Uncertainties in the production of p nuclides in thermonuclear supernovae determined by Monte Carlo variations. Issue 3 (7th December 2017)

• Record Type: Journal Article
• Authors: Nishimura(西村信哉), N; Rauscher, T; Hirschi, R; Murphy, A St J; Cescutti, G; Travaglio, C
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 474:Issue 3(2018)
• Page Start: 3133
• Page End: 3139
• Publication Date: 2017-12-07
• Subjects: nuclear reactions, nucleosynthesis, abundances -- stars: abundances -- supernovae: general; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stx3033
• Languages: English
• ISSNs: 0035-8711

Abstract

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 92 Nb, 97, 98 Tc, 146 Sm, and for the abundance ratios Y ( 92 Mo)/ Y ( 94 Mo), Y ( 92 Nb)/ Y ( 92 Mo), Y ( 97 Tc)/ Y ( 98 Ru), Y ( 98 Tc)/ Y ( 98 Ru), and Y ( 146 Sm)/ Y ( 144 Sm), 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.