24c 24Mg central abundance (mass fraction)
357-366 E10.4 --- Mg24s 24Mg surface abundance (mass fraction)
368-377 E10.4 --- Mg25c 25Mg central abundance (mass fraction)
379-388 E10.4 --- Mg25s 25Mg surface abundance (mass fraction)
390-399 E10.4 --- Mg26c 26Mg central abundance (mass fraction)
401-410 E10.4 --- Mg26s 26Mg surface abundance (mass fraction)
413-422 F10.6 [---] logK2 Log(Apsidal motion constant (j=2))
424-433 F10.6 [---] logK3 Log(Apsidal motion constant (j=3))
435-444 F10.6 [---] logK4 Log(Apsidal motion constant (j=4))
446-455 F10.6 --- XBF Fractional depth of convective envelope
457-466 F10.6 [---] logE2 Log(Tidal torque constant)
468-478 E11.5 --- ECO Polytropic envelope characteristic
480-489 E10.4 --- alphaP αP = -Ep x R/GM2
491-500 F10.6 --- Rgyr Fractional gyration radius
502-511 E10.4 --- beta1 Gravity-darkening exponent
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Note (1): Overshooting:
0: without overshooting,
1: with overshooting
For all models, alpha = 1.680
For models with overshooting, alphaOV= 0.200
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Acknowledgements: Antonio Claret Dos Santos
(End) Patricia Vannier [CDS] 17-Jun-2004