CHIEFFI, ALESSANDROALESSANDROCHIEFFILIMONGI, MarcoMarcoLIMONGI2020-08-252020-08-2520170004-637Xhttp://hdl.handle.net/20.500.12386/26807We discuss the influence of rotation on the combined synthesis of {}<SUP>44</SUP>{Ti} and {}<SUP>56</SUP>{Ni} in massive stars. While {}<SUP>56</SUP>{Ni} is significantly produced by both complete and incomplete explosive Si burning, {}<SUP>44</SUP>{Ti} is mainly produced by complete explosive Si burning, with a minor contribution (in standard non-rotating models) from incomplete explosive Si burning and O burning (both explosive and hydrostatic). We find that, in most cases, the thickness of the region exposed to incomplete explosive Si burning increases in rotating models (initial velocity, v <SUB>ini</SUB> = 300 km s<SUP>-1</SUP>) and since {}<SUP>56</SUP>{Ni} is significantly produced in this zone, the fraction of mass coming from the complete explosive Si burning zone necessary to get the required amount of {}<SUP>56</SUP>{Ni} reduces. Therefore the amount of {}<SUP>44</SUP>{Ti} ejected for a given fixed amount of {}<SUP>56</SUP>{Ni} decreases in rotating models. However, some rotating models at [Fe/H] = -1 develop a very extended O convective shell in which a consistent amount of {}<SUP>44</SUP>{Ti} is formed, preserved, and ejected in the interstellar medium. Hence a better modeling of the thermal instabilities (convection) in the advanced burning phases together with a critical analysis of the cross sections of the nuclear reactions operating in O burning are relevant for the understanding of the synthesis of {}<SUP>44</SUP>{Ti}.STAMPAenArticle10.3847/1538-4357/836/1/792-s2.0-85014312290000397304500031https://iopscience.iop.org/article/10.3847/1538-4357/836/1/792017ApJ...836...79CFIS/05 - ASTRONOMIA E ASTROFISICAERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation