Journal Article

Nucleosynthesis of r‐process elements by jittering jets in core‐collapse supernovae

Oded Papish and Noam Soker

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 421, issue 4, pages 2763-2768
Published in print April 2012 | ISSN: 0035-8711
Published online April 2012 | e-ISSN: 1365-2966 | DOI:
Nucleosynthesis of r‐process elements by jittering jets in core‐collapse supernovae

Show Summary Details


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 10−4 M 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 vj= 0.5c, and their total energy is ∼1051 erg. 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 10−4 M, 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.

Keywords: nuclear reactions, nucleosynthesis, abundances; supernovae: general

Journal Article.  4343 words.  Illustrated.

Subjects: Astronomy and Astrophysics

Full text: subscription required

How to subscribe Recommend to my Librarian

Users without a subscription are not able to see the full content. Please, subscribe or login to access all content.