dc.contributor.author | Eichler, M. | |
dc.contributor.author | Arcones, A. | |
dc.contributor.author | Kelic, A. | |
dc.contributor.author | Korobkin, O. | |
dc.contributor.author | Langanke, K. | |
dc.contributor.author | Marketin, T. | |
dc.contributor.author | Martinez-Pinedo, G. | |
dc.contributor.author | Panov, I. | |
dc.contributor.author | Rauscher, T. | |
dc.contributor.author | Rosswog, S. | |
dc.contributor.author | Winteler, C. | |
dc.contributor.author | Zinner, N. T. | |
dc.contributor.author | Thielemann, F. K. | |
dc.date.accessioned | 2015-09-07T11:28:44Z | |
dc.date.available | 2015-09-07T11:28:44Z | |
dc.date.issued | 2015-07-15 | |
dc.identifier.citation | Eichler , M , Arcones , A , Kelic , A , Korobkin , O , Langanke , K , Marketin , T , Martinez-Pinedo , G , Panov , I , Rauscher , T , Rosswog , S , Winteler , C , Zinner , N T & Thielemann , F K 2015 , ' The Role of Fission in Neutron Star Mergers and Its Impact on the r-Process Peaks ' , The Astrophysical Journal , vol. 808 , no. 1 , 30 . https://doi.org/10.1088/0004-637X/808/1/30 | |
dc.identifier.issn | 0004-637X | |
dc.identifier.uri | http://hdl.handle.net/2299/16381 | |
dc.description.abstract | Comparing observational abundance features with nucleosynthesis predictions of stellar evolution or explosion simulations, we can scrutinize two aspects: (a) the conditions in the astrophysical production site and (b) the quality of the nuclear physics input utilized. We test the abundance features of r-process nucleosynthesis calculations for the dynamical ejecta of neutron star merger simulations based on three different nuclear mass models: The Finite Range Droplet Model, the (quenched version of the) Extended Thomas Fermi Model with Strutinsky Integral, and the Hartree-Fock-Bogoliubov mass model. We make use of corresponding fission barrier heights and compare the impact of four different fission fragment distribution models on the final r-process abundance distribution. In particular, we explore the abundance distribution in the second r-process peak and the rare-earth sub-peak as a function of mass models and fission fragment distributions, as well as the origin of a shift in the third r-process peak position. The latter has been noticed in a number of merger nucleosynthesis predictions. We show that the shift occurs during the r-process freeze-out when neutron captures and β-decays compete and an (n,γ)-(γ,n) equilibrium is no longer maintained. During this phase neutrons originate mainly from fission of material above A = 240. We also investigate the role of β-decay half-lives from recent theoretical advances, which lead either to a smaller amount of fissioning nuclei during freeze-out or a faster (and thus earlier) release of fission neutrons, which can (partially) prevent this shift and has an impact on the second and rare-earth peak as well. | en |
dc.format.extent | 13 | |
dc.format.extent | 864178 | |
dc.language.iso | eng | |
dc.relation.ispartof | The Astrophysical Journal | |
dc.subject | abundancesstars: neutron | |
dc.subject | nuclear reactions | |
dc.subject | nucleosynthesis | |
dc.subject | Space and Planetary Science | |
dc.subject | Astronomy and Astrophysics | |
dc.title | The Role of Fission in Neutron Star Mergers and Its Impact on the r-Process Peaks | en |
dc.contributor.institution | Centre for Astrophysics Research (CAR) | |
dc.contributor.institution | School of Physics, Astronomy and Mathematics | |
dc.contributor.institution | Science & Technology Research Institute | |
dc.description.status | Peer reviewed | |
rioxxterms.versionofrecord | 10.1088/0004-637X/808/1/30 | |
rioxxterms.type | Journal Article/Review | |
herts.preservation.rarelyaccessed | true | |