Ultra high energy cosmic ray sources and experimental results

Biermann, P. L.; Tanco, Gustavo Medina

doi:10.1016/s0920-5632(03)80366-3

Cited by 7 publications

(3 citation statements)

References 99 publications

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“…If the source of EHE particles is such an SHDM, it could be concentrated in our Milky Way Galaxy and might show an enhancement in the direction of Sagittarius [16,22,23], and small clumps can be seen in the outer region [24]. If they belong to clusters of galaxies, they may show the enhancement at nearby clusters such as Virgo, Pisces, Peruses and Heracles [16,25].…”

Section: Possible Identification Of Sources By Arrival Directionmentioning

confidence: 99%

The JEM‐EUSO Mission

2011

AIP Conference Proceedings

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JEM-EUSO is a space science mission to explore the extreme energies and physics of the Universe. Its instrument will watch the darkside of the earth and will detect UV photons emitted from the extensive air shower caused by an ultra-high energy cosmic ray (UHECR above 10 18 eV), or an extremely high energy cosmic ray (EHECR) particle (e.g. above about 10 20 eV). Such a high-rigidity particle as the latter arrives almost in a straight line from its origin through the magnetic fields of our Milky Way Galaxy and is expected to allow us to trace the source location by its arrival direction. This can open the door to new astronomy with charged particles. In its 5 years of operation including the tilted mode, Extreme Universe Space Observatory an Japanese Experiment Module (JEM-EUSO) will detect at least 1000 events with E > 7 × 10 19 eV with the Greisen-Zatsepin-Ku'zmin (GZK) suppression spectrum. It can determine the energy spectrum and source locations of GZK to super-GZK regions with a statistical accuracy of several percent. JEM-EUSO is planned to be deployed by H2 transfer vehicle (HTV) and will be attached to the Japanese Experiment Module/Exposure Facility (JEM/EF) of International Space Station. JAXA has selected JEM-EUSO as one of the mission candidates of the second phase utilization of JEM/EF for launch in the early-to-mid 2010 s.

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Section: Possible Identification Of Sources By Arrival Directionmentioning

confidence: 99%

The JEM‐EUSO Mission

2011

AIP Conference Proceedings

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“…The main models describing the transition are the ankle model, the dip model and the mixed composition model. In the ankle model the transition between the Galactic cosmic rays (GCR) and extragalactic cosmic rays (EGCR) occurs at the ankle E a ≈ 1 × 10 19 eV [5,6,7,8,9,10,11,12]. The dip in the CR spectrum is explained as the intersection of a flat extragalactic component with the steep Galactic component.…”

Section: Galactic and Extragalactic Cosmic Rays: Transition Modelsmentioning

confidence: 99%

Experimental constraints on the astrophysical interpretation of the cosmic ray Galactic–extragalactic transition region

Donato

Medina‐Tanco

2009

Astroparticle Physics

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The energy region spanning from ∼ 10 17 to 10 19 eV is critical for understanding both, the Galactic and the extragalactic cosmic ray fluxes. This is the region where the propagation regime of nuclei inside the Galactic magnetic environment changes from diffusive to ballistic, as well as the region where, very likely, the most powerful Galactic accelerators reach their maximum output energies. In this work, a diffusion Galactic model is used to analyze the end of the Galactic cosmic ray spectrum and its mixing with the extragalactic cosmic ray flux. In particular, we study the conditions that must be met, from the spectral and composition points of view, by the Galactic and the extragalactic fluxes in order to reproduce simultaneously the total spectrum and elongation rate measured over the transition region by HiRes and Auger. Our analysis favors a mixed extragalactic spectrum in combination with a Galactic spectrum enhanced by additional high energy components, i.e., extending beyond the maximum energies expected from regular supernova remnants. The two additional components have mixed composition, with the lowest energy one heavier than the highest energy one. The potential impact on the astrophysical analysis of the assumed hadronic interaction model is also assessed in detail.

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“…In the universe, as we know from direct observation (first Linsley 1963), we have particles up to 300 EeV (= 3 • 10 20 eV); even in the center of mass collision with an identical particle (proton or heavier) this yields energies in the center of mass frame of 5 • 10 14 eV, so more. If we could identify the sources and interaction regions of these extreme energy particles (see the books by Ginzburg & Syrovatskii 1964, Berezinsky et al 1990, Gaisser 1991, Stanev 2004, and recent reviews by Gaisser & Stanev 2006, Biermann et al 2003, as well as Nagano & Watson 2000) we may be able to learn some of the physics at such energies, so perhaps go beyond the LHC.…”

Section: Introductionmentioning

confidence: 99%

Active Galactic Nuclei: Sources for ultra high energy cosmic rays?

Biermann,

Becker,

Caramete

et al. 2008

Preprint

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The origin of ultra high energy cosmic rays promises to lead us to a deeper understanding of the structure of matter. This is possible through the study of particle collisions at center-of-mass energies in interactions far larger than anything possible with the Large Hadron Collider, albeit at the substantial cost of no control over the sources and interaction sites. For the extreme energies we have to identify and understand the sources first, before trying to use them as physics laboratories. Here we describe the current stage of this exploration. The most promising contenders as sources are radio galaxies and gamma ray bursts. The sky distribution of observed events yields a hint favoring radio galaxies. Key in this quest are the intergalactic and galactic magnetic fields, whose strength and structure are not yet fully understood. Current data and statistics do not yet allow a final judgement. We outline how we may progress in the near future.

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Ultra high energy cosmic ray sources and experimental results

Cited by 7 publications

References 99 publications

The JEM‐EUSO Mission

The JEM‐EUSO Mission

Experimental constraints on the astrophysical interpretation of the cosmic ray Galactic–extragalactic transition region

Active Galactic Nuclei: Sources for ultra high energy cosmic rays?

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