Pair-Instability Supernovae, Gravity Waves, and Gamma-Ray Transients

摘要: Growing evidence suggests that the first generation of stars may have been quite massive (~100-300 M☉). If they retain their high mass until death, such will, after about 3 Myr, make pair-instability supernovae. Models for these explosions discussed in literature four decades, but very few included effects rotation and none employed a realistic model neutrino trapping transport. Both turn out to be important, especially those whose cores collapse into black holes (helium above 133 We consider complete evolution two zero-metallicity 250 300 M☉. Despite large masses, we argue low metallicities imply negligible loss. Evolving with no loss, including angular momentum transport rotationally induced mixing, produce helium 130 180 Products central burning (e.g., primary nitrogen) are mixed hydrogen envelope dramatic on radius, case M☉ model. Explosive oxygen silicon cause core (250 star) explode, explosive is unable drive an explosion core, it collapses hole. For this star, calculated presupernova sufficient delay hole formation, star initially forms ~50 M☉, 1000 km within which neutrinos trapped. The growth time secular rotational instabilities shorter than formation time, develop. so, estimated gravitational wave energy amplitude EGW ≈ 10-3 c2 h+ 10-21/d(Gpc), estimates rough depend sensitively nonlinear nature instabilities. After forms, accretion continues through disk. disk depends adopted viscosity large, up 30 when 140 rate can as 1-10 s-1. Although far too cool efficiently axis by annihilation, has ample potential 1054 erg jet driven magnetic fields. interaction surrounding circumstellar gas energetic gamma-ray transient, given probable redshift consequent timescale spectrum, difficulty explaining typical bursts.