Convective Instability in Hot Bubble in a Delayed Supernova Explosion

Nucleosynthesis in the Hot Convective Bubble in Core-Collapse Supernovae

As an explosion develops in the collapsed core of a massive star, neutrino emission drives convection in a hot bubble of radiation, nucleons, and pairs just outside a proto-neutron star. Shortly thereafter, neutrinos drive a wind-like outflow from the neutron star. In both the convective bubble and the early wind, weak interactions temporarily cause a proton excess (Ye >∼0.50) to develop in the...

Matter Mixing in Axisymmetric Supernova Explosion

Growth of Rayleigh-Taylor (R-T) instabilities under the axisymmetric explosion are investigated by two-dimensional hydrodynamical calculations. The degree of the axisymmetric explosion and amplitude of the initial perturbation are varied parametrically to find the most favorable parameter for reproducing the observed line profile of heavy elements. It is found that spherical explosion can not p...

Convective Bubble Growth

Shake a bottle of champagne and pop it open. The champagne will shoot out in a mini-eruption. Do the same to a bottle of beer. Beer will ooze out more slowly. If a bottle of champagne or beer is opened without perturbation, there will be no eruption, but bubbles will rise and grow, often in regularly spaced “trains” (FIG. 1). In Guinness beer, bubbles rise more slowly and may even sink. The myr...

J an 2 01 0 Supernova 2007 bi was a pair - instability explosion

Flavor oscillations in the supernova hot bubble region: nonlinear effects of neutrino background.

The neutrino flux close to a supernova core contributes substantially to neutrino refraction so that flavor oscillations become a nonlinear phenomenon. One unexpected consequence is efficient flavor transformation for antineutrinos in a region where only neutrinos encounter a Mikheyev-Smirnov-Wolfenstein resonance or vice versa. Contrary to previous studies we find that in the neutrino-driven w...