Galactic Positrons from Thermonuclear Supernovae

Type Ia Supernovae (SNe Ia) may originate from a wide variety of explosion scenarios and progenitor channels. They exhibit factor about 10 difference in brightness and, thus, differentiation the mass 56Ni->56Co->56 Fe. We present study on fate positrons within SNe order to evaluate their escape fractions energy spectra. Our detailed Monte Carlo transport simulations for gamma-rays include both beta + decay 56 Co pair production. simulate scenarios, including white dwarfs (WD) close Chandrasekhar mass, M(Ch), He-triggered explosions sub-M Ch WDs, dynamical mergers two WDs. For each model, we influence size morphology magnetic field between 1 1E13 G. Population synthesis based observed distribution was used estimate overall contributions Galactic due SN Ia. find that this is dominated by normal-bright Ia, where variations emitted are small. total contribution < 2% depending morphology, less than 6...20% M(Ch) sub-M(Ch), respectively.