2013/02/05 by Isaac Saba, J. Becker Tjus, Julia Becker Tjus +2 · 9 citations
Physics and Astronomy · #Active galactic nucleus #Astrophysics #Astrophysics and Cosmic Phenomena #Centaurus A #Cosmic ray #Dark Matter and Cosmic Phenomena #Electron #Fermi Gamma-ray Space Telescope #Flux (metallurgy) #Galaxy #Neutrino #Neutrino Physics Research #Neutrino detector #Neutrino oscillation #Nuclear physics #Physics #Proton #astro-ph.HE
paper · pdf · doi:10.1016/j.astropartphys.2013.06.009
published in Astroparticle Physics 48, 30-36 (Elsevier BV)
arxiv created 2013/02/05 · openalex publication_date 2013/07/01 · arxiv updated 2015/06/12 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Active galactic nuclei (AGN) are believed to be the source of ultra high energy cosmic rays (UHECRs). Particles are assumed to be accelerated in the accretion disk and the plasma jets, produced due to conservation of angular momentum, to the highest energies, where they interact with each other and produce pions, which decay among others in neutrinos. For a known cosmic ray spectral behavior, the main parameters in the calcula- tion of the neutrino flux from proton-proton interactions are the target density nH and the ratio of electrons to protons fe . Using most recent neutrino flux limits from IceCube point source searches, we set limits on the target densities for 33 FR-I galaxies. The densities are shown to be smaller than 30 cm-3 to 2000 cm-3, depending on the source and when using a fixed electron to proton ratio of fe = 0.1. This implies that some cosmic ray acceleration sites, espe- cially those close to the core of the AGN, can already be excluded, or else that the ratio of electrons to protons deviates significantly from the commonly used value of 0.1. For Centaurus A (Cen A) and Messier 87 (M 87) we use Fermi observations to model the γ-flux, the neutrino flux and the resulting target density. The detec- tion of these neutrinos will help to find information about acceleration processes in the source.