Production of high-energy μneutrinos from young neutron stars
| dc.creator | Burgio, G. F. | |
| dc.creator | Link, B. | |
| dc.date | 2006-09-20 | |
| dc.date.accessioned | 2026-07-07T11:04:12Z | |
| dc.date.available | 2026-07-07T11:04:12Z | |
| dc.description | Young, rapidly rotating neutron stars could accelerate protons to energies of $\sim 1$ PeV close to the stellar surface, which scatter with x-rays from the stellar surface through the $Δ$ resonance and produce pions. The pions subsequently decay to produce muon neutrinos. We find that the energy spectrum of muon neutrinos consists of a sharp rise at $\sim 50$ TeV, corresponding to the onset of the resonance, above which the flux drops as $ε_ν^{-2}$ up to an upper-energy cut-off that is determined by either kinematics or by the maximum energy to which protons are accelerated. We predict event rates as high as 10-50 km$^{-2}$ yr$^{-1}$ from relatively young, close neutron stars. Such fluxes would be detectable by IceCube. | |
| dc.description | 6 pages, 2 figures, to be published in the proceedings of the CRIS 2006 conference, Catania, Italy, May 29 - June 2, 2006 | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0609561 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0609561 | |
| dc.identifier | Nucl.Phys.Proc.Suppl.165:231-236,2007 | |
| dc.identifier | doi:10.1016/j.nuclphysbps.2006.11.030 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/188808 | |
| dc.subject | Astrophysics | |
| dc.title | Production of high-energy μneutrinos from young neutron stars | |
| dc.type | text |