University of Hertfordshire

By the same authors

Nuclear uncertainty study of the s-process in massive stars based on Monte-Carlo simulations

Research output: Chapter in Book/Report/Conference proceedingConference contribution

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Nuclear uncertainty study of the s-process in massive stars based on Monte-Carlo simulations. / Nishimura, N.; Hirschi, R.; Rauscher, T.

Proceedings of Science. Proceedings of Science (PoS), 2014. 127.

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Harvard

Nishimura, N, Hirschi, R & Rauscher, T 2014, Nuclear uncertainty study of the s-process in massive stars based on Monte-Carlo simulations. in Proceedings of Science., 127, Proceedings of Science (PoS), 13th Nuclei in the Cosmos, NIC 2014, Debrecen, Hungary, 7/07/14.

APA

Nishimura, N., Hirschi, R., & Rauscher, T. (2014). Nuclear uncertainty study of the s-process in massive stars based on Monte-Carlo simulations. In Proceedings of Science [127] Proceedings of Science (PoS).

Vancouver

Nishimura N, Hirschi R, Rauscher T. Nuclear uncertainty study of the s-process in massive stars based on Monte-Carlo simulations. In Proceedings of Science. Proceedings of Science (PoS). 2014. 127

Author

Nishimura, N. ; Hirschi, R. ; Rauscher, T. / Nuclear uncertainty study of the s-process in massive stars based on Monte-Carlo simulations. Proceedings of Science. Proceedings of Science (PoS), 2014.

Bibtex

@inproceedings{c3b7f988a501455fb2b991299cdbc9b3,
title = "Nuclear uncertainty study of the s-process in massive stars based on Monte-Carlo simulations",
abstract = "The s-process in massive stars, the weak s-process, is origin of the solar s-process nuclei up to A = 90 as well as other heavier nuclei, e.g., Ba, in very metal-poor stars. The s-process still has a significant uncertainty of nuclear reactions, although we has used several theoretical abundance prediction for the comparisons with several observations. The present study is aimed at evaluating the reliability of the current theoretical s-process calculations. Based on different stellar evolution models, we performed Monte-Carlo simulations of the s-process with randomly varying neutron- captures rates. We found that the uncertainty propagates through the weak s-process nuclei up to Sr for a solar metallically star. On the other hand, a rotating metal-poor star shows different response to final abundances, which heavier s-process elements, i.e., Ba, have significant variation. In conclusion, the remaining uncertainty of neutron-capture reactions is still possible to change the results of s-process calculations. This uncertainty even can be caused in qualitative difference in the production of heavy s-process nuclei in a metal-poor stars.",
author = "N. Nishimura and R. Hirschi and T. Rauscher",
note = "ISSN 1824-8039",
year = "2014",
month = "12",
day = "31",
language = "English",
booktitle = "Proceedings of Science",
publisher = "Proceedings of Science (PoS)",

}

RIS

TY - GEN

T1 - Nuclear uncertainty study of the s-process in massive stars based on Monte-Carlo simulations

AU - Nishimura, N.

AU - Hirschi, R.

AU - Rauscher, T.

N1 - ISSN 1824-8039

PY - 2014/12/31

Y1 - 2014/12/31

N2 - The s-process in massive stars, the weak s-process, is origin of the solar s-process nuclei up to A = 90 as well as other heavier nuclei, e.g., Ba, in very metal-poor stars. The s-process still has a significant uncertainty of nuclear reactions, although we has used several theoretical abundance prediction for the comparisons with several observations. The present study is aimed at evaluating the reliability of the current theoretical s-process calculations. Based on different stellar evolution models, we performed Monte-Carlo simulations of the s-process with randomly varying neutron- captures rates. We found that the uncertainty propagates through the weak s-process nuclei up to Sr for a solar metallically star. On the other hand, a rotating metal-poor star shows different response to final abundances, which heavier s-process elements, i.e., Ba, have significant variation. In conclusion, the remaining uncertainty of neutron-capture reactions is still possible to change the results of s-process calculations. This uncertainty even can be caused in qualitative difference in the production of heavy s-process nuclei in a metal-poor stars.

AB - The s-process in massive stars, the weak s-process, is origin of the solar s-process nuclei up to A = 90 as well as other heavier nuclei, e.g., Ba, in very metal-poor stars. The s-process still has a significant uncertainty of nuclear reactions, although we has used several theoretical abundance prediction for the comparisons with several observations. The present study is aimed at evaluating the reliability of the current theoretical s-process calculations. Based on different stellar evolution models, we performed Monte-Carlo simulations of the s-process with randomly varying neutron- captures rates. We found that the uncertainty propagates through the weak s-process nuclei up to Sr for a solar metallically star. On the other hand, a rotating metal-poor star shows different response to final abundances, which heavier s-process elements, i.e., Ba, have significant variation. In conclusion, the remaining uncertainty of neutron-capture reactions is still possible to change the results of s-process calculations. This uncertainty even can be caused in qualitative difference in the production of heavy s-process nuclei in a metal-poor stars.

UR - http://www.scopus.com/inward/record.url?scp=84957674390&partnerID=8YFLogxK

M3 - Conference contribution

BT - Proceedings of Science

PB - Proceedings of Science (PoS)

ER -