no code implementations • 24 Dec 2020 • Akihiro Suzuki, Matt Nicholl, Takashi J. Moriya, Tomoya Takiwaki
We suggest that the pulsational pair-instability SNe may provide a natural explanation for the massive CSM and the energetic explosion.
High Energy Astrophysical Phenomena
no code implementations • 24 Dec 2020 • Takashi Yoshida, Tomoya Takiwaki, Kei Kotake, Koh Takahashi, Ko Nakamura, Hideyuki Umeda
Our 3D results show that turbulent mixing occurs in both of the progenitors with the angle-averaged turbulent Mach number exceeding $\sim$ 0. 1 at the maximum.
Solar and Stellar Astrophysics High Energy Astrophysical Phenomena
1 code implementation • 5 Nov 2019 • Sajad Abbar, Huaiyu Duan, Kohsuke Sumiyoshi, Tomoya Takiwaki, Maria Cristina Volpe
Although the $11. 2\mathrm{M}_{\odot}$ model features $\nu_e - \bar\nu_e$ angular crossings and the associated fast modes at different time snapshots, the $27\mathrm{M}_{\odot}$ model does not show any crossings within the decoupling region.
High Energy Astrophysical Phenomena High Energy Physics - Theory
1 code implementation • 1 Jul 2019 • Hirokazu Sasaki, Tomoya Takiwaki, Shio Kawagoe, Shunsaku Horiuchi, Koji Ishidoshiro
We also show that if the spectrum of $\bar{\nu}_e$ in HK becomes softer due to CNO, the spectrum of $\nu_e$ in DUNE becomes harder, and vice versa.
High Energy Astrophysical Phenomena High Energy Physics - Phenomenology
1 code implementation • 30 Sep 2018 • Hajime Kawahara, Takami Kuroda, Tomoya Takiwaki, Kazuhiro Hayama, Kei Kotake
We demonstrate that the polarization states that randomly change with time after bounce are associated with the PNS g-mode oscillation, whereas a slowly changing polarization state in the low-frequency domain is connected to the PNS core oscillation.
High Energy Astrophysical Phenomena Instrumentation and Methods for Astrophysics General Relativity and Quantum Cosmology
