Low Energy Cosmic Ray Nuclei and their Propagation in the Galaxy

Giller, M.

doi:10.1007/978-94-010-0560-9_24

Cited by 3 publications

(3 citation statements)

References 21 publications

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“…The actual values of the parameters differ from our preliminary fit, presented at the ICRC in Japan [5]. (The fit presented here has been done to new simulations where the upper limit for the weight, ascribed to an electron in the thinning procedure, was much lower (10 5 ) than that assumed before (10 30 ).…”

Section: Energy Spectra Of Electronsmentioning

confidence: 71%

Energy spectra of electrons in the extensive air showers of ultra-high energy

Giller

Wieczorek

Kacperczyk

et al. 2004

J. Phys. G: Nucl. Part. Phys.

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We show that the shape of the energy spectrum of electrons in an extensive air shower with an ultra-high energy (E ⩾ 1019 eV) at a given level in the atmosphere depends only on the shower age at this level. It depends practically neither on the primary particle mass nor on its energy. This fact considerably simplifies interpretation of data from the experiments (e.g., Fly's Eye, HiRes and Auger) determining cascade curves of single showers by the fluorescence technique. In particular, the contribution of the scattered Cherenkov light to the total flux produced by a shower can be easily taken into account. Our conclusion has been drawn by analysing results of Monte Carlo simulations of showers with the CORSIKA (Heck et al 1998 Report FZKA 6019) program, using the QGSJet interaction model.

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Section: Energy Spectra Of Electronsmentioning

confidence: 71%

Energy spectra of electrons in the extensive air showers of ultra-high energy

Giller

Wieczorek

Kacperczyk

et al. 2004

J. Phys. G: Nucl. Part. Phys.

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“…This model has its adherents. In one such model [24] a distribution of pulsar periods at birth is chosen-which is not unreasonable-and iron nuclei are involved so as to give the measured CR spectrum. The energetics are reasonable.…”

Section: High Energy Cr From Many Pulsarsmentioning

confidence: 99%

The origin of cosmic rays

Erlykin¹,

Wolfendale²

2005

J. Phys. G: Nucl. Part. Phys.

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It is generally regarded that the bulk of cosmic rays originate in the galaxy and that those below the ‘knee’ (the rapid steepening in the energy spectrum) at a few PeV, come from galactic supernovae, the particles being accelerated by the shocks in the supernova remnants. At higher energies, there are problems in that conventional SNR—which surely constitute the bulk of the sources—have a natural limit at a few tens of PeV (for iron nuclei). The question of the origin of particles above this limit is thus an open one. Here we examine a number of possibilities: a variety of supernovae and hypernovae, pulsars, a giant galactic halo and an extragalactic origin. A relevant property of any model is the extent to which it can provide the lack of significant irregularity of the energy spectrum, its intensity and shape together with structures such as the ‘second knee’ at the sub-EeV energy, in addition to the well-known ‘knee’ and ‘ankle’. Although it is appreciated that spectral measurements are subject to systematic as well as random errors, we consider that contemporary data are good enough to allow at least some progress in this new field. These aspects are examined for particles of all energies and it is shown that they can constrain some parameters of the proposed models. In the search for origin above PeV energies, we conclude that shocks in the galactic halo, whatever their source (galactic wind, relativistic plasmoids—‘cannonballs’, multiple shocks from supernovae etc) are most likely, pulsars such as B0656+14 and hypernovae come a close second although such a suggestion is not without its difficulties. What is most important is that trapping of particles in the halo is needed to reduce irregularities of the energy spectra both below and above the ‘knee’ caused by the stochastic nature of supernova explosions and other potential (discrete) galactic sources. We argue that precise experimental studies of spectral ‘irregularities’ will provide considerable help in the search for cosmic ray origin.

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“…Other functional forms have also been used; e.g., two parts of Gaussian functions with two different widths σ l and σ 2 are used for t < t m and t > t m , respectively, [31]; or other forms [24], for example, the above-mentioned parametrization using the width of the distribution [20]. A wellknown Gaisser-Hillas formula was introduced in [30] to describe the mean particle number in a vertical shower generated by a proton of energy E 0 ≥ 10 15 eV.…”

Section: Some General Problems For Uhe Cascadesmentioning

confidence: 99%

The exponential-normal form and its application to ultra high energy cascades investigation

Kirillov¹,

Kirillov²

2009

Monte Carlo Methods and Applications

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The normalized exponential-normal form A · exp(−(x − c) 2 /(a(x − c) + 2b 2 )) is an asymmetric distribution intermediate between the normal and exponential distributions. Some properties of the form are presented and some methods of approximation are suggested. Appropriate formulae and table are presented. The quality of original data defines the specific features of the methods. Application of the methods is illustrated by ultra high energy atmospheric showers investigation. The relation to the exponential and normal distributions makes the form useful and effective in applications.

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Low Energy Cosmic Ray Nuclei and their Propagation in the Galaxy

Cited by 3 publications

References 21 publications

Energy spectra of electrons in the extensive air showers of ultra-high energy

Energy spectra of electrons in the extensive air showers of ultra-high energy

The origin of cosmic rays

The exponential-normal form and its application to ultra high energy cascades investigation

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