Speaker
Description
Although there is broad agreement that Type Ia Supernovae (SNe Ia) originate from thermonuclear explosions of carbon-oxygen white dwarf stars (WD), the details of the path towards explosion remain uncertain: the degeneracy of the binary system, mass, and chemical composition of the WD, and the explosion mechanism of the SNe Ia. Using the reaction rates in STARLIB [1] we probe the sensitivities of nuclear reactions responsible for the abundance of potential observables in hopes to shed light on some of these uncertainties. This is done by employing a Monte Carlo reaction network method [2] by varying all reaction rates simultaneously according to their rate probability densities in each simulation. The hydrodynamical trajectories were derived from a near-M$_{Ch}$ WD shell model with a 5 x 10$^{-4}$ M He layer surrounding its carbon oxygen core [3]. To take advantage of future early time observations, we focus on both early-time (e.g. gamma ray emitters) and late-time observables (e.g. elemental abundances in ejecta, supernova remnants). Results will be discussed.
*This work is supported by the DOE, Office of Science, Office of Nuclear Physics, under Grants No. DE-FG02-97ER41041 (UNC) and No. DE-FG02-97ER41033 (TUNL).
References
[1] A. L. Sallaska et al. ApJS 207 18 (2013)
[2] C. Iliadis et al. J Phys. G 42, 034007 (2015)
[3] Hoeflich, P. et al. Nuclei in the Cosmos XV. Springer Proceedings in Physics, 219 (2019)
