Electron Component of the Primary Cosmic Radiation at Energies ≳15 GeV

Daniel, R. R.; Stephens, S. A.

doi:10.1103/physrevlett.15.769

Cited by 50 publications

(20 citation statements)

References 5 publications

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“…The pioneering work using emulsions to detect highenergy electrons was Ðrst done by the Tata group (Daniel & Stephens 1965). They used emulsion stacks and detected electrons up to several hundred GeV.…”

Section: Introductionmentioning

confidence: 99%

The Energy Spectrum of Cosmic‐Ray Electrons from 10 to 100 GeV Observed with a Highly Granulated Imaging Calorimeter

Torii

Tamura

Tateyama

et al. 2001

ApJ

117

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Cosmic-ray electrons1 have been observed in the energy range from 12 to D100 GeV with a new balloon-borne payload, the Balloon-borne Electron Telescope with Scintillating Fibers (BETS). This is the Ðrst publication of the absolute energy spectrum of electrons measured with a highly granulated Ðber calorimeter. The calorimeter makes it possible to select electrons against the background protons by detailed observation of both the longitudinal and the lateral shower development. The performance of the detector was calibrated by the CERN-SPS accelerator beams : electrons from 5 to 100 GeV, protons from 60 to 250 GeV. The balloon observations were carried out twice, in 1997 and 1998, at the Sanriku Balloon Center (Institute of Space and Astronautical Science) in Japan. The observation time was D13 hr in all at an altitude above 34 km. A total of 1349 electron candidates were collected, and the 628 events with energies above 12.5 GeV, well above the geomagnetic rigidity cuto † of D10 GV, have been used to compose a di †erential absolute energy spectrum at the top of the atmosphere. The energy spectrum is described by a power-law index of 3.00^0.09, and the absolute di †erential intensity at 10 GeV is 0.199^0.015 m~2 s~1 sr~1 GeV~1. The overall shape of the energy spectrum in 10 D 100 GeV can be explained by a di †usion model, in which we assume an energy-dependent di †usion coefficient (PE0.3) for an injection spectrum, E~2.4.

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Section: Introductionmentioning

confidence: 99%

The Energy Spectrum of Cosmic‐Ray Electrons from 10 to 100 GeV Observed with a Highly Granulated Imaging Calorimeter

Torii

Tamura

Tateyama

et al. 2001

ApJ

117

View full text Add to dashboard Cite

show abstract

“…High energy electron-positron pairs are thought to be produced from the collisions of cosmic ray hadrons and gamma rays with interstellar gas, and the expected positron to electron ratio in cosmic rays arriving at Earth is roughly 10% and it decreases with energy. This picture is based on the experimental data collected over 35 years [19,[32][33][34] by balloon experiments as well as phenomenological model descriptions developed over the same period [20,35,36].…”

Section: Introductionmentioning

confidence: 99%

The Alpha Magnetic Spectrometer (AMS) on the International Space Station: Part I – results from the test flight on the space shuttle

Aguilar¹,

Alcaraz²,

et al. 2002

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“…Also shown are the electron measurements in the higher-energy region; not all observations known are included, but those a r e displayed that are the only data available in a given energy interval (Schmoker and Earl, 1965 Daniel and Stephens, 1965), the most recent data with the best statistics (L'Heureux and Meyer, 1965), and the original data (Earl, 1961, Meyer andVogt, 1961). It is inferred from the measurements on the positron to electron ratio (DeShong, Hildebrand andMeyer, 1964, Hartman, Meyer andHildebrand, 1965) that approximately one third to two thirds of the electrons in the 1…”

Section: Introduction and Discussion Of Observationsmentioning

confidence: 99%

“…In order to determine, (for case ii), the behavior of n ( y , t ) when a steady state prevails, we must investigate the rate of energy loss, of Agrinier, et al (1964) and Daniel and Stephens (1965) were converted to differential intensities by assuming a slope of -1.5 and an infinitely high cutoff.…”

Section: Appendixmentioning

confidence: 99%