The Pisa Evolutionary Library This directory contains the evolutionary tracks and the isochrones for Population II stars presented in the papers: V. Castellani, S. Degl'Innocenti, M. Marconi. P.G. Prada Moroni, P. Sestito "Stellar evolutionary models for Magellanic Clouds" A&A 404, 645 P. Cariulo, V. Castellani, S. Degl'Innocenti "Stellar evolutionary models of Population II stars" submitted to Astronomy and Astrophysics. =============================================================== Magellanic Clouds Models The models are calculated for different chemical compositions both without overshooting (standard models, including microscopic diffusion of He and heavy elements) and with different overshooting efficiency. Each set of models can be found in a different sub-directory. It is possible to get all the content for each chemical composition, the content of each selected sub-directory or just a given file. In each directory there are evolutionary tracks (TRACKS), isochrones (ISOCHRONES), horizontal branch models together with a table of the ZAHB characteristics (HB) and files with some relevant physical values of selected models (STRUCTURES). Models with overshooting are calculated for masses higher than 1 Mo to avoid the unobserved presence of the overall contraction feature in 1Mo stars. Thus isochrones for ages higher than about 5 Gyr are the same as in the standard case and thus are not included in the overshooting directories. Models with overshooting does not include microscopic diffusion because for masses higher than about 1Mo the effect of this mechanism is almost negligible. All the tracks and isochrones have been transformed in the observation plane by adopting the model atmospheres by Castelli (1999), see also Castelli, Gratton & Kurucz (1997). =================================================================================================== CONTENTS 1) Z=0.004 Y=0.238 diffusion ml=1.9 standard tracks up to the TO tracks from MS to AGB isochrones structure HB (0.9 Mo progenitor) (0.6-0.7) Mo (0.8-11.0) Mo (100 Myr-12.9 Gyr) 0.9, 2.0, 4.0 Mo HB masses from 0.52 to 0.9 Mo 2) Z=0.004 Y=0.270 diffusion ml=1.9 standard tracks up to the TO tracks from MS to AGB isochrones structure HB (0.8 Mo progenitor) (0.6-0.7) Mo (0.8-8.0) Mo (100 Myr-13Gyr) 0.9, 2.0, 4.0 Mo HB masses from 0.53 to 0.8 Mo 3) Z=0.004 Y=0.238 no diffusion ml=1.9 overshooting 0.25 Hp tracks from MS to AGB isochrones structure (1.2-9.0) Mo (100 Myr-5 Gyr) 2.0, 4.0 Mo 4) Z=0.008 Y=0.250 diffusion ml=1.9 standard tracks up to the TO tracks from MS to AGB isochrones structure HB (0.9 Mo progenitor) (0.6-0.7) Mo (0.8-7.0) Mo (100 Myr-12Gyr) 0.9, 2.0, 4.0 Mo HB masses from 0.53 to 0.9 Mo 5) Z=0.008 Y=0.250 no diffusion ml=1.9 overshooting 0.10 Hp tracks from MS to AGB isochrones structure (1.2-7.0) Mo (100 Myr-5 Gyr) 2.0, 4.0 Mo 6) Z=0.008 Y=0.250 no diffusion ml=1.9 overshooting 0.25 Hp tracks from MS to AGB isochrones structure (1.2-7.0) Mo (100 Myr-5Gyr) 2.0, 4.0 Mo ================================================================================== Population II Models The models are calculated for different chemical compositions suitable to cover with a fine grid the range for Pop.II stars. Models include microscopic diffusion of He and heavy elements. Each set of models can be found in a different sub-directory. It is possible to get all the content for each chemical composition, the content of each selected sub-directory or just a given file. In each directory there are evolutionary tracks (TRACKS), isochrones (ISOCHRONES), horizontal branch models together with a table of the ZAHB characteristics (HB) and files with some relevant physical values of selected models (STRUCTURES). For Z=0.001 models are caluculated for two different values of the mixing lenght parameter:ml=2.0, ml=2.3. All the tracks and isochrones have been transformed in the observation plane by adopting the model atmospheres by Castelli (1999), see also Castelli, Gratton & Kurucz (1997). =================================================================================================== CONTENTS 1) Z=0.0002 Y=0.230 ml=2.0 tracks up to the He flash tracks from MS to AGB isochrones structures HB (0.8 Mo progenitor) (0.6 Mo (0.8-11.0) Mo (20 Myr-20 Gyr) 0.9, 2.0, 4.0 Mo HB masses from 0.53 to 0.8 Mo 2) Z=0.0004 Y=0.230 ml=2.0 tracks up to the He flash tracks from MS to AGB isochrones structure HB (0.8 Mo progenitor) 0.6 Mo (0.7-11.0) Mo (20 Myr-20Gyr) 0.9, 2.0, 4.0 Mo HB masses from 0.54 to 0.8 Mo 3) Z=0.0006 Y=0.230 ml=2.0 tracks up to the TO tracks from MS to AGB isochrones structure HB (0.8 Mo progenitor) 0.6 Mo (0.7-11.0) Mo (20 Myr-20Gyr) 0.9, 2.0, 4.0 Mo HB masses from 0.52 to 0.8 Mo 4) Z=0.001 Y=0.232 ml=2.3 tracks up to the TO tracks from MS to AGB isochrones structure HB (0.8 Mo progenitor) 0.6 Mo (0.7-11.0) Mo (20 Myr-20Gyr) 0.9, 2.0, 4.0 Mo HB masses from 0.53 to 0.8 Mo 5) Z=0.001 Y=0.232 ml=2.0 tracks up to the TO tracks from MS to AGB isochrones structure HB (0.8 Mo progenitor) 0.6 Mo (0.7-11.0) Mo (100 Myr-21Gyr) 0.9, 2.0, 4.0 Mo HB masses from 0.53 to 0.8 Mo =============================================================================================== TRACKS The name of the evolutionary tracks is as follows: MASSm1m2.m3m4Zz1Ez2Yy1y2y3.AAAAAA example:MASS0.6z4E3y238.std 1) The numbers m1m2.m3m4 provide informations about the stellar mass: example: MASS0.85 --> 0.85Mo, MASS10.0 --> 10 Mo 2) z1Ez2 indicates the metallicity: z1Ez2 ---> z1*10**(-z2) 4E3 ---> Z= 0.004 3) y1y2y3 indicates the initial He abundance: y1y2y3 ---> Y=0.y1y2y3 examples: Y238 ---> Y=0.238 4) AAAAAA is STD for standard models and ov0pAAA for tracks with a given amount of overshooting examples: ov0p25 ---> overshooting with l_ov=0.25 Hp 5) For the models most massive than 0.7 Mo the He burning phases up to the thermal pulses or to the carbon ignition have been included. Mass loss has not be taken into account. Each file shows, from left to right: 1) the logarithm of the age (in year) 2) the mass in solar units 3) the logarithm of the luminosity 4) the logarithm of the effective temperature 5) the absolute visual magnitude 6) the B-V color 7) the U-B color 8) the V-I color 9) the V-R color 10) the R-I color =================================================================================================== HB Evolutionary tracks for HB models: HBm1.m2m3z1Ez2yy1y2y3.std example: HB0.58z4E3y238.std 1) The files contains the He burning evolutionary tracks for HB stars until the onset of the thermal pulses 2) The numbers m1.m2m3 provides informations about the HB stellar mass: example: 0.65 --> 0.65Mo 3) The numbers z1Ez_2indicate the metallicity: examples: 4E3 ---> Z=4.0E-3 4) yy1y2y3 indicates the initial He abundance: y1y2y3 ---> Y=0.y_1y_2y_3 examples: Y232 ---> Y=0.232, Y340 ---> Y=0.340 The content of the various columns is the following: 1) the logarithm of the age (in year) 2) the mass in solar units 3) the logarithm of the luminosity 4) the logarithm of the effective temperature 5) the absolute visual magnitude 6) the B-V color 7) the U-B color 8) the V-I color 9) the V-R color 10) the R-I color ==================================================================================================== ISOCHRONES AGEa1.a2zz1Ez2yy1y2y3.AAA example: AGE0.1z4E3y238.std 1) The isochrones include the evolutionary phases from the MS to the AGB 2) The numbers a1.a2 indicates the age in Gyr: AGE0.1 --> 0.1 Gyr 3) The term zz1Ez2 indicates the metallicity: 4E3 ---> Z=4.0E-3 4) yy1y2y3 indicates the initial He abundance: y1y2y3 ---> Y=0.y_1y_2y_3 examples: Y232 ---> Y=0.232, Y340 ---> Y=0.340 5) AAAAAA is STD for standard models and ov0pAAA for tracks with a given amount of overshooting examples: ov0p25 ---> overshooting with l_ov=0.25 Hp Each file shows, from left to right: 1) the mass in solar units 2) the logarithm of the luminosity 3) the logarithm of the effective temperature 4) the absolute visual magnitude 5) the B-V color 6) the U-B color 7) the V-I color 8) the V-R color 9) the R-I color ==================================================================================================== STRUCTURES STRm1pm2Zz1Ez2Yy1y2y3.AAA example: STR0p9Z4E3Y238.STD 1) The numbers m1pm2 provides informations about the HB stellar mass: example: 0p9 --> 0.9 Mo 2) The term zz1Ez2 indicates the metallicity: 4E3 ---> Z=4.0E-3 3) yy1y2y3 indicates the initial He abundance: y1y2y3 ---> Y=0.y_1y_2y_3 examples: Y232 ---> Y=0.232, Y340 ---> Y=0.340 4) AAAAAA is STD for standard models and ov0pAAA for tracks with a given amount of overshooting examples: ov0p25 ---> overshooting with l_ov=0.25 Hp The files show from left to right: 1) Model 2) Logarithm of the age (in Gyr) 3) Central abundance of H/He 4) Logarithm of the luminosity (Lo) 5) Logarithm of the effective temperature (K) 5) Logarithm of the central temperature (K) 6) Logarithm of the central density (g/cm**3) 7) Logarithm of the not central maximum temperature (K) 8) Mass coordinate of the maximum in temperature (M/Mtot) 9) Mass extension of the central convective region (Mo) 10) Mass extension of the helium core (Mo) 11) Mass coordinate of the bottom of the convective envelope (M/Mtot) 12) Fraction of the luminosity of the proton-proton chain over the total luminosity 13) Fraction of the luminosity of the CNO cicle over the total luminosity 14) Fraction of the luminosity of the He burning over the total luminosity 15) Fraction of the luminosity of the gravothermal energy over the total luminosity ===================================================================================== For any question please write to: scilla@df.unipi.it. last update 12/1/2004 =====================================================================================