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According to a standard initial mass function, stars in the range 7-12 Msunconstitute ~50% (by number) of the stars more massive than ~7 Msun, but, inspite of this, their evolutionary properties, and in particular their finalfate, are still scarcely studied. In this paper we present a detailed study ofthe evolutionary properties of solar metallicity, non rotating stars in therange 7-15 Msun, from the pre main sequence phase up to the presupernova stageor up to an advanced stage of the thermally pulsing phase, depending on theinitial mass. We find that (1) the 7.00 Msun develops a degenerate CO core andevolves as a classical AGB star in the sense that it does not ignite the Cburning reactions; (2) stars with the initial mass M >= 9.22 Msun end theirlife as core collapse supernovae; (3) stars in the range 7.50 <= M/Msun <= 9.20develop a degenerate ONeMg core and evolve through the thermally pulsing SAGBphase; 4) stars in the mass range 7.50 <= M/Msun <= 8.00 end their life ashybrid CO/ONeMg- or ONeMg- WD; (5) stars with the initial mass in the range8.50 <= M/Msun <= 9.20 may potentially explode as electron capture supernovae.

Evolution and final fate of solar metallicity stars in the mass range  7-15 Msun. I. The transition from AGB to SAGB stars, Electron Capture and  Core Collapse Supernovae progenitors