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Nucleosynthesis in neutrino-driven, aspherical Population III supernovae

Published online by Cambridge University Press:  05 September 2012

Shin-ichiro Fujimoto ,
Masa-aki Hashimoto ,
Masaomi Ono  and
Kei Kotake
Shin-ichiro Fujimoto
Affiliation:
Kumamoto National College of Technology, 2659-2 Suya, Goshi, Kumamoto 861-1102, Japan email: [email protected]
Masa-aki Hashimoto
Affiliation:
Kyushu University, Fukuoka 810-8560, Japan
Masaomi Ono
Affiliation:
Kyoto University, Kyoto, 606-8502, Japan
Kei Kotake
Affiliation:
National Astronomical Observatory Japan, Tokyo, 181-8588, Japan
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Abstract

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We investigate explosive nucleosynthesis during neutrino-driven, aspherical supernova (SN) explosion aided by standing accretion shock instability (SASI), based on two-dimensional hydrodynamic simulations of the explosion of 11, 15, 20, 25, 30 and 40M⊙ stars with zero metallicity. The magnitude and asymmetry of the explosion energy are estimated with simulations, for a given set of neutrino luminosities and temperatures, not as in the previous study in which the explosion is manually and spherically initiated by means of a thermal bomb or a piston and also some artificial mixing procedures are applied for the estimate of abundances of the SN ejecta.

By post-processing calculations with a large nuclear reaction network, we have evaluated abundances and masses of ejecta from the aspherical SNe. We find that matter mixing induced via SASI is important for the abundant production of nuclei with atomic number ≥ 21, in particular Sc, which is underproduced in the spherical models without artificial mixing. We also find that the IMF-averaged abundances are similar to those observed in extremely metal poor stars. However, observed [K/Fe] cannot be reproduced with our aspherical SN models.

Keywords

Supernovae: generalnuclear reactionsnucleosynthesisabundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S279: Death of Massive Stars: Supernovae and Gamma-Ray Bursts , April 2011 , pp. 237 - 240
Copyright
Copyright © International Astronomical Union 2012

References

Cayrel, R., Depagne, E., Spite, M., et al. 2004, A&A, 416, 1117Google Scholar
Tominaga, N., Umeda, H., & Nomoto, K. 2007, ApJ, 660, 516CrossRefGoogle Scholar
Heger, A. & Woosley, S. E. 2010, ApJ, 724, 341CrossRefGoogle Scholar
Joggerst, C. C., Woosley, S. E., & Heger, A. 2009, ApJ, 693, 1780CrossRefGoogle Scholar
Joggerst, C. C., Almgren, A., Bell, J., et al. 2010, ApJ, 709, 11CrossRefGoogle Scholar
Marek, A., & Janka, H.-T. 2009, ApJ, 694, 664CrossRefGoogle Scholar
Suwa, Y., Kotake, K., Takiwaki, T., Whitehouse, S., & Liebendörfer, M. 2010, PASJ, 62, L49.CrossRefGoogle Scholar
Ohnishi, N., Kotake, K., & Yamada, S. 2006, ApJ, 641, 1018CrossRefGoogle Scholar
Fujimoto, S., Hashimoto, M., Ono, M., & Kotake, K. 2011, ApJ, 738, 61CrossRefGoogle Scholar
O'Connor, E. & Ott, C. D. 2011, ApJ, 730, 70CrossRefGoogle Scholar
Andrievsky, S. M., Spite, M., Korotin, S. A., et al. 2008, A&A, 481, 481Google Scholar
Preston, G. W., Sneden, C., Thompson, I. B., et al. 2006, AJ, 132, 85CrossRefGoogle Scholar