22 research outputs found
Diffuse Gamma Rays from the Galactic Plane in the TeV region
Abstract The diffuse gamma rays beyond 1 TeV from the Galactic plane have been considered as mainly due to the inverse Compton(IC) scattering of the interstellar photons with the high-energy cosmic-ray electrons. In the recent studies of the evolution of SNR, the electron spectrum inside the SNR at the high energy side are suppressed by the synchrotron loss or the insufficient time for the acceleration. The electron spectrum is approximated as the power law spectrum with exponential form of . We calculate the diffuse gamma-ray spectrum for E max =10,20,50,100 TeV, and discuss the significance of these results by comparing with the gamma-ray flux observed by experiments. In addition to these IC gamma rays by the interstellar electrons, the electrons inside the sources also contribute significantly to the high-energy gamma rays
Observations of High Energy Cosmic-Ray Electrons from 30 GeV to 3 TeV with Emulsion Chambers
We have performed a series of cosmic-ray electron observations using the
balloon-borne emulsion chambers since 1968. While we previously reported the
results from subsets of the exposures, the final results of the total exposures
up to 2001 are presented here. Our successive experiments have yielded the
total exposure of 8.19 m^2 sr day at the altitudes of 4.0 - 9.4 g/cm^2. The
performance of the emulsion chambers was examined by accelerator beam tests and
Monte-Carlo simulations, and the on-board calibrations were carried out by
using the flight data. In this work we present the cosmic-ray electron spectrum
in the energy range from 30 GeV to 3 TeV at the top of the atmosphere, which is
well represented by a power-law function with an index of -3.28+-0.10. The
observed data can be also interpreted in terms of diffusive propagation models.
The evidence of cosmic-ray electrons up to 3 TeV suggests the existence of
cosmic-ray electron sources at distances within ~1 kpc and times within ~1x10^5
yr ago.Comment: 38 pages, 10 figures, 3 tables, Accepted for publication in Ap
High energy electron observation by Polar Patrol Balloon flight in Antarctica
We accomplished a balloon observation of the high-energy cosmic-ray electrons in 10-1000GeV to reveal the origin and the acceleration mechanism. The observation was carried out for 13 days at an average altitude of 35km by the Polar Patrol Balloon (PPB) around Antarctica in January 2004. The detector is an imaging calorimeter composed of scintillating-fiber belts and plastic scintillation counters sandwiched between lead plates. The geometrical factor is about 600cm^2sr, and the total thickness of lead absorber is 9 radiation lengths. The performance of the detector has been confirmed by a test flight at the Sanriku Balloon Center and by an accelerator beam test using the CERN-SPS (Super Proton Synchrotron at CERN). The new telemetry system using the Iridium satellite, the power system supplied by solar panels and the automatic flight level control operated successfully during the flight. We collected 5.7×10^3 events over 100GeV, and selected the electron candidates by a preliminary data analysis of the shower images. We report here an outline of both detector and observation, and the first result of the electron energy spectrum over 100GeV obtained by an electronic counter