"Neutrino halo effect on collective neutrino oscillation in iron core-collapse supernova model of a 9.6 M⊙ star"

Masamichi Zaizen, John F. Cherry, Tomoya Takiwaki, Shunsaku Horiuchi, Kei Kotake, Hideyuki Umeda, and Takashi Yoshida
arXiv:1908.10594

These animations show the time evolution of matter profile and halo contribution in Fig.4. They illustrate the development of inward contribution in self-interaction Hamiltonian with shock expanding. The non-negligible contribution violates the availability of the bulb+halo model.
Left: Matter density Right: Halo contribution, which is the ratio of \( H^{\mathrm{in}}_{\nu\nu} \) to \( H^{\mathrm{out}}_{\nu\nu} \)
\( t_{\mathrm{pb}} \): Post-bounce time