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http://hdl.handle.net/20.500.12386/26807
Titolo: | The Synthesis of 44 Ti and 56 Ni in Massive Stars | Autori: | CHIEFFI, ALESSANDRO LIMONGI, Marco |
Data pubblicazione: | 2017 | Rivista: | THE ASTROPHYSICAL JOURNAL | Numero: | 836 | Fascicolo: | 1 | Da pagina:: | 79 | Abstract: | We 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}. | URI: | http://hdl.handle.net/20.500.12386/26807 | URL: | https://iopscience.iop.org/article/10.3847/1538-4357/836/1/79 | ISSN: | 0004-637X | DOI: | 10.3847/1538-4357/836/1/79 | Bibcode ADS: | 2017ApJ...836...79C | Fulltext: | open |
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