High Energy Neutrino Emission from the Earliest Gamma-Ray Bursts

TL;DR

This paper models high energy neutrino emissions from the earliest gamma-ray bursts caused by Population III stars, predicting detectable signals that can inform us about early universe conditions and stellar progenitors.

Contribution

It provides the first detailed calculations of neutrino fluxes from Population III gamma-ray bursts, linking neutrino signals to progenitor mass and early cosmic environment.

Findings

Detectable neutrino fluxes in the 1-300 PeV range with current detectors.

Neutrino signals depend on black hole mass and surrounding gas density.

Potential to probe early star formation and cosmological conditions.

Abstract

We discuss the high energy neutrino emission from gamma-ray bursts resulting from the earliest generation (`population III') stars forming in the Universe, whose core collapses into a black hole. These gamma-ray bursts are expected to produce a highly relativistic, magnetically dominated jet, where protons can be accelerated to ultra-high energies. These interact with the photons produced by the jet, leading to ultra-high energy photo-meson neutrinos as well as secondary leptons and photons. The photon luminosity and the shock properties, and thus the neutrino spectrum, depend on the mass of the black holes as well as on the density of the surrounding external gas. We calculate the individual source neutrino spectral fluxes and the expected diffuse neutrino flux for various source parameters and evolution scenarios. Both the individual and diffuse signals appear detectable in the 1-300 PeV range with current and planned neutrino detectors such as IceCube and ARIANNA, provided the black hole mass is in excess of 30-100 solar masses. This provides a possible test for the debated mass of the progenitor stellar objects, as well as a probe for the early cosmological environment and the formation rate of the earliest structures.