dc.contributor.author | Nishimura, N. | |
dc.contributor.author | Rauscher, T. | |
dc.contributor.author | Hirschi, R. | |
dc.contributor.author | Murphy, A. St J. | |
dc.contributor.author | Cescutti, G. | |
dc.contributor.author | Travaglio, C. | |
dc.date.accessioned | 2018-09-12T00:12:40Z | |
dc.date.available | 2018-09-12T00:12:40Z | |
dc.date.issued | 2018-03-01 | |
dc.identifier.citation | Nishimura , N , Rauscher , T , Hirschi , R , Murphy , A S J , Cescutti , G & Travaglio , C 2018 , ' Uncertainties in the production of p nuclides in thermonuclear supernovae determined by Monte Carlo variations ' , Monthly Notices of the Royal Astronomical Society , vol. 474 , no. 3 , pp. 3133-3139 . https://doi.org/10.1093/mnras/stx3033 | |
dc.identifier.issn | 0035-8711 | |
dc.identifier.uri | http://www.scopus.com/inward/record.url?scp=85040256073&partnerID=8YFLogxK | |
dc.description | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society. © 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. | |
dc.description.abstract | Thermonuclear supernovae originating from the explosion of a white dwarf accreting mass from a companion star have been suggested as a site for the production of p nuclides. Such nuclei are produced during the explosion, in layers enriched with seed nuclei coming from prior strong s processing. These seeds are transformed into proton-richer isotopes mainly by photodisintegration reactions. Several thousand trajectories from a 2D explosion model were used in a Monte Carlo approach. Temperature-dependent uncertainties were assigned individually to thousands of rates varied simultaneously in post-processing in an extended nuclear reaction network. The uncertainties in the final nuclear abundances originating from uncertainties in the astrophysical reaction rates were determined. In addition to the 35 classical p nuclides, abundance uncertainties were also determined for the radioactive nuclides 92Nb, 97, 98Tc, 146Sm, and for the abundance ratios Y(92Mo)/Y(94Mo), Y(92Nb)/Y(92Mo), Y(97Tc)/Y(98Ru), Y(98Tc)/Y(98Ru), and Y(146Sm)/Y(144Sm), important for Galactic Chemical Evolution studies. Uncertainties found were generally lower than a factor of 2, although most nucleosynthesis flows mainly involve predicted rates with larger uncertainties. The main contribution to the total uncertainties comes from a group of trajectories with high peak density originating from the interior of the exploding white dwarf. The distinction between low-density and high-density trajectories allows more general conclusions to be drawn, also applicable to other simulations of white dwarf explosions. | en |
dc.format.extent | 7 | |
dc.format.extent | 1638368 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | |
dc.subject | Abundances | |
dc.subject | Nuclear reactions | |
dc.subject | Nucleosynthesis | |
dc.subject | Stars: abundances | |
dc.subject | Supernovae: general | |
dc.subject | Astronomy and Astrophysics | |
dc.subject | Space and Planetary Science | |
dc.title | Uncertainties in the production of p nuclides in thermonuclear supernovae determined by Monte Carlo variations | en |
dc.contributor.institution | Centre for Astrophysics Research (CAR) | |
dc.contributor.institution | School of Physics, Astronomy and Mathematics | |
dc.description.status | Peer reviewed | |
dc.identifier.url | http://www.scopus.com/inward/record.url?scp=85040256073&partnerID=8YFLogxK | |
rioxxterms.versionofrecord | 10.1093/mnras/stx3033 | |
rioxxterms.type | Journal Article/Review | |
herts.preservation.rarelyaccessed | true | |