In this Letter, we present the result of an axisymmetric CCSN simulation conducted with appropriate treatments of neutrino transport and proper motions of proto-neutron star (PNS), in which a remarkable PNS acceleration is observed in association with asymmetric neutrino emissions by the time of 300ms after bounce. We find that these asymmetric neutrino emissions play important roles in the acceleration of PNS in this phase. The correlation between the PNS proper motion and the asymmetric ejecta is similar to that in the neutron star (NS) kick of hydrodynamic origin. Both electron-type neutrinos (νe) and their anti-particles (¯ νe) have ∼ 10% level of asymmetry between the northern and southern hemispheres, while other heavy-leptonic neutrinos (νx) have much smaller asymmetry of ∼ 1%. The emissions of ν¯e and νx are higher in the hemisphere of stronger shock expansion whereas the νe emission is enhanced in the opposite hemisphere: in total the neutrinos carry some linear momentum to the hemisphere of the stronger shock expansion. The asymmetry is attributed to the non-spherical distribution of electron-fraction (Ye) in the envelope of PNS. Although it is similar to LESA (lepton-emission self-sustained asymmetry), the Ye asymmetry seems to be associated with the PNS motion: the latter triggers lateral circular motions in the envelope of PNS by breaking symmetry of the matter distribution there, which are then sustained by a combination of convection, lateral neutrino diffusion and matter-pressure gradient. Our findings may have an influence on the current theories on the NS kick mechanism although long-term simulations are required to assess their impact on the later evolution.
|Publication status||Published - 2019 Jul 10|
- Radiative transfer
- Supernovae: general
ASJC Scopus subject areas