Speaker
Description
Non-thermal electromagnetic radiation up to PeV gamma-rays from pulsar wind nebulae is powered by relativistic electron-positron plasma supplied by a central pulsar. The origin of the radio-emitting particles, however, remains unresolved because of their large number compared with that expected from pair cascades in the pulsar magnetosphere. A stochastic acceleration model has been proposed in which low-energy electrons responsible for the radio emission are injected from the supernova ejecta via photoionization and subsequently accelerated by turbulence in the nebula. The observed flat radio spectra are also consistent with this stochastic acceleration scenario. In this work we explore whether ions can be injected through the same process and accelerated together with the radio-emitting electrons. The accelerated ions produce high-energy neutrinos through hadronic interactions. We estimate the resulting neutrino spectra and discuss their detectability with next-generation neutrino telescopes, focusing on the Crab Nebula.
