Relativistic Jets in Population III Supernova and Extremely Metal-Poor Stars

Details Relativistic Jets in Population III Supernova and Extremely Metal-Poor Stars Relativistic Jets in Population III Supernova and Extremely Metal-Poor Stars

Mar 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007ebhe.conf..361t&link_type=abstract

ENERGY BUDGET IN THE HIGH ENERGY UNIVERSE . Proceedings of the International Workshop. Held 22-24 February 2006 in Kashiwa, Japa

Computer Science

Scientific paper

We calculate explosive nucleosynthsis induced by relativistic jets in Population III stars with 2-dimensional special relativistic hydrodynamics code. The resulting yields are compared with the abundance patterns of extremely metal-poor stars. Extremely metal-poor stars in Galactic halo, whose metallicities are much smaller than the Sun ([Fe/H] < -3), have been extensively observed. These stars are classified by their metallicities, i.e., extremely metal-poor (EMP: -4 < [Fe/H]< -3 and [C/Fe] ˜ 0), carbon-rich EMP (CEMP: -4 < [Fe/H]< -3 and +1 < [C/Fe]), and hyper metal-poor (HMP: [Fe/H]< -5 and [C/Fe]~ +4) stars. The abundance patterns of these stars have been reproduced by 1-dimensional mixing-fallback model in the previous studies. Though the differences among the EMP, CEMP, HMP stars have been well-explained by the different mixing region and ejection factor, it has not been clear what causes these differences. In this study, we show that the yields of 2-dimensional jet-like explosions give good agreements with the abundance patterns of EMP, CEMP, HMP stars and that an energy injection rate from the central engine plays an important role in producing the differences among EMP, CEMP, HMP stars.

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