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

Grids of stellar models. VIII. From 0.4 to 1.0 M_{Sun}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..405CADC_Keywords: Models, evolutionary; Mass loss; HR diagramsKeywords: stars: evolution - stars: Hertzsprung-Russel diagram - stars: interiors - stars: low-massAbstract: 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^{12}C surface abundance (mass fraction) 67- 74 F8.6 --- C13^{13}C surface abundance (mass fraction) 76- 83 F8.6 --- N14^{14}N surface abundance (mass fraction) 85- 92 F8.6 --- O16^{16}O surface abundance (mass fraction) 94-101 F8.6 --- O17^{17}O surface abundance (mass fraction) 103-110 F8.6 --- O18^{18}O surface abundance (mass fraction) 112-119 F8.6 --- Ne20^{20}Ne surface abundance (mass fraction) 121-128 F8.6 --- Ne22^{22}Ne 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^{12}C central abundance (mass fraction) 191-198 F8.6 --- C13c^{13}C central abundance (mass fraction) 200-207 F8.6 --- N14c^{14}N central abundance (mass fraction) 209-216 F8.6 --- O16c^{16}O central abundance (mass fraction) 218-225 F8.6 --- O17c^{17}O central abundance (mass fraction) 227-234 F8.6 --- O18c^{18}O central abundance (mass fraction) 236-243 F8.6 --- Ne20c^{20}Ne central abundance (mass fraction) 245-252 F8.6 --- Ne22c^{22}Ne central abundance (mass fraction)

Acknowledgements: Corinne CharbonnelHistory: Pre-main sequence tracks can be asked to(End)Patricia Bauer [CDS] 14-Dec-1998

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