TY - JOUR
T1 - Nucleosynthesis of r-process elements by jittering jets in core-collapse supernovae
AU - Papish, Oded
AU - Soker, Noam
N1 - Copyright:
Copyright 2012 Elsevier B.V., All rights reserved.
PY - 2012/4
Y1 - 2012/4
N2 - We calculate the nucleosynthesis inside the hot bubble formed in the jittering-jets model for core-collapse supernova explosions, and find the formation of several times 10 -4M ⊙ r-process elements. In the jittering-jets model, fast jets launched from a stochastic accretion disc around the newly formed neutron star are shocked at several thousand km, and form hot high-pressure bubbles. These bubbles merge to form a large bubble that explodes the star. In this study, we assume a spherically symmetric homogenous bubble, and follow its evolution for about 1 s during which nuclear reactions take place. The jets last for about 1 s, their velocity v j= 0.5c, and their total energy is ∼10 51erg. We use jets' neutron enrichment independent of time, and follow the nuclear reactions to the formation of seed nuclei up to Z≤ 50, on which more neutrons will be absorbed to form r-process elements. Based on the mass of the seed nuclei, we find the r-process element mass in our idealized model to be several times 10 -4M ⊙, which is slightly larger than the value deduced from observations. More realistic calculations that relax the assumptions of a homogenous bubble and constant-power jets' composition might lead to agreement with observations.
AB - We calculate the nucleosynthesis inside the hot bubble formed in the jittering-jets model for core-collapse supernova explosions, and find the formation of several times 10 -4M ⊙ r-process elements. In the jittering-jets model, fast jets launched from a stochastic accretion disc around the newly formed neutron star are shocked at several thousand km, and form hot high-pressure bubbles. These bubbles merge to form a large bubble that explodes the star. In this study, we assume a spherically symmetric homogenous bubble, and follow its evolution for about 1 s during which nuclear reactions take place. The jets last for about 1 s, their velocity v j= 0.5c, and their total energy is ∼10 51erg. We use jets' neutron enrichment independent of time, and follow the nuclear reactions to the formation of seed nuclei up to Z≤ 50, on which more neutrons will be absorbed to form r-process elements. Based on the mass of the seed nuclei, we find the r-process element mass in our idealized model to be several times 10 -4M ⊙, which is slightly larger than the value deduced from observations. More realistic calculations that relax the assumptions of a homogenous bubble and constant-power jets' composition might lead to agreement with observations.
KW - Nuclear reactions, nucleosynthesis, abundances
KW - Supernovae: general
UR - http://www.scopus.com/inward/record.url?scp=84859619546&partnerID=8YFLogxK
U2 - 10.1111/j.1365-2966.2011.20284.x
DO - 10.1111/j.1365-2966.2011.20284.x
M3 - 文章
AN - SCOPUS:84859619546
VL - 421
SP - 2763
EP - 2768
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 4
ER -