Explosive Nucleosynthesis in Pair-Instability Supernovae

Details Explosive Nucleosynthesis in Pair-Instability Supernovae Explosive Nucleosynthesis in Pair-Instability Supernovae

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003omeg.conf..362n&link_type=abstract

ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2000. Proceedings of the International Symposium. Held 19-21 January 2000 in Universi

Astronomy and Astrophysics

Astronomy

Scientific paper

We calculate the final evolution of very massive population III stars in the mass range of 150 to 300 M&sun; and obtain detailed nucleosynthesis yields of their explosions. We perform hydrodynamic simulations of the collapse-explosion process caused by e+e--pair creation instability during their oxygen burning phase and calculate explosive nucleosynthesis with an extended nuclear reaction network. We then obtain the following results: 1) Population III Stars of 150 - 200M&sun; explode as pair-instability supernovae. The upper mass limit for the explosion is between 200 - 300M&sun;. 2) In pair-instability supernovae, iron is produced more abundantly from more massive progenitors. 3) Pair-instability supernovae produce large amounts of Si, S, Ar and Ca relative to O. This is a similar characteristic as that of hypernovae (E ≥ 1052 erg), the progenitors of which have 30-40 M&sun; on their main-sequence. 4) We compare our yields with those of the observed metal-deficient stars. The abundance patterns are not in good accord and it implies that pair-instability supernovae were not dominant in the early Galaxy. 5) We also calculate theoretical light curves of a pair-instability supernova and find that they are very luminous (L ~ 1043 erg s-1) because of the large production of 56Ni.

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