<scp>parsec</scp>: stellar tracks and isochrones with the PAdova and TRieste Stellar Evolution Code

Abstract

We present the updated version of the code used to compute stellar\nevolutionary tracks in Padova. It is the result of a thorough revision of the\nmajor input physics, together with the inclusion of the pre-main sequence\nphase, not present in our previous releases of stellar models. Another\ninnovative aspect is the possibility of promptly generating accurate opacity\ntables fully consistent with any selected initial chemical composition, by\ncoupling the OPAL opacity data at high temperatures to the molecular opacities\ncomputed with our AESOPUS code (Marigo &amp; Aringer 2009). In this work we present\nextended sets of stellar evolutionary models for various initial chemical\ncompositions, while other sets with different metallicities and/or different\ndistributions of heavy elements are being computed. For the present release of\nmodels we adopt the solar distribution of heavy elements from the recent\nrevision by Caffau et al. (2011), corresponding to a Sun's metallicity\nZ=0.0152. From all computed sets of stellar tracks, we also derive isochrones\nin several photometric systems. The aim is to provide the community with the\nbasic tools to model star clusters and galaxies by means of population\nsynthesis techniques.\n

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