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HEP: Gamma-ray bursts: high-energy neutrino predictions in the IceCube era

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Mauricio Bustamante, Ohio State University
When
09 December 2015 from 2:30 PM to 3:30 PM
Where
339 Davey Laboratory
Contact Name
Kohta Murase
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Gamma-ray bursts (GRBs) --the short and luminous flashes associated to stellar mergers and deaths of massive stars-- naturally stand out as potential sources of high-energy neutrinos, on account of their compact sizes and associated high proton and photon densities. However, recent bounds from IceCube and theoretical considerations have constrained their contribution to the observed astrophysical neutrino diffuse flux to be subdominant. Regardless, they remain potential sites of ultra-high-energy cosmic ray (UHECR) production, and are arguably the best targets to search for a correlation between a high-energy electromagnetic signal and a neutrino signal. I will introduce well-motivated generalizations in the form of a model of joint prompt neutrino and UHECR emission, whose predictions satisfy the current observations. By embedding this mechanism in a simulation of multiple internal collisions within the GRB jet, we obtain a robust prediction of a minimal diffuse GRB neutrino flux that will likely be within reach of the next generation of neutrino telescopes. Finally, I will show preliminary results that could help assess whether a particular observed GRB has a bright accompanying prompt neutrino signal, on the basis of the morphology of its gamma-ray light curve alone.

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