Diffuse emission of TeV Neutrinos and Gamma-rays from young pulsars by Photo-meson interaction in the galaxy

TL;DR

This paper models the production of TeV neutrinos and gamma-rays from young pulsars via photo-meson interactions, finding that the diffuse neutrino flux is too low for current detection capabilities.

Contribution

It introduces a Monte Carlo simulation of young pulsars to estimate their TeV neutrino and gamma-ray emissions through proton-photon interactions, a novel approach in this context.

Findings

Diffuse TeV neutrino flux is below current detection thresholds.

Neutrino production is limited by the low interaction probability.

Gamma-ray flux from pulsars is also predicted to be weak.

Abstract

It's generally believed that young and rapidly rotating pulsars are important sites of particle's acceleration, in which protons can be accelerated to relativistic energy above the polar cap region if the magnetic moment is antiparallel to the spin axis($\vec{\mu}\cdot\vec{\Omega}<0$). To obtain the galactic diffusive neutrinos and gamma-rays for TeV, firstly,we use Monte Carlo(MC) method to generate a sample of young pulsars with ages less than $10^6$ yrs in our galaxy ; secondly, the neutrinos and high-energy gamma-rays can be produced through photomeson process with the interaction of energetic protons and soft X-ray photons ($p+\gamma\rightarrow \Delta^+\rightarrow n+\pi^+/p+\pi^0$) for single pulsar, and these X-ray photons come from the neutron star surface. The results suggest that the diffusive TeV flux of neutrinos are lower than background flux, which indicated it is difficult to be detected by the current neutrino telescopes.