Explosive nucleosynthesis in magnetohydrodynamical jets from collapsars. II

Heavy-element nucleosynthesis of s, p, r-processes

Masaomi Ono, Masa-Aki Hashimoto, Shin Ichiro Fujimoto, Kei Kotake, Shoichi Yamada

Research output: Contribution to journalArticle

14 Citations (Scopus)

Abstract

p-elements of A 90 are produced via photodisintegrations of seed s-elements. However, the produced p-elements are disintegrated in later stages except for 180Ta. In the explosive nucleosynthesis, elements of 90 A 160 are significantly overproduced relative to the solar values owing to the r-process, which is very different from the results of spherical explosion models. Only heavy p-elements (N 50) are overproduced via the p-process because of the low peak temperatures in the oxygen- and neon-rich layers. Compared with the previous study of r-process nucleosynthesis calculations in the collapsar model of 40 M- by Fujimoto et al. [S. Fujimoto, M. Hashimoto, K. Kotake and S. Yamada, Astrophys. J. 656 (2007), 382; S. Fujimoto, N. Nishimura and M. Hashimoto, Astrophys. J. 680 (2008), 1350], our jet model cannot contribute to the third peak of the solar r-elements and intermediate p-elements, which have been much produced because of the distribution of the lowest part of electron fraction in the ejecta. Averaging the overproduction factors over the progenitor masses with the use of Salpeter's IMF, we suggest that the 70 M star could contribute to the solar weak s-elements of 60 A 90 and neutron-rich elements of 90 ; A 160. We confirm the primary synthesis of light p-elements in the ejected matter of high peak temperature. The ejected matter has [Sr/Eu] 0.4, which is different from that of a typical r-process-enriched star CS22892-052 ([Sr/Eu] 1). We find that Sr-Y-Zr isotopes are primarily synthesized in the explosive nucleosynthesis in a similar process of the primary production of light p-elements, which has been considered as one of the sites of a lighter element primary process (LEPP). Tokyo 113-0033 JPN.

Original languageEnglish
Pages (from-to)741-765
Number of pages25
JournalProgress of Theoretical Physics
Volume128
Issue number4
DOIs
Publication statusPublished - Oct 1 2012

Fingerprint

heavy elements
nuclear fusion
M stars
ejecta
neon
explosions
seeds
isotopes
neutrons
stars
temperature
oxygen
synthesis
electrons

All Science Journal Classification (ASJC) codes

  • Physics and Astronomy (miscellaneous)

Cite this

Explosive nucleosynthesis in magnetohydrodynamical jets from collapsars. II : Heavy-element nucleosynthesis of s, p, r-processes. / Ono, Masaomi; Hashimoto, Masa-Aki; Fujimoto, Shin Ichiro; Kotake, Kei; Yamada, Shoichi.

In: Progress of Theoretical Physics, Vol. 128, No. 4, 01.10.2012, p. 741-765.

Research output: Contribution to journalArticle

Ono, Masaomi ; Hashimoto, Masa-Aki ; Fujimoto, Shin Ichiro ; Kotake, Kei ; Yamada, Shoichi. / Explosive nucleosynthesis in magnetohydrodynamical jets from collapsars. II : Heavy-element nucleosynthesis of s, p, r-processes. In: Progress of Theoretical Physics. 2012 ; Vol. 128, No. 4. pp. 741-765.
@article{957238e972d448e9adce1474de700e60,
title = "Explosive nucleosynthesis in magnetohydrodynamical jets from collapsars. II: Heavy-element nucleosynthesis of s, p, r-processes",
abstract = "p-elements of A 90 are produced via photodisintegrations of seed s-elements. However, the produced p-elements are disintegrated in later stages except for 180Ta. In the explosive nucleosynthesis, elements of 90 A 160 are significantly overproduced relative to the solar values owing to the r-process, which is very different from the results of spherical explosion models. Only heavy p-elements (N 50) are overproduced via the p-process because of the low peak temperatures in the oxygen- and neon-rich layers. Compared with the previous study of r-process nucleosynthesis calculations in the collapsar model of 40 M- by Fujimoto et al. [S. Fujimoto, M. Hashimoto, K. Kotake and S. Yamada, Astrophys. J. 656 (2007), 382; S. Fujimoto, N. Nishimura and M. Hashimoto, Astrophys. J. 680 (2008), 1350], our jet model cannot contribute to the third peak of the solar r-elements and intermediate p-elements, which have been much produced because of the distribution of the lowest part of electron fraction in the ejecta. Averaging the overproduction factors over the progenitor masses with the use of Salpeter's IMF, we suggest that the 70 M star could contribute to the solar weak s-elements of 60 A 90 and neutron-rich elements of 90 ; A 160. We confirm the primary synthesis of light p-elements in the ejected matter of high peak temperature. The ejected matter has [Sr/Eu] 0.4, which is different from that of a typical r-process-enriched star CS22892-052 ([Sr/Eu] 1). We find that Sr-Y-Zr isotopes are primarily synthesized in the explosive nucleosynthesis in a similar process of the primary production of light p-elements, which has been considered as one of the sites of a lighter element primary process (LEPP). Tokyo 113-0033 JPN.",
author = "Masaomi Ono and Masa-Aki Hashimoto and Fujimoto, {Shin Ichiro} and Kei Kotake and Shoichi Yamada",
year = "2012",
month = "10",
day = "1",
doi = "10.1143/PTP.128.741",
language = "English",
volume = "128",
pages = "741--765",
journal = "Progress of Theoretical Physics",
issn = "0033-068X",
publisher = "Published for the Research Institute for Fundamental Physics by Physical Society of Japan",
number = "4",

}

TY - JOUR

T1 - Explosive nucleosynthesis in magnetohydrodynamical jets from collapsars. II

T2 - Heavy-element nucleosynthesis of s, p, r-processes

AU - Ono, Masaomi

AU - Hashimoto, Masa-Aki

AU - Fujimoto, Shin Ichiro

AU - Kotake, Kei

AU - Yamada, Shoichi

PY - 2012/10/1

Y1 - 2012/10/1

N2 - p-elements of A 90 are produced via photodisintegrations of seed s-elements. However, the produced p-elements are disintegrated in later stages except for 180Ta. In the explosive nucleosynthesis, elements of 90 A 160 are significantly overproduced relative to the solar values owing to the r-process, which is very different from the results of spherical explosion models. Only heavy p-elements (N 50) are overproduced via the p-process because of the low peak temperatures in the oxygen- and neon-rich layers. Compared with the previous study of r-process nucleosynthesis calculations in the collapsar model of 40 M- by Fujimoto et al. [S. Fujimoto, M. Hashimoto, K. Kotake and S. Yamada, Astrophys. J. 656 (2007), 382; S. Fujimoto, N. Nishimura and M. Hashimoto, Astrophys. J. 680 (2008), 1350], our jet model cannot contribute to the third peak of the solar r-elements and intermediate p-elements, which have been much produced because of the distribution of the lowest part of electron fraction in the ejecta. Averaging the overproduction factors over the progenitor masses with the use of Salpeter's IMF, we suggest that the 70 M star could contribute to the solar weak s-elements of 60 A 90 and neutron-rich elements of 90 ; A 160. We confirm the primary synthesis of light p-elements in the ejected matter of high peak temperature. The ejected matter has [Sr/Eu] 0.4, which is different from that of a typical r-process-enriched star CS22892-052 ([Sr/Eu] 1). We find that Sr-Y-Zr isotopes are primarily synthesized in the explosive nucleosynthesis in a similar process of the primary production of light p-elements, which has been considered as one of the sites of a lighter element primary process (LEPP). Tokyo 113-0033 JPN.

AB - p-elements of A 90 are produced via photodisintegrations of seed s-elements. However, the produced p-elements are disintegrated in later stages except for 180Ta. In the explosive nucleosynthesis, elements of 90 A 160 are significantly overproduced relative to the solar values owing to the r-process, which is very different from the results of spherical explosion models. Only heavy p-elements (N 50) are overproduced via the p-process because of the low peak temperatures in the oxygen- and neon-rich layers. Compared with the previous study of r-process nucleosynthesis calculations in the collapsar model of 40 M- by Fujimoto et al. [S. Fujimoto, M. Hashimoto, K. Kotake and S. Yamada, Astrophys. J. 656 (2007), 382; S. Fujimoto, N. Nishimura and M. Hashimoto, Astrophys. J. 680 (2008), 1350], our jet model cannot contribute to the third peak of the solar r-elements and intermediate p-elements, which have been much produced because of the distribution of the lowest part of electron fraction in the ejecta. Averaging the overproduction factors over the progenitor masses with the use of Salpeter's IMF, we suggest that the 70 M star could contribute to the solar weak s-elements of 60 A 90 and neutron-rich elements of 90 ; A 160. We confirm the primary synthesis of light p-elements in the ejected matter of high peak temperature. The ejected matter has [Sr/Eu] 0.4, which is different from that of a typical r-process-enriched star CS22892-052 ([Sr/Eu] 1). We find that Sr-Y-Zr isotopes are primarily synthesized in the explosive nucleosynthesis in a similar process of the primary production of light p-elements, which has been considered as one of the sites of a lighter element primary process (LEPP). Tokyo 113-0033 JPN.

UR - http://www.scopus.com/inward/record.url?scp=84868140359&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84868140359&partnerID=8YFLogxK

U2 - 10.1143/PTP.128.741

DO - 10.1143/PTP.128.741

M3 - Article

VL - 128

SP - 741

EP - 765

JO - Progress of Theoretical Physics

JF - Progress of Theoretical Physics

SN - 0033-068X

IS - 4

ER -