TYPE Ia SUPERNOVAE AS SITES OF THE p -PROCESS: TWO-DIMENSIONAL MODELS COUPLED TO NUCLEOSYNTHESIS

Beyond Fe, there is a class of 35 proton-rich nuclides, between 74 Se and 196 Hg, called p -nuclei. They are bypassed by the s and r neutron capture processes and are typically 10–1000 times less abundant than the s - and/or r -isotopes in the solar system. The bulk of p -isotopes is created in the "gamma processes" by sequences of photodisintegrations and beta decays in explosive conditions in both core collapse supernovae (SNe II) and in Type Ia supernovae (SNe Ia). SNe II contribute to the production of p -nuclei through explosive neon and oxygen burning. However, the major problem in SN II ejecta is a general underproduction of the light p -nuclei for A < 120. We explore SNe Ia as p -process sites in the framework of a two-dimensional SN Ia delayed detonation model as well as pure deflagration models. The white dwarf precursor is assumed to have reached the Chandrasekhar mass in a binary system by mass accretion from a giant/main-sequence companion. We use enhanced s -seed distributions, with seeds directly obtained from a sequence of thermal pulse instabilities both in the asymptotic giant branch phase and in the accreted material. We apply the tracer-particle method to reconstruct the nucleosynthesis by the thermal histories of Lagrangian particles, passively advected in the hydrodynamic calculations. For each particle, we follow the explosive nucleosynthesis with a detailed nuclear reaction network for all isotopes up to 209 Bi. We select tracers within the typical temperature range for p -process production, (1.5–3.7) × 10 9 K, and analyze in detail their behavior, exploring the influence of different s -process distributions on the p -process nucleosynthesis. In addition, we discuss the sensitivity of p -process production to parameters of the explosion mechanism, taking into account the consequences on Fe and alpha elements. We find that SNe Ia can produce a large amount of p -nuclei, both the light p -nuclei below A = 120 and the heavy- p nuclei, at quite flat average production factors, tightly related to the s -process seed distribution. For the first time, we find a stellar source able to produce both light and heavy p -nuclei almost at the same level as 56 Fe, including the debated neutron magic 92, 94 Mo and 96, 98 Ru. We also find that there is an important contribution from the p -process nucleosynthesis to the s -only nuclei 80 Kr, 86 Sr, to the neutron magic 90 Zr, and to the neutron-rich 96 Zr. Finally, we investigate the metallicity effect on p -process production in our models. Starting with different s -process seed distributions for two metallicities Z = 0.02 and Z = 0.001, running two-dimensional SN Ia models with different initial composition, we estimate that SNe Ia can contribute to at least 50% of the solar p -process composition. A more detailed analysis of the role of SNe Ia in Galactic chemical evolution of p -nuclei is in preparation.