TY - GEN
T1 - Nucleosynthesis in Jets from Collapsars
AU - Fujimoto, Shin Ichiro
AU - Nishimura, Nobuya
AU - Hashimoto, Masa Aki
N1 - Funding Information:
This work was supported in part by Grant-in-Aid for tlie Scientific Researcli from tlie Ministry of Education, Science and Culture of Japan (No. 17540267)
PY - 2008
Y1 - 2008
N2 - We investigate nucleosynthesis inside magnetically driven jets ejected from collapsars, or rotating magnetized stars collapsing to a black hole, based on two-dimensional magnetohydrodynamic simulation of the collapsars during the core collapse. We follow the evolution of the abundances of about 4000 nuclides from the collapse phase to the ejection phase using a large nuclear reaction network. We find that the r-process successfully operates only in the energetic jets (>1051 erg), so that U and Th are synthesized abundantly, even when the collapsars have a relatively small magnetic field (1010 G) and a moderately rotating core before the collapse. The abundance patterns inside the jets are similar to that of the r-elements in the solar system. The higher energy jets have larger amounts of 56Ni. Less energetic jets, which have small amounts of 56Ni, could induce GRB without supernova, such as GRB060505 and GRB060614.
AB - We investigate nucleosynthesis inside magnetically driven jets ejected from collapsars, or rotating magnetized stars collapsing to a black hole, based on two-dimensional magnetohydrodynamic simulation of the collapsars during the core collapse. We follow the evolution of the abundances of about 4000 nuclides from the collapse phase to the ejection phase using a large nuclear reaction network. We find that the r-process successfully operates only in the energetic jets (>1051 erg), so that U and Th are synthesized abundantly, even when the collapsars have a relatively small magnetic field (1010 G) and a moderately rotating core before the collapse. The abundance patterns inside the jets are similar to that of the r-elements in the solar system. The higher energy jets have larger amounts of 56Ni. Less energetic jets, which have small amounts of 56Ni, could induce GRB without supernova, such as GRB060505 and GRB060614.
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U2 - 10.1063/1.2943639
DO - 10.1063/1.2943639
M3 - Conference contribution
AN - SCOPUS:85036579542
T3 - AIP Conference Proceedings
SP - 99
EP - 104
BT - Origin of Matter and Evolution of Galaxies - 10th International Symposium on Origin of Matter and Evolution of Galaxies
A2 - Kajino, Toshitaka
A2 - Suda, Takuma
A2 - Nozawa, Takaya
A2 - Ohnishi, Akira
A2 - Fujimoto, Masayuki Y.
A2 - Kubono, Shigeru
A2 - Kato, Kiyoshi
PB - American Institute of Physics Inc.
T2 - 10th International Symposium on Origin of Matter and Evolution of Galaxies: From the Dawn of Universe to the Formation of Solar System, OMEG 2007
Y2 - 4 December 2007 through 7 December 2007
ER -