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Carbon-oxygen white dwarfs contain neon-22 formed from alpha-captures ontonitrogen during core He burning in the progenitor star. In a white dwarf (typeIa) supernova, the neon-22 abundance determines, in part, the neutron-to-protonratio and hence the abundance of radioactive nickel-56 that powers thelightcurve. The neon-22 abundance also changes the burning rate and hence thelaminar flame speed. We tabulate the flame speedup for different initial carbonand neon-22 abundances and for a range of densities. This increase in thelaminar flame speed--about 30% for a neon-22 mass fraction of 6%--affects thedeflagration just after ignition near the center of the white dwarf, where thelaminar speed of the flame dominates over the buoyant rise, and in regions oflower density ~ 10^7 g/cm3 where a transition to distributed burning isconjectured to occur. The increase in flame speed will decrease the density ofany transition to distributed burning.

The Laminar Flame Speedup by 22 Ne Enrichment in White Dwarf Supernovae

The Laminar Flame Speedup by ²² Ne Enrichment in White Dwarf Supernovae