Investigating the 2nd knee: The KASCADE-Grande experiment

Haungs, A.; Apel, W. D.; Badea, F.; Bekk, K.; Bercuci, A.; Bertaina, M.; Bliimer, J.; Bozdog, H.; Brancus, I. M.; Brüggemann, M.; Buchholz, P.; Чиавасса, А.; Daumiller, K.; Pierre, Fritz; Döll, P.; Engel, R.; Engler, J.; Ghia, P. L.; Gils, H.J.; Glasstetter, R.; Grupen, C.; Heck, D.; Hörandel, J. R.; Kampert, K.‐H.; Klages, H. O.; Kolotaev, Y.; Maier, G.; Mathes, H.J.; Mayer, H.J.; Milke, J.; Mitricat, B.; Morello, C.; Müller, M. A.; Navarra, G.; Obenland, R.; Oehlschläger, J.; Ostapchenko, S.; Over, S.; Petcut, M.; Pierog, T.; Plewnia, S.; Rebel, H.; Risse, A.; Roth, M.; Schieler, H.; Sima, O.; Stümpert, M.; Toma, G.; Trinchero, G.; Ulrich, H.; Valchierotti, S.; Buren, J. van; Walkowiak, W.; Weindl, A.; Wochele, J.; Zabierowski, J.; Zagromski, S.; Zimmermann, D.

doi:10.1088/1742-6596/47/1/029

Cited by 6 publications

(8 citation statements)

References 20 publications

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“…Regular measurements with this new array and the original KASCADE detectors, forming the KASCADE-Grande experiment, are performed since summer 2003 (Chiavassa et al, 2005). The objective is to reconstruct energy spectra for groups of elements up to 10 18 eV (Haungs et al, 2006a). First analyses extend the lateral distributions of electrons and muons up to 600 m (Glasstetter et al, 2005;v.…”

Section: Transition To Extragalactic Cosmic Raysmentioning

confidence: 99%

Cosmic-ray composition and its relation to shock acceleration by supernova remnants

Hörandel

2008

Advances in Space Research

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An overview is given on the present status of the understanding of the origin of galactic cosmic rays. Recent measurements of charged cosmic rays and photons are reviewed. Their impact on the contemporary knowledge about the sources and acceleration mechanisms of cosmic rays and their propagation through the Galaxy is discussed. Possible reasons for the knee in the energy spectrum and scenarios for the end of the galactic cosmic-ray component are described.

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Section: Transition To Extragalactic Cosmic Raysmentioning

confidence: 99%

Cosmic-ray composition and its relation to shock acceleration by supernova remnants

Hörandel

2008

Advances in Space Research

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“…But for a sufficiently small dt the ionization fractions hardly change, so that Q(t) ≈ Q(t − dt), and latter can be derived from the previous calculation step. The total ionization and recombination rate λ ion ji and λ rec ji , respectively, are taken from the Chianti atomic database 4 which is also part of Cloudy. This procedure adopts some of the basic ideas of the ChiantiPy v0.9.5 5 realization of the collisional ionization equilibrium [52], and ensures that the equilibrium values are obtained for t → ∞, as displayed in Fig.…”

Section: Shock Heating and Downstream Ionization Time Scalesmentioning

confidence: 99%

“…Subsequently, we apply our model to the LECR data in Sect. 4, and conclude with an outlook to further applications of the model in Sect. 5.…”

Section: Introductionmentioning

confidence: 98%

“…Longest known are the steepening at around 1 PeV [2] commonly called "the knee". Later, a long-suspected flattening at around 4 EeV has been experimentally confirmed [3], and became known as "the ankle" to complete the anatomic analogy, which was then stretched by the discovery of another steepening at around 100 PeV [4], now called "the second knee" [5]. All these features are thought to hide information about the origin of cosmic rays, but unfortunately their meaning is disputed: The knee could be explained by a source cutoff [e.g., 6,7] or a transport effect in the Galaxy [8,9], in which case the second knee would mark the Galactic source cutoff.…”

Section: Introductionmentioning

confidence: 99%

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Nonthermal element abundances at astrophysical shocks

Eichmann,

Rachen

2020

Preprint

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The nonthermal source abundances of elements play a crucial role in the understanding of cosmic ray phenomena from a few GeV up to several tens of EeV. We present a first systematic approach to describe the change of the abundances from the thermal to the nonthermal state via diffusive shock acceleration by a temporally evolving shock. We consider hereby not only ionization states of elements contained in the ambient gas, which we allow to be time dependent due to shock heating, but also elements condensed on solid, charged dust grains which can be injected into the acceleration process as well. Our generic parametrized model is then applied to the case of particle acceleration by supernova remnants in various ISM phases, for which we use state-of-the-art computation packages to calculate the ionization states of all elements. The resulting predictions for low energy cosmic ray source abundances are compared with the data obtained by various experiments.We obtain excellent agreement for shocks in warm ionized ISM environments, which include HII regions, if dust grains are injected into the diffusive shock acceleration process with a much higher efficiency than ions. Less dependence of the fit quality is found on the mass-to-charge ratio of ions. In contrast, for neutral ISM environments, assuming that there are shocks in the weak ionized component, or for the hot ionized medium we obtain generally inferior fits. Hereby, the main reason for this difference does not seem to be the density or temperature of the ISM environments, but their gas-to-dust ratio. We briefly discuss potential consequences for the understanding of the composition around the second knee or the cosmic ray spectrum, or for the viability of explaining ultra-high energy cosmic rays with a dominant contribution by radio galaxies.

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“…Regular measurements with this new array and the original KASCADE detectors, forming the KASCADE-Grande experiment, are performed since summer 2003 [63]. The objective is to reconstruct energy spectra for groups of elements up to 10 18 eV [64], covering the energy region of the second knee, where the galactic cosmic ray spectrum is expected to end [65]. First analyses extend the lateral distributions of electrons and muons up to 600 m [66,67].…”

Section: Eas-topmentioning

confidence: 99%

COSMIC RAYS FROM THE KNEE TO THE SECOND KNEE: 10¹⁴ TO 10¹⁸ eV

Hörandel

2007

Astrophysics at Ultra-High Energies

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The energies of cosmic rays, fully ionized charged nuclei, extend over a wide range up to 10 20 eV. A particularly interesting energy region spans from 10 14 to 10 18 eV, where the all-particle energy spectrum exhibits two interesting structures, the 'knee' and the 'second knee'. An explanation of these features is thought to be an important step in understanding of the origin of the highenergy particles. Recent results of air shower experiments in this region are discussed. Special attention is drawn to explain the principle of air shower measurements -a simple Heitler model of (hadronic) air showers is developed.

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Investigating the 2nd knee: The KASCADE-Grande experiment

Cited by 6 publications

References 20 publications

Cosmic-ray composition and its relation to shock acceleration by supernova remnants

Cosmic-ray composition and its relation to shock acceleration by supernova remnants

Nonthermal element abundances at astrophysical shocks

COSMIC RAYS FROM THE KNEE TO THE SECOND KNEE: 10¹⁴ TO 10¹⁸ eV

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Investigating the 2nd knee: The KASCADE-Grande experiment

Cited by 6 publications

References 20 publications

Cosmic-ray composition and its relation to shock acceleration by supernova remnants

Cosmic-ray composition and its relation to shock acceleration by supernova remnants

Nonthermal element abundances at astrophysical shocks

COSMIC RAYS FROM THE KNEE TO THE SECOND KNEE: 1014 TO 1018 eV

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COSMIC RAYS FROM THE KNEE TO THE SECOND KNEE: 10¹⁴ TO 10¹⁸ eV