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Stellar structure model data during the Asymptotic Giant Branch phase. If you use these data please provide a reference to the following paper: Karakas & Lattanzio (2007, PASA, submitted) Each file contains: 1) pulse number 2) the core mass, Mcore (Msun) 3) maximum mass of the intershell convection zone, M_csh (Msun) 4) duration of intershell convection, t_csh (years) 5) mass dredged into the envelope, D_dredge (Msun) 6) lambda 7) lambda_dup defined by Goriely & Mowlavi (= lambda x (DMh/Mpulse) where Mpulse is the maximum mass of the intershell convection zone, given in column 2 8) maximum temperature in the He-shell, THeshell (K) 9) maximum temperature at the base of the convective envelope during the previous interpulse period, Tbce (K) 10) maximum temperature in the H-shell during the previous interpulse period, THshell (K) 11) interpulse period (years) - note that the first entry is set to zero 12) the total mass, Mtot (Msun) 13) maximum radiated luminosity during the interpulse period, MaxL (Lsun) 14) maximum He-luminosity during a thermal pulse, MaxLHe (Lsun) All units are in solar units except temperatures, which are in kelvin and times, which are in years.