GAMMA RAYS FROM THE DEUTERON BOMBARDMENT OF BORON 10

1955 ◽  
Vol 33 (12) ◽  
pp. 828-840 ◽  
Author(s):  
J. T. Sample ◽  
G. C. Neilson ◽  
G. B. Chadwick ◽  
J. B. Warren
Keyword(s):  
Energy Level ◽  
Cross Section ◽  
Gamma Rays ◽  
High Energy ◽  
Crystal Spectrometer ◽  
Upper Limit ◽  
Very High Energy ◽  
Deuteron Bombardment ◽  
Bombarding Energy ◽  
Very High

Bombardment of B10 with 1.4 Mev. deuterons has been found to produce gamma rays of energy 4.46 ±.04, 4.75 ±.03, 5.03 ±.09, 5.35 ±.05, 6.52 ±.04, 6.78 ±.07, 7.29 ±.04, 8.27 ±.09, and 8.87 ±.02 Mev., as measured with a three-crystal pair spectrometer. Tentative assignments to transitions in B11 and C11 agree well in most cases with the known energy level schemes. No gamma rays of very high energy were observed, even with a single-crystal spectrometer; consequently an upper limit of 10−31 cm.2 has been placed on the cross-section of B10(d, γ)C12 at 0.95 Mev. bombarding energy.

scholarly journals Cross section to multiplicity ratios at very high energy

2014 ◽  
Vol 734 ◽  
pp. 207-209 ◽  
Author(s):  
M.M. Block ◽  
L. Stodolsky
Keyword(s):  
Cross Section ◽  
High Energy ◽  
Very High Energy ◽  
Very High

Deflectometric measurement of large mirrors

2014 ◽  
Vol 3 (3) ◽  
Author(s):  
Evelyn Olesch ◽  
Gerd Häusler ◽  
André Wörnlein ◽  
Friedrich Stinzing ◽  
Christopher van Eldik
Keyword(s):  
Gamma Rays ◽  
High Energy ◽  
Spherical Mirror ◽  
Large Space ◽  
Telescope Array ◽  
Spread Function ◽  
Very High Energy ◽  
Energy Gamma ◽  
Concentric Geometry ◽  
Very High

AbstractWe discuss the inspection of large-sized, spherical mirror tiles by ‘Phase Measuring Deflectometry’ (PMD). About 10 000 of such mirror tiles, each satisfying strict requirements regarding the spatial extent of the point-spread-function (PSF), are planned to be installed on the Cherenkov Telescope Array (CTA), a future ground-based instrument to observe the sky in very high energy gamma-rays. Owing to their large radii of curvature of up to 60 m, a direct PSF measurement of these mirrors with concentric geometry requires large space. We present a PMD sensor with a footprint of only 5×2×1.2 m

Very high energy gamma rays from x-ray binary pulsars

1990 ◽  
Vol 16 (12) ◽  
pp. 1773-1803 ◽  
Author(s):  
P M Chadwick ◽  
T J L McComb ◽  
K E Turver
Keyword(s):  
Gamma Rays ◽  
High Energy ◽  
X Ray ◽  
Binary Pulsars ◽  
High Energy Gamma ◽  
Very High Energy ◽  
Energy Gamma ◽  
Very High

RESULTS FROM GALACTIC OBSERVATIONS WITH MAGIC

2010 ◽  
Vol 19 (06) ◽  
pp. 1023-1029
Author(s):  
◽  
JAVIER RICO
Keyword(s):  
Gamma Rays ◽  
Energy Band ◽  
Binary Systems ◽  
High Energy ◽  
Cherenkov Telescope ◽  
La Palma ◽  
Very High Energy ◽  
Energy Gamma ◽  
High Energy Emission ◽  
Very High

MAGIC is a single-dish Cherenkov telescope located on La Palma (Spain), hence with an optimal view on the Northern sky. Sensitive to the 30 GeV–30 TeV energy band, it is nowadays the only ground-based instrument being able to measure high-energy gamma-rays below 100 GeV. With the operation in coincidence with MACIC-II, starting in Fall 2009, the sensitivity will be improved by a factor ~ 2. We review the results obtained by MAGIC on the very-high energy emission from pulsars, binary systems and microquasars.

scholarly journals Recent Results from the CANGAROO Project

1996 ◽  
Vol 160 ◽  
pp. 363-364
Author(s):  
S.A. Dazeley ◽  
P.G. Edwards ◽  
J.R. Patterson ◽  
G.P. Rowell ◽  
M. Sinnott ◽  
...  
Keyword(s):  
Gamma Rays ◽  
South Australia ◽  
Cosmic Ray ◽  
High Energy ◽  
Relativistic Electrons ◽  
Large Numbers ◽  
Inverse Compton ◽  
Very High Energy ◽  
Large Telescopes ◽  
Very High

TheCollaboration ofAustralia andNippon for aGAmmaRayObservatory in theOutback operates two large telescopes at Woomera (South Australia), which detect the Čerenkov light images produced in the atmosphere by electronpositron cascades initiated by very high energy (~1 TeV or 1012eV) gamma rays. These gamma rays arise from a different mechanism than at EGRET energies: inverse Compton (IC) emission from relativistic electrons.The spoke-like images are recorded by a multi-pixel camera which facilitates the rejection of the large numbers of oblique and ragged cosmic ray images. A field of view ~3.5° is required. The Australian team operates a triple 4 m diameter mirror telescope, BIGRAT, with a 37 photomultiplier tube camera and energy threshold 600 GeV. The Japanese operate a single, highly accurate 3.8 m diameter f/1 telescope and high resolution 256 photomultipler tube camera. In 1998 a new 7 m telescope is planned for Woomera with a design threshold ~;200GeV.

scholarly journals Very High Energy Gamma Rays from Plerions: CANGAROO Results

1998 ◽  
Vol 188 ◽  
pp. 125-128
Author(s):  
T. Kifune
Keyword(s):  
Gamma Rays ◽  
Gamma Ray ◽  
High Energy ◽  
Current Status ◽  
Emission Region ◽  
Thermal Processes ◽  
High Energy Gamma ◽  
Very High Energy ◽  
Energy Gamma ◽  
Very High

The current status of very high energy gamma ray astronomy (in ~ 1 TeV region) is described by using as example results of CANGAROO (Collaboration of Australia and Nippon for a GAmma Ray Observatory in the Outback). Gamma rays at TeV energies, emitted through inverse Compton effect of electrons or π0 decay from proton interaction, provide direct evidence on “hot” non-thermal processes of the Universe, as well as environmental features, such as the strength of magnetic field in the emission region, for the non-thermal processes.

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