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Gas Dynamics of the Nickel-56 Decay Heating in Pair-Instability Supernovae
Ke-Jung Chen, S. E. Woosley, Daniel J. Whalen
Very massive 140-260 Msun stars can die as highly-energetic pair-instability supernovae (PI SNe) with energies of up to 100 times those of core-collapse SNe that can completely des…
Three-Dimensional Simulations of Magnetar-Powered Superluminous Supernovae
Ke-Jung Chen, S. E. Woosley, Daniel J. Whalen
A rapidly spinning magnetar in a young supernova (SN) can produce a superluminous transient by converting a fraction of its rotational energy into radiation. Here, we present the f…
Multidimensional Radiation Hydrodynamics Simulations of Pulsational Pair-Instability Supernovae
Ke-Jung Chen, Daniel J. Whalen, S. E. Woosley +1
Stars with masses of 80 - 130 Msun can encounter the pulsational pair-instability at the end of their lives, which triggers consecutive episodes of explosive burning that eject mul…