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Lithium, beryllium, and boron production in core-collapse supernovae

Published online by Cambridge University Press:  23 April 2010

Ko Nakamura ,
Takashi Yoshida ,
Toshikazu Shigeyama  and
Toshitaka Kajino
Ko Nakamura
Affiliation:
National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo, 181-8588Japan email: nakamura.ko@nao.ac.jp
Takashi Yoshida
Affiliation:
Department of Astronomy, Graduate School of Science, University of Tokyo, Hongo 7-3-1, Bunkyo-ku, Tokyo, 113-0033Japan
Toshikazu Shigeyama
Affiliation:
Department of Astronomy, Graduate School of Science, University of Tokyo, Hongo 7-3-1, Bunkyo-ku, Tokyo, 113-0033Japan Research Center for the Early Universe, Graduate School of Science, University of Tokyo
Toshitaka Kajino
Affiliation:
National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo, 181-8588Japan email: nakamura.ko@nao.ac.jp Department of Astronomy, Graduate School of Science, University of Tokyo, Hongo 7-3-1, Bunkyo-ku, Tokyo, 113-0033Japan
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Abstract

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Type Ic supernova (SN Ic) is the gravitational collapse of a massive star without H and He layers. It propels several solar masses of material to the typical velocity of 10,000 km/s, a very small fraction of the ejecta nearly to the speed of light. We investigate SNe Ic as production sites for the light elements Li, Be, and B, via the neutrino-process and spallations. As massive stars collapse, neutrinos are emitted in large numbers from the central remnants. Some of the neutrinos interact with nuclei in the exploding materials and mainly 7Li and 11B are produced. Subsequently, the ejected materials with very high energy impinge on the interstellar/circumstellar matter and spall into light elements. We find that the ν-process in the current SN Ic model produces a significant amount of 11B, consistent with observations if combined with B isotopes from the following spallation production.

Keywords

Neutrinosnuclear reactionsnucleosynthesisabundances – Supernovae: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S268: Light Elements in the Universe , November 2009 , pp. 463 - 468
Copyright
Copyright © International Astronomical Union 2010

References

Cameron, A. G. W. 1955, ApJ, 121, 144CrossRefGoogle Scholar
Fields, B. D., Daigne, F., Cassé, M., & Vangioni-Flam, E. 2002, ApJ, 581, 389CrossRefGoogle Scholar
Heger, A., Kolbe, E., Haxton, W. C., Langanke, K., Martínez-Pinedo, G., & Woosley, S. E. 2005, Phys. Lett. B, 606, 258CrossRefGoogle Scholar
Higdon, J. C., Lingenfelter, R. E., & Ramaty, R. 1998, ApJl, 509, L33CrossRefGoogle Scholar
Kohri, K., Narayan, R., & Piran, T. 2005, ApJ, 629, 341CrossRefGoogle Scholar
Maceroni, C., Testa, V., Plez, B., García Lario, P., & D'Antona, F. 2002, A&A, 395, 179Google Scholar
Meneguzzi, M., Audouze, J., & Reeves, H. 1971, A&A, 15, 337Google Scholar
Meynet, G. & Maeder, A. 2002, A&A, 390, 561Google Scholar
Nakamura, K. & Shigeyama, T. 2004, ApJ, 610, 888CrossRefGoogle Scholar
Nakamura, K., Inoue, S., Wanajo, S., & Shigeyama, T. 2006, ApJl, 643, L115CrossRefGoogle Scholar
Nakamura, T., Mazzali, P. A., Nomoto, K., & Iwamoto, K. 2001, ApJ, 550, 991CrossRefGoogle Scholar
Read, S. M. & Viola, V. E. 1984, Atomic Data and Nuclear Data Tables, 31, 359CrossRefGoogle Scholar
Rollinde, E., Maurin, D., Vangioni, E., Olive, K. A., & Inoue, S. 2008, ApJ, 673, 676CrossRefGoogle Scholar
Romano, D., Matteucci, F., Ventura, P., & D'Antona, F. 2001, A&A, 374, 646Google Scholar
Spite, F. & Spite, M. 1982,A&A, 115, 357Google Scholar
Sumiyoshi, K., Yamada, S., Suzuki, H., & Chiba, S. 2006, Phys. Rev. Lett., 97, 091101CrossRefGoogle Scholar
Surman, R. & McLaughlin, G. C. 2005, ApJ, 618, 397CrossRefGoogle Scholar
Suzuki, T. K. & Inoue, S. 2002, ApJ, 573, 168CrossRefGoogle Scholar
Ventura, P., D'Antona, F., & Mazzitelli, I. 2002, A&A, 393, 215Google Scholar
Woosley, S. E., Hartmann, D. H., Hoffman, R. D., & Haxton, W. C. 1990, ApJ, 356, 272CrossRefGoogle Scholar
Yoshida, T., Kajino, T., & Hartmann, D. H. 2005, Phys. Rev. Lett., 94, 231101CrossRefGoogle Scholar
Yoshida, T., Suzuki, T., Chiba, S., Kajino, T., Yokomakura, H., Kimura, K., Takamura, A., & Hartmann, D. H. 2008, ApJ, 686, 448CrossRefGoogle Scholar