| Title: | The Nature and Origin of Ultra-high Energy Cosmic Ray Particles |
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| Authors: | ID Biermann, P.L. (Author)
ID Lundquist, Jon Paul (Author), et al. |
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| Files: |  http://www.lnf.infn.it/sis/frascatiseries/Volume64/Volume64.pdf
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| Language: | English |
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| Work type: | Not categorized |
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| Typology: | 1.06 - Published Scientific Conference Contribution (invited lecture) |
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| Organization: | UNG - University of Nova Gorica
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| Abstract: | We outline two concepts to explain Ultra High Energy Cosmic Rays (UHECRs), one based on radio galaxies and their relativistic jets and terminal hot spots, and one based on relativistic Super-Novae (SNe) or Gamma Ray Bursts (GRBs) in starburst galaxies, one matching the arrival direction data in the South (the radio galaxy Cen A) and one in the North (the starburst galaxy M82). The most likely identification of the origin of observed Gravitational Wave (GW) events is stellar binary black hole (BH) mergers in starburst galaxies such as M82 with the highest rate of star formation, so the highest far-infrared (FIR) luminosity, at the edge of the universe visible in 10 - 300 Hz GWs; at low heavy element abundance Zch the formation of stellar BHs extends to a larger mass range. A radio galaxy such as Cen A sequence of events involves first the merger of two Super-Massive Black Holes (SMBHs), with the associated ejection of low frequency GWs, then the formation of a new relativistic jet aiming into a new direction: ubiquitous neutrino emission follows accompanied by compact TeV photon emission, detectable more easily if the direction is towards Earth. The ejection of UHECRs is last. Both these sites are the perfect high energy physics laboratory: We have observed particles up to ZeV, neutrinos up to PeV, photons up to TeV, 30 - 300 Hz GW events, and hope to detect soon of order µHz to mHz GW events. Energy turnover in single low frequency GW events may be of order ∼1063 erg. How can we further test these concepts? First of all by associating individual UHECR events, or directional groups of events, with chemical composition in both the Telescope Array (TA) Coll. and the Auger Coll. data. Second by identifying more TeV
to PeV neutrinos with recent SMBH mergers. Third by detecting the order < mHz GW events of SMBH binaries, and identifying the galaxies host to the stellar BH mergers and their GW events in the range up to 300 Hz. Fourth by finally detecting the formation of the first generation of SMBHs and their mergers, surely a spectacular discovery. |
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| Keywords: | UHECR, cosmic rays, anisotropy |
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| Publication version: | Version of Record |
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| Year of publishing: | 2016 |
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| Number of pages: | 19 |
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| Numbering: | 64, 64 |
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| PID: | 20.500.12556/RUNG-5175-49eedb19-9955-2718-a0c1-eec6d5f33a62  |
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| COBISS.SI-ID: | 13079043 |
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| NUK URN: | URN:SI:UNG:REP:R8TMBCJJ |
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| Publication date in RUNG: | 29.04.2020 |
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| Views: | 3107 |
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| Downloads: | 129 |
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