We present the updated Pisa evolutionary database (available at the link: http://astro.df.unipi.it/stellar-models) which includes tracks and isochrones for evolutionary phases from the Pre-Main Sequence to the Asympthotic Giant Branch. Models are calculated by adopting a well-tested evolutionary code (FRANEC) implemented with updated physical and chemical inputs. Calculations for all the evolutionary phases have been computed for a grid of 216 chemical compositions with the fractional metal abundance in mass, Z, ranging from 0.0001 to 0.01, and the original helium content, Y, from 0.25 to 0.42 while PMS models includes metallicities up to Z=0.03. Models were computed for both solar-scaled and alpha -enhanced abundances with different external convection efficiencies.
The updated Pisa evolutionary model database
VALLE, GIADA;TOGNELLI, EMANUELE;DEGL'INNOCENTI, SCILLA;PRADA MORONI, PIER GIORGIO
2015-01-01
Abstract
We present the updated Pisa evolutionary database (available at the link: http://astro.df.unipi.it/stellar-models) which includes tracks and isochrones for evolutionary phases from the Pre-Main Sequence to the Asympthotic Giant Branch. Models are calculated by adopting a well-tested evolutionary code (FRANEC) implemented with updated physical and chemical inputs. Calculations for all the evolutionary phases have been computed for a grid of 216 chemical compositions with the fractional metal abundance in mass, Z, ranging from 0.0001 to 0.01, and the original helium content, Y, from 0.25 to 0.42 while PMS models includes metallicities up to Z=0.03. Models were computed for both solar-scaled and alpha -enhanced abundances with different external convection efficiencies.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
