Radiation Transport Simulations of Pulsational Pair-Instability Supernovae
Ke-Jung (Ken) Chen1*
1IAA, Academia Sinica, Taipei, Taiwan
* Presenter:Ke-Jung (Ken) Chen, email:chenken1229@gmail.com
Massive stars of helium cores in the range of 35 to 65 solar masses (Ms) eventually encounters the electron/positron pair-instability repeatedly and the resulting Carbon or Oxygen burning can produce several thermonuclear eruptions.
In case of energetic events, one single burst may carry about 10$^{50}$ erg and can easily ejects several solar masses of material from hydrogen envelope. A catastrophe collisions of ejected shells sometimes produce very luminous transients.
Previous 2D studies of these events show that the development of a Rayleigh-Taylor instability and drives mixing between the shells. Here, I will present the radiation hydrodynamical simulations of pulsational pair-instability supernova of a 110 Ms solar-metallicity star that was shown in our earlier work to produce a superluminous supernova. Our comprehensive results contain 1D, 2D, and 3D models. I will discuss the impact of dimensionity and fluid instabilities to the light curves for observational predication.

Keywords: Supernovae, Radiation Hydro , Fluid Instability