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Nomoto, K., Tominaga, N., Tanaka, M., Maeda, K. & Umeda, H. Nucleosynthesis in core-collapse supernovae and GRB-metal-poor star connection. And Woosley Neutrino Signals from Pulsations and their Detection by Terrestrial Neutrino Detectors - NASA/ADS A Pulsational Pair-instability supernova (PPISN) evolves from a massive star with a mass $\sim 80$ -- 140 $M_{\odot}$ which develops the electron-positron pair-instability … Mass loss rates in the Hertzsprung-Russell diagram. The evolution and fate of very massive objects. & Blondin, J. M. Hydrodynamic instabilities in supernova remnants: early radiative cooling. Internet Explorer).

Two groups now present evidence to support alternative explanations for this supernova, both involving collision.

Foley, R. J. et al. (PDF 333 kb)Woosley, S., Blinnikov, S. & Heger, A. Pulsational pair instability as an explanation for the most luminous supernovae. At zero metallicity, stars with a mass 100 – 140 solar mass (or He core from 40 – 64 solar mass) forms the pulsational pair-instability SN Recent progress (in 1D) Woosley (2017) has presented the first systematic study of PPISN using the Kepler code, the pulsation … MacFadyen, A. I. This leads the star to become dynamically unstable and leads to the collapse then explosion of these stars. In Heger, A., Woosley, S. E. & Spruit, H. Presupernova evolution ofdifferentially rotating massive stars including magnetic fields.

Pressure nonetheless increases, but in a pair-instability collapse, the increase in pressure is not enough to resist the increase in gravitational forces as the star becomes denser. Vink, J. S. & de Koter, A.

Depending on the nature of the progenitor star they may take the appearance of either a type II, type Ib or type Ic supernova.

The sudden heating and compression of the core generates gamma rays energetic enough to be converted into an avalanche of electron-positron pairs, further reducing the pressure. In Leung et al. To obtain Possible examples of pulsational pair-instability supernovae include the 1843 eruption of Eta Carinae A, and possibly SN 1000+0216 which could have been either a pulsational pair-instability supernova or a supernova of pair-instability.

& Ferrara, A. Blinnikov, S. I. et al.

This work was supported by the Scientific Discovery through Advanced Computing (SciDAC) Program of the US Department of Energy, by NASA, and by the Russian Foundation for Basic Research and Science Schools. You are using a browser version with limited support for CSS.

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A Pulsational Pair-instability supernova (PPISN) evolves from a massive star with a mass ~80–140 M⊙ that develops electron–positron pair-instability after hydrostatic He-burning in the core has finished. Pulsational pair-instability supernovae are likely the most common pair-instability events and are probably common causes of supernova impostor events. Pair-instability supernovae are popularly thought to be highly luminous. Woosley, S. E., Heger, A. Type IIn supernova 1994W: evidence for the explosive ejection of a circumstellar envelope.

Chevalier, R. A. The pulsations are stronger for more massive He cores and result in a large amount of mass ejection such as 3─13 M ☉for 40−62 M ☉He cores. The figures show the evolution of the composition through the two outbursts, the bolometric light curve of the two bursts, the multicolor photometry of models in which the density and explosion energy are varied, and other details of the emission.

The higher the temperature, the higher the gamma ray energies, and the larger the amount of energy transferred. Duncan, R. C. & Thompson, C. Formation of very strongly magnetized neutron stars—Implications for gamma-ray bursts.

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