Propagation and source energy spectra of cosmic ray nuclei at high energies

42Citations
Citations of this article
13Readers
Mendeley users who have this article in their library.

Abstract

A recent measurement of the TRACER instrument on long-duration balloon has determined the individual energy spectra of the major primary cosmic ray nuclei from oxygen (Z = 8) to iron (Z = 26). The measurements cover a large range of energies and extend to energies beyond 1014 eV. We investigate if the data set can be described by a simple but plausible model for acceleration and propagation of cosmic rays. The model assumes a power-law energy spectrum at the source with a common spectral index α for all nuclear species, and an energy-dependent propagation path length (Λ E -0.6) combined with an energy-independent residual path length Λ0. We find that the data can be fitted with a fairly soft source spectrum (α = 2.3-2.4), and with a residual path length Λ0 as high as 0.3 g cm-2. We discuss this model in the context of other pertinent information, and we determine the relative abundances of the elements at the cosmic ray source. © 2009. The American Astronomical Society.

Cite

CITATION STYLE

APA

Ave, M., Boyle, P. J., Höppner, C., Marshall, J., & Müller, D. (2009). Propagation and source energy spectra of cosmic ray nuclei at high energies. Astrophysical Journal, 697(1), 106–114. https://doi.org/10.1088/0004-637X/697/1/106

Register to see more suggestions

Mendeley helps you to discover research relevant for your work.

Already have an account?

Save time finding and organizing research with Mendeley

Sign up for free