Seminarium Fizyki Wielkich Energii

Even though the first UHECR was detected almost 60 years ago, the origin of these particles remains a mystery. For lower energies, their paths are twisted by the Galactic magnetic field, while for higher energies their fluxes are too low to give a statistically significant location on the sky. This is even though the largest observatories occupy hundreds to thousands of square kilometres.In this seminar, I will show two approaches to solving this problem. The first one is significantly increasing the volume of the atmosphere observed. This can be achieved either with covering tens of thousands of square kilometres with simple radio antennas, which is the aim of the Giant Radio Array for Neutrino Detection (GRAND) experiment. Alternatively, UHECR induced fluorescent tracks in the atmosphere can be observed from the orbit, which is the idea behind JEM-EUSO and Poemma experiments. The second approach is to detect ultra-high energy neutrinos, unaffected by Galactic magnetic fields, created by the UHECRs close to their origin. This is, again, the aim of both GRAND and Poemma experiments. Spotkanie odbędzie się za pośrednictwem platformy zoom: Join Zoom Meeting https://us02web.zoom.us/j/84516096743?pwd=a3BYQ24zY1ZjQTF4eFIwUnM2WlNaZz09 (Meeting ID: 845 1609 6743; Passcode: HEP_UW)

Even though the first UHECR was detected almost 60 years ago, the origin of these particles remains a mystery. For lower energies, their paths are twisted by the Galactic magnetic field, while for higher energies their fluxes are too low to give a statistically significant location on the sky. This is even though the largest observatories occupy hundreds to thousands of square kilometres.In this seminar, I will show two approaches to solving this problem. The first one is significantly increasing the volume of the atmosphere observed. This can be achieved either with covering tens of thousands of square kilometres with simple radio antennas, which is the aim of the Giant Radio Array for Neutrino Detection (GRAND) experiment. Alternatively, UHECR induced fluorescent tracks in the atmosphere can be observed from the orbit, which is the idea behind JEM-EUSO and Poemma experiments. The second approach is to detect ultra-high energy neutrinos, unaffected by Galactic magnetic fields, created by the UHECRs close to their origin. This is, again, the aim of both GRAND and Poemma experiments. Spotkanie odbędzie się za pośrednictwem platformy zoom: Join Zoom Meeting https://us02web.zoom.us/j/84516096743?pwd=a3BYQ24zY1ZjQTF4eFIwUnM2WlNaZz09 (Meeting ID: 845 1609 6743; Passcode: HEP_UW)