Measurement of primary cosmic-ray electrons and positrons from 4 to 50 GeV

Details Measurement of primary cosmic-ray electrons and positrons from 4 to 50 GeV Measurement of primary cosmic-ray electrons and positrons from 4 to 50 GeV

Aug 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...199..669b&link_type=abstract

Astrophysical Journal, vol. 199, Aug. 1, 1975, pt. 1, p. 669-679. Research supported by the University of California;

Astronomy and Astrophysics

Astrophysics

67

Bremsstrahlung, Cosmic Ray Showers, Electron Flux Density, Positrons, Primary Cosmic Rays, Abundance, Balloon-Borne Instruments, Data Acquisition, Data Reduction, Energy Spectra, Interstellar Matter

Scientific paper

We have used a bremsstrahlung-identification technique to measure electron and positron spectra in the primary cosmic rays from 4 to 50 GeV. Above our average geomagnetic cutoff of 4.0 GV/c, we find fluxes of 4.4 (plus or minus 0.3) electrons and 0.37 (plus or minus 0.09 positrons) per sq m/sr/sec. The electron events follow a differential power law whose spectral index is 2.8 (plus or minus 0.1). Our ratio electrons/(electrons + positrons) = 0.08 (plus or minus 0.02) implies traversal of an equivalent slab thickness of 4.3 (plus or minus 1.5) g/sq cm of interstellar and source material.

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