J/A+A/440/647 New grids of stellar models. II. (Claret, 2005)
New grids of stellar models including tidal-evolution constants up to carbon
burning.
II. From 0.8 to 125M☉: the Small Magellanic Cloud (Z=0.002-0.004).
Claret A.
<Astron. Astrophys. 440, 647 (2005)>
=2005A&A...440..647C 2005A&A...440..647C (SIMBAD/NED BibCode)
ADC_Keywords: Models, evolutionary
Keywords: stars: abundances - stars: rotation - stars: binaries: eclipsing -
stars: rotation
Abstract:
New stellar models spefically designed for the Small Magellanic Cloud
are presented in this paper. In order to take into account the
uncertainties in the metal content we computed two grids with
different metallicities: Z=0.002 and Z=0.004. 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.
We have introduced a recent measurement of the nuclear rate
14N(p,γ)15O. A comparison among models with the old and new
rate was carried out revealed that the former are slightly hotter than
the first ones. Such differences depend on the mass range. The
opacities, the equation of state, the remaining nuclear reactions
rates, the core overshooting parameterization and the convective
transport of energy are the same as discussed previously by us. We
also give, besides the classical evolutionary models outputs, the
internal structure constants needed to investigate apsidal motion and
tidal evolution in close binaries. This aspect acquires importance in
the light of recent investigations on circularization and
synchronization levels in binary systems belonging to the Magellanic
Clouds. The role of rotation can also be investigated through the
gravity-darkening exponents which allow us to compute the brightness
distribution of a given stellar surface.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
grid.dat 39 60 Summary of parameters
z002.dat 500 51404 X=0.754, Z=0.002 models (log(M)=-0.0969 to 2.1000)
z004.dat 500 58966 X=0.748, Z=0.004 models (log(M)=-0.0969 to 2.1000)
x754z002/* . 31 Original tables (1-30) and explanations (README)
x748z004/* . 31 Original tables (31-60) 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/453/769 : New grids of stellar models - III. (Claret, 2006)
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 [0.748,0.754] X initial X composition
7- 11 F5.3 --- Z [0.002,0.004] Z initial composition
13- 19 F7.4 [solMass] logM Initial mass
21 I1 --- Ov [0/1] 1 = with Overshooting
23- 39 A17 --- FileName Original filename with result
(in subdirectory)
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Byte-by-byte Description of file: z002.dat z004.dat
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Bytes Format Units Label Explanations
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1- 7 F7.4 [solMass] logM Initial mass
9 I1 --- Ov [0/1] Overshooting (1)
12- 23 D12.6 yr Age Age of the models
25- 34 F10.6 [solLum] log(L) Log (Total luminosity)
36- 45 F10.6 [cm/s2] log(g) Log (Surface gravity)
47- 56 F10.6 [K] log(Teff) Log (Effective temperature)
58- 67 F10.6 solMass Mass Actual mass of the model
69- 78 F10.6 [solMass/yr] logdM/dt Log (mass loss rate)
80- 89 F10.6 [g/cm3] logDc Log (central density)
91-100 F10.6 [K] logTc Log (central temperature)
102-111 F10.6 --- Qc Core mass (fraction)
113-122 E10.4 --- Xc H central abundance (mass fraction)
124-133 E10.4 --- Xs H surface abundance (mass fraction)
136-145 E10.4 --- Yc 4He central abundance (mass fraction)
147-156 E10.4 --- Ys 4He surface abundance (mass fraction)
158-167 E10.4 --- C12c 12C central abundance (mass fraction)
169-178 E10.4 --- C12s 12C surface abundance (mass fraction)
180-189 E10.4 --- C13c 13C central abundance (mass fraction)
191-200 E10.4 --- C13s 13C surface abundance (mass fraction)
202-211 E10.4 --- N14c 14N central abundance (mass fraction)
213-222 E10.4 --- N14s 14N surface abundance (mass fraction)
224-233 E10.4 --- O16c 16O central abundance (mass fraction)
235-244 E10.4 --- O16s 16O surface abundance (mass fraction)
246-256 E11.4 --- O17c 17O central abundance (mass fraction)
258-267 E10.4 --- O17s 17O surface abundance (mass fraction)
270-279 E10.4 --- O18c 18O central abundance (mass fraction)
281-290 E10.4 --- O18s 18O surface abundance (mass fraction)
292-301 E10.4 --- Ne20c 20Ne central abundance (mass fraction)
303-312 E10.4 --- Ne20s 20Ne surface abundance (mass fraction)
314-323 E10.4 --- Ne22c 22Ne central abundance (mass fraction)
325-334 E10.4 --- Ne22s 22Ne surface abundance (mass fraction)
336-345 E10.4 --- Mg24c 24Mg central abundance (mass fraction)
347-356 E10.4 --- Mg24s 24Mg surface abundance (mass fraction)
358-367 E10.4 --- Mg25c 25Mg central abundance (mass fraction)
369-378 E10.4 --- Mg25s 25Mg surface abundance (mass fraction)
380-389 E10.4 --- Mg26c 26Mg central abundance (mass fraction)
391-400 E10.4 --- Mg26s 26Mg surface abundance (mass fraction)
403-412 F10.6 [---] logK2 Log(Apsidal motion constant (j=2))
414-423 F10.6 [---] logK3 Log(Apsidal motion constant (j=3))
425-434 F10.6 [---] logK4 Log(Apsidal motion constant (j=4))
436-445 F10.6 --- XBF Fractional depth of convective envelope
447-456 F10.6 [---] logE2 Log(Tidal torque constant)
458-468 E11.5 --- ECO Polytropic envelope characteristic
469-478 E10.4 --- alphaP alphaP = -Ep x R/GM2
480-489 F10.6 --- Rgyr Fractional gyration radius
491-500 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, claret(at)iaa.es
(End) Patricia Vannier [CDS] 02-Jun-2005