GCOS - The Global Cosmic Ray Observatory

Hörandel, J. R.

doi:10.22323/1.395.0027

Cited by 23 publications

(35 citation statements)

References 71 publications

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“…At even higher energies, ZeV neutrinos might come from cosmic strings [137,138]. Next-generation, multipurpose EeV-ZeV detectors are being planned or under construction with a variety of detection strategies: in-water and in-ice Cherenkov (IceCube-Gen2 [115]), in-air Cherenkov, fluorescence, and particle showers (EUSO-SPB2 [121], POEMMA [122], AugerPrime [139], GCOS [140]), and radio (GRAND [141], RNO-G [142], PUEO [143], BEACON [144], TAROGE [145], AugerPrime [139], GCOS [140]).…”

Section: Present and Future Experimental Landscapementioning

confidence: 99%

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High-Energy and Ultra-High-Energy Neutrinos

Ackermann,

Agarwalla,

Alvarez-Muñiz

et al. 2022

Preprint

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Astrophysical neutrinos are excellent probes of astroparticle physics and high-energy physics. With energies far beyond solar, supernovae, atmospheric, and accelerator neutrinos, high-energy and ultrahigh-energy neutrinos probe fundamental physics from the TeV scale to the EeV scale and beyond. They are sensitive to physics both within and beyond the Standard Model through their production mechanisms and in their propagation over cosmological distances. They carry unique information about their extreme non-thermal sources by giving insight into regions that are opaque to electromagnetic radiation. This white paper describes the opportunities astrophysical neutrino observations offer for astrophysics and high-energy physics, today and in coming years.Fully opening the HE and UHE neutrino windows requires a multi-pronged approach that explores a broad range of proposed experimental techniques. With upcoming neutrino telescopes, the goal is to improve the sensitivity ten-fold in the HE range and hundred-fold in the UHE range. In the HE range, we are moving into the high-statistics era, where subtle features may be resolved and multiple sources may be discovered. In the UHE range, neutrino flux predictions and physics tests are well-motivated, but we will likely need new techniques to enable discoveries. The ongoing efforts to develop new instruments will improve sensitivity, increase statistics, and expand the energy range. A broad range of experimental approaches, with complementary capabilities, must be developed and tested in the coming decades. Because it is not clear which techniques will prevail, we advocate for a broad portfolio of experiments in the HE and UHE neutrino sector. Owing to their potential, HE and UHE neutrinos should be at the forefront of the high-energy physics program, as they push the boundaries for the neutrino, cosmic, energy, theory, and instrumentation frontiers. 4 Experimental landscape 32 4.1 Overview 32 4.2 High-energy range 35 4.3 Ultra-High Energy Range (> 100-PeV) 45

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Section: Present and Future Experimental Landscapementioning

confidence: 99%

“…More detailed considerations can be found in Ref. [140] and references therein. With the goal of reaching an exposure of at least 2 × 10 5 km 2 yr in a period of 10 years and full-sky coverage a set of surface arrays with a total area of about 40000 km 2 is anticipated as shown in Fig.…”

Section: Gcosmentioning

confidence: 99%

High-Energy and Ultra-High-Energy Neutrinos

Ackermann,

Agarwalla,

Alvarez-Muñiz

et al. 2022

Preprint

Self Cite

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“…The next generation of ground-based UHE CR observatories are envisioned for the 2030s. The community has started to collect ideas for the scientific scope and detector concept of a Global Cosmic Ray Observatory (GCOS) [882]. The detector design will need to be optimized for the competing requirements for energy and mass resolution on one hand -typically achieved by small and dense surface arrays -and event statistics from large exposures on the other hand -requiring larger arrays with sparser detectors.…”

Section: Future Ground-based Extensive Air Shower Detectors For Cosmi...mentioning

confidence: 99%

Advancing the Landscape of Multimessenger Science in the Next Decade

Engel¹,

Lewis²,

Muzio³

et al. 2022

Preprint

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The last decade has brought about a profound transformation in multimessenger science. Ten years ago, facilities had been built or were under construction that would eventually discover the nature of objects in our universe could be detected through multiple messengers. Nonetheless, multimessenger science was hardly more than a dream. The rewards for our foresight were finally realized through IceCube's discovery of the diffuse astrophysical neutrino flux, the first observation of gravitational waves by LIGO, and the first joint detections in gravitational waves and photons and in neutrinos and photons. Today we live in the dawn of the multimessenger era.The successes of the multimessenger campaigns of the last decade have pushed multimessenger science to the forefront of priority science areas in both the particle physics and the astrophysics communities. Multimessenger science provides new methods of testing fundamental theories about the nature of matter and energy, particularly in conditions that are not reproducible on Earth. This white paper will present the science and facilities that will provide opportunities for the particle physics community renew its commitment and maintain its leadership in multimessenger science.

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“…It was these composite interlinks of local triggers that made it possible in practice to measure ultra-high-energy cosmic-ray (UHECR) flux above 10 20 eV, which is on the order of one particle per few km 2 per century. The construction of larger surface detector arrays for the measurement of increasingly higher cosmic-ray energies, where the flux is increasingly lower is, today, only considered theoretically with the prospect of realization in the next decades [3]. For larger statistics measurements above the Greisen-Zatsepin-Kuzmin cutoff, new techniques are needed, such as satellite or radio measurements, which dozens or hundreds of scientists from many countries are working on [4,5].…”

Section: Introductionmentioning

confidence: 99%

Symmetries in the Superposition Model of Extensive Air Shower Development

Wibig

2022

Symmetry

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According to the superposition principle, an extensive air shower initiated by a nucleus with energy E and mass number A can be approximated as the superposition of A proton-initiated showers each with energy E/A. The superposition principle for interactions of atomic nuclei proposes to describe nucleus-initiated extensive air showers using simulations performed for proton showers. Single detectors and systems working in tight coincidence mainly register events initiated by particles with very low energies, which are affected by major statistical fluctuations, such as those used in high schools for education and outreach purposes. Verifying whether the superposition principle is still a good approximation in the low-energy region is important for the validity of the interpretation of such measurements. We present results of the comparison of results of the superposition model with detailed simulations of showers with the CORSIKA program from the energy of 10 GeV. While the energy dependence of the mean shower parameters satisfies the superposition principle, the higher moments do not. A modification of the superposition model based on the wounded nucleon model, reducing these discrepancies, is proposed. The semi-analytical description of showers in the modified superposition model can give the density spectrum of cosmic ray particles, which is consistent with the measurements. In this paper, we present results both consistent with the superposition model and indicating the need for its modification. This modification is proposed and tested.

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GCOS - The Global Cosmic Ray Observatory

Cited by 23 publications

References 71 publications

High-Energy and Ultra-High-Energy Neutrinos

High-Energy and Ultra-High-Energy Neutrinos

Advancing the Landscape of Multimessenger Science in the Next Decade

Symmetries in the Superposition Model of Extensive Air Shower Development

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