Cosmic ray / gamma ray / neutrino and similar experiments. Multimessenger Search for the Sources of Cosmic Rays Using Cosmic Neutrinos

The luminosity of this source class is relatively low or the production radius is largesince low enough radiation densities in the source are a necessary requirement for that. Google Scholar. Gamma-ray bursts GRBs are short-lived, luminous explosions at cosmological distances, thought to originate from relativistic jets launched at the deaths of massive stars. In order to test the GRB-UHECR paradigm, a combined source-propagation model is needed: the accelerated nuclei are injected into the radiation zone, where the secondaries are produced, escape from that zone, and are then propagated through the extragalactic space to Earth see Baerwald et al. Lu, L. For details, see Gokus et al.

 

List of links to experiments for cosmic rays, gamma rays, and neutrinos. Includes space, balloon, airshower, and underground experiments.We have taken into account two possibilities for UHECR escape: emission as neutrons, which are not magnetically confined, and emission as protons from the edges of the shells—the dominant mechanism in each collision depends on the parameters of the colliding shells.

 

The similar energy densities of the extragalactic gamma-ray flux observed by Fermi and the high-energy cosmic neutrino.Mixed Composition Ankle Model.

 

Results. We demonstrate that the expected neutrino flux from GRBs weakly depends on the injection composition for the same injection spectra and luminosities.Clearly, the quasi-diffuse flux coming from the simulations is independent of the value of t vas expected from equation 4.

 

The quest for these faint but energetic signals is the focus of more than 50 large, ground-based experiments that are looking for high energy photons or.This means that we can extrapolate our assumptions to below the photosphere to some degree.Forum Cosmic ray / gamma ray / neutrino and similar experiments

 

As a consequence, neutrinos, cosmic rays and Fermi Large Area Telescope (LAT)/CTA gamma rays probe different emission radii.Services Articles citing this article CrossRef

 

Neutrino telescopes and high-energy cosmic neutrinos Incidentally, the study of gamma-ray radiation began in the same years by.The neutrino flux is dominated by photo-meson production off the primary nuclei; it is relatively low because of the low target photon density.

 

several experiments that search for neutrinos, cosmic rays, gamma rays, by cosmic rays, subatomic particles—like protons—of cosmic origin with.At the lowest energies, nuclei lose energy adiabatically because of the expansion of the Universe.

 

Cosmic neutrinos are generated by cosmic rays in extragalactic sources that on Earth—and more than we could hope to produce in any of our experiments.Modelling the coincident observation of a high-energy neutrino and a bright blazar flare.

 

Parenthesis on Cosmic Rays and Extensive Air Showers. Particle Physics experiments: Radio astronomy: Gamma ray sources, radio Galaxies, AGNs.While there are continuous transitions among these cases, we discuss three prototypes, which exhibit the behavior characteristic for their class.

 

Kobayashi, S.

 

The IceCube neutrino observatory: instrumentation and online systems.

 

Lemoine, M.

 

This model does not yet exploit the strength of our method in full, which is to be discussed in future publications.

 

The impact of the injection isotope for pure composition injection is shown in Fig.

 

As a next step, we identify the relevant channels and set up the PDE system Eq.

 

Neutrons, on the other hand, can typically escape from the region because they are not magnetically confined, or by photohadronic interactions 2.

 

The IceCube neutrino observatory: instrumentation and online systems.

 

We note that the energy per messenger per bin is obtained as a product of energy released per collision, and the number of collisions occurring per R C -bin; especially the latter number is important to get the proper weighing of R C.

 

In the main text of this work, we assume that the minimal photon energy is low enough for the high-energy cosmic ray nuclei to find interaction partners above the GDR threshold.

 

Parameter space scan for Mixed Composition Ankle Model in the internal shock scenario.

 

This is numerically equivalent to computing the steady state for the neutrons fromassuming that it is dominated by the photohadronic interaction rate at the peak of the spectrum.

 

For protons, the intermediate energy range is dominated by energy losses by electron-positron pair production on the CMB.

 

Figure 5: Energy dissipated beyond the photosphere.

 

One can also read off from Fig.

 

The best fit to the spectrum of neutrinos observed through the Earth is compared to the unfolded spectrum of events starting inside the detector.

 

A schematic illustration can be found in Fig.

 

Can internal shocks produce the variability in GRBs?

 

The first method has traditionally focused on the observation of muon neutrinos that interact primarily outside the detector.Forum Cosmic ray / gamma ray / neutrino and similar experiments

 

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The nuclear cascade lower left panel is, relative to the injection energy, well populated, where light nucleons are occupied similar to the near- 56 Fe isotopes.

 

Maximal energy.

 

We show in Fig.

 

There are a few important caveats in this picture.

 

We illustrate this quantity for three different examples in Fig.

 

Our standard parameter set is assumed for the simulation.

 

Hidden cosmic-ray accelerators as an origin of TeV-PeV cosmic neutrinos.