27-31 August 2018
LVH, Luisenstraße 58, 10117 Berlin
Europe/Berlin timezone
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Neutrino + Cosmic Rays


Location: LVH, Luisenstraße 58, 10117 Berlin
Address: LANGENBECK VIRCHOW HAUS Luisenstraße 58, 10117 Berlin
Date: 31 Aug 14:00 - 3:45 PM


Chair: Markus Ahlers


  • 6
    • Dr. Palladino, Andrea (DESY)
    • Kopper, Claudio (University of Alberta)
    • Dr. Heijboer, Aart (NIKHEF)
    • Dr. Casanova, Sabrina (IFJ PAN & MPIK HD)
    • Dr. boncioli, denise (DESY)
    • Bykov, Andrei (Ioffe Physico-Technical Institute)

Timetable | Contribution List

Displaying 7 contributions out of 7
Type: Talk Session: Neutrino + Cosmic Rays
Track: Cosmic Rays
The study of UHECR is challenged by both the rarity of events and the difficulty in modelling their production, propagation and detection. The physics behind these processes is complicated, requiring high-dimensional models which are impossible to fit to data using traditional methods. Whilst non-trivial, it is indeed possible to directly fit realistic, physical models to the UHECR data. The combi ... More
Presented by Ms. Francesca CAPEL on 31/8/2018 at 13:00
Type: Talk Session: Neutrino + Cosmic Rays
Track: Cosmic Rays
We present a combined fit of the Auger spectrum and composition based on a newly developed code for the extragalactic propagation of cosmic ray nuclei (PriNCe). This very efficient numerical solver of the transport equations allows for scans over large ranges of unknown UHECR source parameters. Here, we present a study of a generalized source population with three parameters (rigidity-dependent ... More
Presented by Mr. Jonas HEINZE on 31/8/2018 at 12:45
Type: Talk Session: Neutrino + Cosmic Rays
Track: Neutrinos
The existence of an astrophysical neutrino flux at TeV to PeV energies has now been firmly established by the IceCube collaboration. However, the sources responsible for this flux have not yet been identified. The most important candidates, steady emitting blazars and transient gamma-ray bursts, favoured on the basis of their high gamma-ray luminosity, are now ruled out as the dominant source popu ... More
Presented by Matthias VEREECKEN on 31/8/2018 at 13:30
Type: Talk Session: Neutrino + Cosmic Rays
Track: Cosmic Rays
The Pierre Auger Observatory is the world’s largest cosmic-ray detector, sensitive to cosmic rays with energy exceeding $\sim 10^{17}$ eV. In addition to charged cosmic rays that form the bulk of the cosmic-ray flux at ultra-high energies, Auger is sensitive to ultra-high energy neutral messengers (photons, neutrinos, and neutrons). The latter are particularly exciting as they are expected to ar ... More
Presented by Dr. Foteini OIKONOMOU on 31/8/2018 at 12:00
Type: Talk Session: Neutrino + Cosmic Rays
Track: Neutrinos
Cosmic rays were discovered a century ago, however the sources of the ultra-high-energy events remain unidentified. It is believed that the same environments that accelerate ultra-high-energy cosmic rays (UHECRs) also produce high-energy neutrinos via hadronic interactions. Two out of three joint analyses of the IceCube Neutrino Observatory, the Pierre Auger Observatory and the Telescope Array y ... More
Presented by Lisa SCHUMACHER on 31/8/2018 at 12:15
Type: Talk Session: Neutrino + Cosmic Rays
Track: Neutrinos
In the context of the recent multi-messenger observation of neutron-star merger GW170817, we examine whether such objects could be sources of ultrahigh energy cosmic rays. At first order, the energetics and the population number is promising to envisage the production of a copious amount of particles, during the first minutes to weeks from the merger. On the other hand, the strong radiative enviro ... More
Presented by Mr. Valentin DECOENE on 31/8/2018 at 13:15
Type: Talk Session: Neutrino + Cosmic Rays
Track: Cosmic Rays
When ultra-high-energy cosmic rays (UHECRs) travel through the universe they create cosmogenic neutrinos via several interactions. The expected flux at Earth of these cosmogenic neutrinos generally depends on multiple parameters describing the sources and propagation of UHECRs. However, at a neutrino energy of ~1 EeV a 'sweet spot' occurs where this flux only depends strongly on two parameters, th ... More
Presented by Dr. Arjen VAN VLIET on 31/8/2018 at 12:30
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