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J/A+AS/135/405      Grids of stellar models. VIII.           (Charbonnel+ 1999)

Grids of stellar models. VIII. From 0.4 to 1.0 MSun at Z=0.020 and Z=0.001, with the MHD equation of state Charbonnel C., Dappen W., Schaerer D., Bernasconi P.A., Maeder A., Meynet G., Mowlavi N. <Astron. Astrophys. Suppl. Ser. 135, 405 (1999)> =1999A&AS..135..405C
ADC_Keywords: Models, evolutionary; Mass loss; HR diagrams Keywords: stars: evolution - stars: Hertzsprung-Russel diagram - stars: interiors - stars: low-mass Abstract: We present stellar evolutionary models covering the mass range from 0.4 to 1M calculated for metallicities Z=0.020 and 0.001 with the MHD equation of state (Hummer & Mihalas, 1988ApJ...331..794H, Mihalas et al., 1988ApJ...331..815M, Daeppen et al., 1988ApJ...332..261D). A parallel calculation using the OPAL (Rogers et al., 1996ApJ...456..902R) equation of state has been made to demonstrate the adequacy of the MHD equation of state in the range of 1.0 to 0.8M (the lower end of the OPAL tables). Below, down to 0.4M, we have justified the use of the MHD equation of state by theoretical arguments and the findings of Chabrier & Baraffe (1997A&A...327.1039C). We use the radiative opacities by Iglesias & Rogers (1996ApJ...464..943I), completed with the atomic and molecular opacities by Alexander & Fergusson (1994ApJ...437..879A). We follow the evolution from the Hayashi fully convective configuration up to the redgiant tip for the most massive stars, and up to an age of 20Gyr for the less massive ones. We compare our solar-metallicity models with recent models computed by other groups and with observations. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 258 2 M=0.4, Z=0.001, Y=0.243, without overshooting table2.dat 258 3 M=0.5, Z=0.001, Y=0.243, without overshooting table3.dat 258 6 M=0.6, Z=0.001, Y=0.243, without overshooting table4.dat 258 11 M=0.7, Z=0.001, Y=0.243, without overshooting table5.dat 258 51 M=0.8, Z=0.001, Y=0.243, without overshooting table6.dat 258 51 M=0.9, Z=0.001, Y=0.243, without overshooting table7.dat 256 51 M=1.0, Z=0.001, Y=0.243, without overshooting table8.dat 256 3 M=0.4, Z=0.020, Y=0.300, without overshooting table9.dat 256 4 M=0.5, Z=0.020, Y=0.300, without overshooting table10.dat 256 5 M=0.6, Z=0.020, Y=0.300, without overshooting table11.dat 256 11 M=0.7, Z=0.020, Y=0.300, without overshooting table12.dat 256 14 M=0.8, Z=0.020, Y=0.300, without overshooting table13.dat 256 51 M=0.9, Z=0.020, Y=0.300, without overshooting table14.dat 256 51 M=1.0, Z=0.020, Y=0.300, without overshooting table15.dat 256 3 M=0.4, Z=0.020, Y=0.280, without overshooting table16.dat 256 4 M=0.5, Z=0.020, Y=0.280, without overshooting table17.dat 256 5 M=0.6, Z=0.020, Y=0.280, without overshooting table18.dat 256 7 M=0.7, Z=0.020, Y=0.280, without overshooting table19.dat 256 14 M=0.8, Z=0.020, Y=0.280, without overshooting table20.dat 256 51 M=0.9, Z=0.020, Y=0.280, without overshooting table21.dat 256 51 M=1.0, Z=0.020, Y=0.280, without overshooting
See also: J/A+AS/96/269 : Paper I. 0.8 to 120 M, Z=0.020 (Schaller+, 1992) J/A+AS/98/523 : Paper II. 0.8 to 120 M, Z=0.008 (Schaerer+ 1993) J/A+AS/101/415 : Paper III. 0.8 to 120 M, Z=0.004 (Charbonnel+ 1993) J/A+AS/102/339 : Paper IV. 0.8 to 120 M, Z=0.040 (Schaerer+, 1993) J/A+AS/103/97 : Paper V. 12 to 120 M, Z=0.001, 0.004, 0.008, 0.020 0.040 (Meynet+ 1994) J/A+AS/115/339 : Paper VI. HB abd AGB, Z=0.020, 0.001 (Charbonnel+, 1996) J/A+AS/128/471 : Paper VII. 0.8 to 60M, Z=0.10 (Mowlavi+ 1998) Byte-by-byte Description of file: table*.dat
Bytes Format Units Label Explanations
1- 2 I2 --- No Number of selected point 4- 17 E14.7 yr Age Age 18- 25 F8.4 solMass Mass Actual mass 27- 32 F6.3 [solLum] log(L) log(luminosity) 34- 38 F5.3 [K] log(Te) log(effective temperature) 40- 47 F8.6 --- Hs H surface abundance (mass fraction) 49- 56 F8.6 --- Hes He surface abundance (mass fraction) 58- 65 F8.6 --- C12 12C surface abundance (mass fraction) 67- 74 F8.6 --- C13 13C surface abundance (mass fraction) 76- 83 F8.6 --- N14 14N surface abundance (mass fraction) 85- 92 F8.6 --- O16 16O surface abundance (mass fraction) 94-101 F8.6 --- O17 17O surface abundance (mass fraction) 103-110 F8.6 --- O18 18O surface abundance (mass fraction) 112-119 F8.6 --- Ne20 20Ne surface abundance (mass fraction) 121-128 F8.6 --- Ne22 22Ne surface abundance (mass fraction) 130-136 F7.5 --- QCC Core mass fraction 143-149 F7.3 [Msun/yr] log(Mdot) log(mass loss rate) 152-156 F5.3 [g/cm3] rhoc log(central density) 158-162 F5.3 [K] log(Tc) log(central temperature) 164-171 F8.6 --- Hc H central abundance (mass fraction) 173-180 F8.6 --- Hec He central abundance (mass fraction) 182-189 F8.6 --- C12c 12C central abundance (mass fraction) 191-198 F8.6 --- C13c 13C central abundance (mass fraction) 200-207 F8.6 --- N14c 14N central abundance (mass fraction) 209-216 F8.6 --- O16c 16O central abundance (mass fraction) 218-225 F8.6 --- O17c 17O central abundance (mass fraction) 227-234 F8.6 --- O18c 18O central abundance (mass fraction) 236-243 F8.6 --- Ne20c 20Ne central abundance (mass fraction) 245-252 F8.6 --- Ne22c 22Ne central abundance (mass fraction)
Acknowledgements: Corinne Charbonnel History: Pre-main sequence tracks can be asked to
(End) Patricia Bauer [CDS] 14-Dec-1998
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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