Sign up for the Get the most important science stories of the day, free in your inbox. Scannapieco, E., Madau, P., Woosley, S. E., Heger, A. In Vink, J. S. & de Koter, A. To obtain The 1961 Supernova-like events SN 1961V and SN 2010dn are believed to be the potential supernova impostors involving a massive LBVs (Luminous Blue Variables) and could have been pair-instability pulsations, as could the repeating events at iPTF14hls. In Leung et al. In some of these events, solar masses of material are ejected in repeated outbursts of several ﾃ・1050erg each. Internet Explorer). Smith, N. & Owocki, S. P. On the role of continuum-driven eruptions in the evolution of very massive stars and population III stars. Figer, D. F. An upper limit to the masses of stars. Pair-instability supernovae are popularly thought to be highly luminous. The detectability of pair-production supernovae at z < 6. Kudritzki, R. P. Line-driven winds, ionizing fluxes, and ultraviolet spectra of hot stars at extremely low metallicity. The table presents a summary of results for other similar mass stars with highly variable explosion properties. On the metallicity dependence of Wolf-Rayet wind. You can also search for this author in Barkat, Z., Rakavy, G. & Sack, N. Dynamics of supernova explosions resulting from pair formation. the best experience, we recommend you use a more up to date browser (or turn off compatibility mode in & Weaver, T. 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. This ‘pair instability’ leads to explosive burning that is insufficient to unbind the star, but ejects many solar masses of the envelope. 2006jc: a Wolf-Rayet star exploding in a dense He-rich circumstellar medium. and JavaScript.Get time limited or full article access on ReadCube.Smith, N. et al. Woosley, S. E. Gamma-ray bursts from stellar mass accretion disks around black holes. This leads the star to become dynamically unstable and leads to the collapse then explosion of these stars. 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 … Pulsational pair-instability supernovae are likely the most common pair-instability events and are probably common causes of supernova impostor events. Simon Portegies Zwart and Edward van den Heuvel show that the collision frequency of massive stars in a dense young cluster is sufficient to cause an explosion of the scale of SN 2006gy. Massive stars that end their lives with helium cores in the range of 35窶・5Mare known to produce repeated thermonuclear outbursts due to a recurring pair-instability. 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. This is only the case for the most massive progenitors since the luminosity depends strongly on the ejected mass of radioactive Ni. & Ferrara, A. 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 … Two groups now present evidence to support alternative explanations for this supernova, both involving collision. Mass loss rates in the Hertzsprung-Russell diagram. (PDF 333 kb)Woosley, S., Blinnikov, S. & Heger, A. Pulsational pair instability as an explanation for the most luminous supernovae.
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