R-process nucleosynthesis during the magnetohydrodynamics explosions of a massive star

Motoaki Saruwatari; Masa Aki Hashimoto; Kei Kotake; Shoichi Yamada

doi:10.1063/1.3485183

R-process nucleosynthesis during the magnetohydrodynamics explosions of a massive star

Motoaki Saruwatari, Masa Aki Hashimoto, Kei Kotake, Shoichi Yamada

Experimental Particle Physics

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

Abstract

We investigate the possibility of the r-process during the magnetohydrohynamical explosion of supernova in a massive star of 13 solar mass with the effects of neutrinos induced. We adopt five kinds of initial models which include properties of rotation and the toroidal component of the magnetic field. The simulations which succeed the explosions are limitted to a concentrated magnetic field and strong differential rotation. Low Y_e ejecta produce heavy elements and the third peak can be reprocuced. However, the second peak is low because Y_e distribution as a function of radius is steep and ejecta corresponding to middle Y_e is very few.

Original language	English
Title of host publication	10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10
Pages	409-411
Number of pages	3
DOIs	https://doi.org/10.1063/1.3485183
Publication status	Published - 2010
Event	10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10 - Osaka, Japan Duration: Mar 8 2010 → Mar 10 2010

Publication series

Name	AIP Conference Proceedings
Volume	1269
ISSN (Print)	0094-243X
ISSN (Electronic)	1551-7616

Other

Other	10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10
Country	Japan
City	Osaka
Period	3/8/10 → 3/10/10

All Science Journal Classification (ASJC) codes

Physics and Astronomy(all)

Access to Document

10.1063/1.3485183

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R-process nucleosynthesis during the magnetohydrodynamics explosions of a massive star. / Saruwatari, Motoaki; Hashimoto, Masa Aki; Kotake, Kei; Yamada, Shoichi.

10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10. 2010. p. 409-411 (AIP Conference Proceedings; Vol. 1269).

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

Saruwatari, M, Hashimoto, MA, Kotake, K & Yamada, S 2010, R-process nucleosynthesis during the magnetohydrodynamics explosions of a massive star. in 10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10. AIP Conference Proceedings, vol. 1269, pp. 409-411, 10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10, Osaka, Japan, 3/8/10. https://doi.org/10.1063/1.3485183

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abstract = "We investigate the possibility of the r-process during the magnetohydrohynamical explosion of supernova in a massive star of 13 solar mass with the effects of neutrinos induced. We adopt five kinds of initial models which include properties of rotation and the toroidal component of the magnetic field. The simulations which succeed the explosions are limitted to a concentrated magnetic field and strong differential rotation. Low Ye ejecta produce heavy elements and the third peak can be reprocuced. However, the second peak is low because Ye distribution as a function of radius is steep and ejecta corresponding to middle Ye is very few.",

author = "Motoaki Saruwatari and Hashimoto, {Masa Aki} and Kei Kotake and Shoichi Yamada",

note = "Copyright: Copyright 2010 Elsevier B.V., All rights reserved.; 10th International Symposium on Origin of Matter and Evolution of Galaxies, OMEG10 ; Conference date: 08-03-2010 Through 10-03-2010",

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AB - We investigate the possibility of the r-process during the magnetohydrohynamical explosion of supernova in a massive star of 13 solar mass with the effects of neutrinos induced. We adopt five kinds of initial models which include properties of rotation and the toroidal component of the magnetic field. The simulations which succeed the explosions are limitted to a concentrated magnetic field and strong differential rotation. Low Ye ejecta produce heavy elements and the third peak can be reprocuced. However, the second peak is low because Ye distribution as a function of radius is steep and ejecta corresponding to middle Ye is very few.

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