Abstract
High energy neutrinos can arise from a variety of processes. Interactions of ultra high energy cosmic rays with radiation and matter lead to secondary particles, some of which create neutrinos. Interactions of the 2.7 K CMB radiation with protons gives rise to pions and neutrons, and neutrons produced in the photodisintegration of heavy nuclei are also a source of neutrinos. There is speculation that super-heavy relic particles with masses of ~1021 eV are created in the early Universe: if such particles exist then their decay channels are expected to contain neutrinos. The different sources of neutrinos are summarised. High energy neutrinos can be detected through the extensive air showers that they create in the atmosphere and the potential of the Pierre Auger Observatory, now nearing completion, and of the planned EUSO and ASHRA instruments, to detect neutrino-induced air showers, will be described.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
