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Thermonuclear supernovae originating from the explosion of a white dwarfaccreting mass from a companion star have been suggested as a site for theproduction of $p$ nuclides. Such nuclei are produced during the explosion, inlayers enriched with seed nuclei coming from prior strong $s$ processing. Theseseeds are transformed to proton-richer isotopes mainly by photodisintegrationreactions. Several thousand trajectories from a 2D explosion model were used ina Monte Carlo approach. Temperature-dependent uncertainties were assignedindividually to thousands of rates varied simultaneously in post-processing inan extended nuclear reaction network. The uncertainties in the final nuclearabundances originating from uncertainties in the astrophysical reaction rateswere determined. In addition to the 35 classical $p$ nuclides, abundanceuncertainties 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 Evolutionstudies. Uncertainties found were generally lower than a factor of two,although most nucleosynthesis flows mainly involve predicted rates with largeruncertainties. The main contribution to the total uncertainties comes from agroup of trajectories with high peak density originating from the interior ofthe exploding white dwarf. The distinction between low-density and high-densitytrajectories allows more general conclusions to be drawn, also applicable toother simulations of white dwarf explosions.

Uncertainties in the production of p nuclides in thermonuclear supernovae determined by Monte Carlo variations