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We calculate the neutrino signal from Population III supermassive star collapse using a neutrino transfer code originally developed for core collapse supernovae and massive star collapse. Using this code, we are able to investigate the supermassive star mass range thought to undergo neutrino trapping ($sim 10^4$ M$_odot$), a mass range which has been neglected by previous works because of the difficulty of neutrino transfer. For models in this mass range, we observe a neutrino-sphere with a large radius and low density compared to typical massive star neutrino-spheres. We calculate the neutrino light-curve emitted from this neutrino-sphere. The resulting neutrino luminosity is significantly lower than the results of a previous analytical model. We briefly discuss the possibility of detecting a neutrino burst from a supermassive star or the neutrino background from many supermassive stars and conclude that the former is unlikely with current technology, unless the SMS collapse is located as close as 1 Mpc, while the latter is also unlikely even under very generous assumptions. However, the supermassive star neutrino background is still of interest as it may serve as a source of noise in proposed dark matter direct detection experiments.
We investigate the possibility of a supernova in supermassive ($5 times 10^4 ;M_odot$) population III stars induced by a general relativistic instability occurring in the helium burning phase. This explosion could occur via rapid helium burning durin
Supermassive primordial stars forming in atomically-cooled halos at $z sim15-20$ are currently thought to be the progenitors of the earliest quasars in the Universe. In this picture, the star evolves under accretion rates of $0.1 - 1$ $M_odot$ yr$^{-
Supermassive black holes observed at high redshift $zgtrsim6$ could grow from direct collapse black holes (DCBHs) with mass $sim10^5,M_{odot}$, which result from the collapse of supermassive stars (SMSs). If a relativistic jet is launched from a DCBH
The formation of supermassive Population III stars with masses $gtrsim$ 10,000 Msun in primeval galaxies in strong UV backgrounds at $z sim$ 15 may be the most viable pathway to the formation of supermassive black holes by $z sim$ 7. Most of these st
In the case of zero-metal (population III or Pop III) stars, we show that the total mass of binary black holes from binary Pop III star evolution can be $sim 150 ,M_{odot}$, which agrees with the mass of the binary black hole GW190521 recently discov