Ultra High Energy Cosmic Rays an overview

Aloisio, Roberto

doi:10.1088/1742-6596/2429/1/012008

Cited by 4 publications

(4 citation statements)

References 48 publications

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“…Auger (and the smaller TA experiment in the northern hemisphere) detected cosmic rays up to energy E ≈ 2 10 11 GeV with flux roughly given by [43][44][45]…”

Section: Highest-energy Cosmic-ray Collisionsmentioning

confidence: 99%

Triggering Higgs vacuum decay

Strumia

2023

J. High Energ. Phys.

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The Standard Model Higgs potential seems unstable at field values h > htop ~ 1010 GeV. Vacuum decay can be triggered by N ~ 4π/λ ~ 1000 overlapped Higgs bosons with energy $$ \sqrt{\lambda } $$ λ htop. However, this configuration is stimulated by ultra-high energy collisions with a exp(−$$ \mathcal{O} $$ O (N)) suppression, comparable to spontaneous vacuum decay: no ‘Higgspolosion’ enhancement arises. This implies that ultra-high energy cosmic ray collisions are safe, despite that their number (in production sites) likely is tens of orders of magnitude higher than what usually estimated (in space). We speculate on how vacuum decay could be induced classically, forming a in-coming wave of N boosted Higgs bosons at futuristic ultra-high energy colliders, and on how the resulting vacuum bubble could be controlled to extract energy.

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“…Auger (and the smaller TA experiment in the northern hemisphere) detected cosmic rays up to energy E ≈ 2 10 11 GeV with flux roughly given by [43][44][45]…”

Section: Highest-energy Cosmic-ray Collisionsmentioning

confidence: 99%

Triggering Higgs vacuum decay

Strumia

2023

J. High Energ. Phys.

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“…Accordingly, various research efforts are being undertaken to observe and analyse such objects and phenomena. Observations can be carried out directly in space [ 17 ] or indirectly based on detectors placed on the Earth’s surface [ 18 ]. In the second case, particles or groups of particles that result from the collision of primary high-energy cosmic particles with the atmosphere are detected.…”

Section: Introductionmentioning

confidence: 99%

The Practice of Detecting Potential Cosmic Rays Using CMOS Cameras: Hardware and Algorithms

Hachaj

Piekarczyk

2023

Sensors

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In this paper, we discuss a practice of potential cosmic ray detection using off-the-shelves CMOS cameras. We discuss and presents the limitations of up-to-date hardware and software approaches to this task. We also present a hardware solution that we made for long-term testing of algorithms for potential cosmic ray detection. We have also proposed, implemented and tested a novel algorithm that enables real-time processing of image frames acquired by CMOS cameras in order to detect tracks of potential particles. We have compared our results with already published results and obtained acceptable results overcoming some limitation of already existing algorithms. Both source codes and data are available to download.

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“…As charges they are bent, deflected and smeared in their flight through cosmic and galactic magnetic fields losing most of the astrophysical source imprint. Thus for a century the CR origin remained a mystery and a compelling question continually addressed by high-energy astrophysics [1]. Indeed the Ultra High Energy CR (UHECR) nature itself connects the most violent sources of the Universe with the deep inner secrets of nuclear and particle physics.…”

Section: Introductionmentioning

confidence: 99%

“…Candidate sources, whether they are small as SN, GRB, Star-Burst, or larger as AGN Jet, can be found both far from us and close -even in our galaxy-in a complex inhomogeneous cosmic structure. We show how this difficult source correlation search can be approached and partially solved by constrains based on last two decades of observational discoveries [1] on UHECR composition, their clustering and anisotropies at different energy windows.…”

Section: Introductionmentioning

confidence: 99%

UHECR Signatures and Sources

2023

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We discuss recent results on the clustering, composition and distribution of Ultra-High Energy Cosmic Rays (UHECR) in the sky; from the energy of several tens of EeV in the dipole anisotropy, up to the highest energy of a few narrow clusters, those of Hot Spots. Following the early UHECR composition records deviations from proton we noted that the UHECR events above 40 EeV can be made not just by any light or heavy nuclei, but mainly by the lightest ones as He,D, Li,Be. The remarkable Virgo absence and the few localized nearby extragalactic sources, such as CenA, NGC 253 and M82, are naturally understood: lightest UHECR nuclei cannot reach us from the Virgo distance of twenty Mpc, due to their nuclei fragility above a few Mpc distances. Their deflection and smearing in wide hot spots is better tuned to the lighter nuclei than to the preferred proton or heavy nuclei candidate courier. We note that these lightest nuclei still suffer of a partial photodistruction even from such close sources. Therefore, their distruption in fragments, within few tens EeV multiplet chain of events, have been expected and later on observed by Auger collaboration, nearly a decade ago. These multiplet presences, strongly correlate with the same CenA, NGC253 sources. The statistical weight of such correlation is reminded. We conclude that the same role of NGC 253 clustering at lower energies could also feed the Auger dipole anisotropy at lower energy ranges. Such lower energy anisotropy could be fed and integrated by nearest Vela, Crab, LMC and Cas A contributes. In our present UHECR model, based on lightest nuclei in local volumes of a few Mpcs, closest AGN, Star-Burst or very close SNR are superimposing their signals, frozen in different epochs, distances and directions, feeding small and wide anisotropy. Possible tests to confirm, or untangle the current model from alternative ones, are suggested and updated.

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Ultra High Energy Cosmic Rays an overview

Cited by 4 publications

References 48 publications

Triggering Higgs vacuum decay

Triggering Higgs vacuum decay

The Practice of Detecting Potential Cosmic Rays Using CMOS Cameras: Hardware and Algorithms

UHECR Signatures and Sources

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