Physics
Scientific paper
Jan 1963
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1963pthph..29...29t&link_type=abstract
Progress of Theoretical Physics, Vol. 29, No. 1, pp. 29-43
Physics
15
Scientific paper
With an increase of temperature in a stellar core in which helium has been consumed completely, various thermonuclear reactions occur successively: C^{12} + C^{12} reactions occur at 6 {×} 10^8 ^{circ}K, Ne^{20} ({γ} , {α})O^{16} reactions occur at 1.0 {×} 10^9 ^{circ}K and O^{16} + O^{16} reactions occur at 1.25{×}10^9 ^{circ}K. These reactions are accompanied by production and absorption of protons and α-particles, and various elements are synthesized. In the cases of C^{12} + C^{12} and O^{16} + O^{16} reactions, neutrons are also produced. If the stellar core is rich in carbon after helium burning, a considerable amount of heavy metals are produced, but if the core is rich in oxygen, heavy metals are scarecely produced. The elements remaining after oxygen burning are Mg^{24}, Mg^{25}, Si^{28}, P^{31}, etc., if carbon is abundant initially, and Si^{28}, S^{32}, etc., if oxygen is abundant. Reactions next arising are Mg^{25} ({γ}, n), P^{31}({γ}, p), S^{32}({γ}, p), S^{32}({γ}, {α}), etc., at 1.5 {×} 10^9 ^{circ}K. Further, Mg^{24} and Si^{28} are disintegrated at 2 {×} 10^9 ^{circ}K and then thermal equilibrium will be established for the concentrations of the disintegration products.
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