J/A+A/467/1389 New grids of stellar models. IV. (Claret, 2007)
New grids of stellar models including tidal-evolution constants up to carbon
burning. IV. From 0.8 to 125 M☉: high metallicities (Z=0.04-0.10).
Claret A.
<Astron. Astrophys. 467, 1389 (2007)>
=2007A&A...467.1389C 2007A&A...467.1389C
ADC_Keywords: Models, evolutionary
Keywords: binaries: eclipsing - stars: evolution - stars: abundances -
stars: rotation
Abstract:
The aim of the present grid of stellar models is to complete our
previous calculations and provide a tool for investigating the
astrophysical properties of eclipsing binaries, stellar clusters,
galactic bulges, and elliptical galaxies with a high metal content. To
explore the applicability of high metallic models, we have computed
three grids: (X, Z)=(0.64, 0.04), (0.58, 0.06), and (0.46, 0.10).
For all these grids, we adopted an enrichment law
ΔY/ΔZ=2.0, as in our previous papers on this subject. The
input physics is almost the same as adopted in our earlier work except
for some numerical details, recent measurement of the rate for the
reaction 14N(p,gamma)15O, and the recent mass-loss rate
for the Wolf-Rayet stages. Two high-metallicity clusters, NGC 6253 and
NGC 6791, were used to test the present calculations with very
satisfactory results. On the other hand, as this series of grids was
mainly designed to investigate the tidal evolution of close binaries,
we analyse the present status of circularization times in both
clusters and isolated binaries.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
grid.dat 33 90 Summary of parameters
z04.dat 510 62777 Grid for (X,Z)=(0.640,0.04)
z06.dat 510 59588 Grid for (X,Z)=(0.580,0.06)
z10.dat 510 42191 Grid for (X,Z)=(0.460,0.10)
all/* . 90 Original files
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See also:
J/A+A/453/769 : New grids of stellar models III (Claret, 2006)
J/A+A/440/647 : New grids of stellar models II (Claret, 2005)
J/A+A/424/919 : New grids of stellar models I (Claret, 2004)
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- 7 F7.4 [solMass] logM Initial mass
9- 13 F5.3 --- X [0.460-0.640] X initial X composition (H)
15- 18 F4.2 --- Z [0.04-0.10] Z initial composition
20 I1 --- Ov [0/1] 1=with overshooting
22- 33 A12 --- FileName Original filename with result (in subdirectory)
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Byte-by-byte Description of file: z04.dat z06.dat z10.dat
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Bytes Format Units Label Explanations
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1- 7 F7.4 [solMass] logM Initial mass
9- 13 F5.3 --- X [0.460-0.640] X initial X composition (H)
15- 18 F4.2 --- Z [0.04-0.10] Z initial composition
20 I1 --- Ov [0/1] 1=with overshooting
22- 33 D12.6 yr Age Age of the models
35- 44 F10.6 [solLum] log(L) Log (Total luminosity)
46- 55 F10.6 [cm/s2] log(g) Log (Surface gravity)
57- 66 F10.6 [K] log(Teff) Log (Effective temperature)
68- 77 F10.6 solMass Mass Actual mass of the model
79- 88 F10.6 [solMass/yr] logdM/dt Log (mass loss rate)
90- 99 F10.6 [g/cm3] logDc Log (central density)
101-110 F10.6 [K] logTc Log (central temperature)
112-121 F10.6 --- Qc Core mass (fraction)
123-132 E10.5 --- Xc H central abundance (mass fraction)
134-143 E10.5 --- Xs H surface abundance (mass fraction)
146-155 E10.5 --- Yc 4He central abundance (mass fraction)
157-166 E10.5 --- Ys 4He surface abundance (mass fraction)
168-177 E10.5 --- C12c 12C central abundance (mass fraction)
179-188 E10.5 --- C12s 12C surface abundance (mass fraction)
190-199 E10.5 --- C13c 13C central abundance (mass fraction)
201-210 E10.5 --- C13s 13C surface abundance (mass fraction)
212-221 E10.5 --- N14c 14N central abundance (mass fraction)
223-232 E10.5 --- N14s 14N surface abundance (mass fraction)
234-243 E10.5 --- O16c 16O central abundance (mass fraction)
245-254 E10.5 --- O16s 16O surface abundance (mass fraction)
256-266 E11.5 --- O17c 17O central abundance (mass fraction)
268-278 E11.5 --- O17s 17O surface abundance (mass fraction)
280-289 E10.5 --- O18c 18O central abundance (mass fraction)
291-300 E10.5 --- O18s 18O surface abundance (mass fraction)
302-311 E10.5 --- Ne20c 20Ne central abundance (mass fraction)
313-322 E10.5 --- Ne20s 20Ne surface abundance (mass fraction)
324-333 E10.5 --- Ne22c 22Ne central abundance (mass fraction)
335-344 E10.5 --- Ne22s 22Ne surface abundance (mass fraction)
346-355 E10.5 --- Mg24c 24Mg central abundance (mass fraction)
357-366 E10.5 --- Mg24s 24Mg surface abundance (mass fraction)
368-377 E10.5 --- Mg25c 25Mg central abundance (mass fraction)
379-388 E10.5 --- Mg25s 25Mg surface abundance (mass fraction)
390-399 E10.5 --- Mg26c 26Mg central abundance (mass fraction)
401-410 E10.5 --- 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)
468-477 E10.5 --- ECO Polytropic envelope characteristic
479-488 E10.5 --- alphaP alphaP = -Ep x R/GM2
490-499 F10.6 --- Rgyr Fractional gyration radius
501-510 E10.5 --- beta1 Gravity-darkening exponent
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Acknowledgements:
Antonio Claret dos Santos claret(at)iaa.es
(End) Patricia Vannier [CDS] 12-Mar-2007