Calculational Procedure for Evaluating Time- and Spatial-Dependent Energy Deposition in Air for Anisotropic Nuclear Sources: Volume IV. Secondary Gamma-Ray Data for Isotropic Neutron Sources.

1979 ◽  
Author(s):  
M. B. Wells ◽  
R. B. Livesay
Keyword(s):  
Energy Deposition ◽  
Gamma Ray ◽  
Neutron Sources ◽  
Calculational Procedure

Gamma Ray Attenuation Coefficient Measurement in Energies 1172 keV and 1332 keV for Neutron Absorbent Saturated Solutions

2006 ◽  
Author(s):  
Majid Jalali
Keyword(s):  
Attenuation Coefficient ◽  
Gamma Rays ◽  
Gamma Ray ◽  
Neutron Absorption ◽  
Attenuation Coefficients ◽  
Neutron Sources ◽  
Coefficient Measurement ◽  
Gamma Ray Attenuation ◽  
Mass Attenuation Coefficients ◽  
Saturated Solutions

The compounds, Na2B4O7, H3BO3, CdCl2 and NaCl and their solutions, attenuate gamma rays in addition to neutron absorption. These compounds are widely used in shielding of neutron sources, reactor control and neutron converters. Mass attenuation coefficients of gamma related to saturated solutions of the above four compounds, in energies 1172 keV and 1332 keV have been measured by NaI detector and agree very well with the results obtained by Xcom code. Experiment and computation show that, H3BO3 has the highest gamma ray attenuation coefficient among the aforementioned compounds.

scholarly journals Neutron Star Mergers, Disks Around Black Holes, and Gamma-Ray Bursts

1997 ◽  
Vol 163 ◽  
pp. 384-387 ◽  
Author(s):  
H.-Th. Janka ◽  
M. Ruffert
Keyword(s):  
Neutron Stars ◽  
Energy Deposition ◽  
Gamma Ray ◽  
Three Dimensional ◽  
Energy Output ◽  
Central Black Hole ◽  
Order Of Magnitude ◽  
Hydrodynamical Simulations ◽  
Piecewise Parabolic ◽  
Favorable Conditions

AbstractWe have performed three-dimensional hydrodynamical simulations of the coalescence of binary neutron stars taking into account the emission and backreaction of gravitational waves in the Newtonian code based on the “Piecewise Parabolic Method”. The use of the physical equation of state (EOS) of Lattimer & Swesty (1991) allowed us to calculate the production of neutrinos. We evaluated our models for the efficiency of v⊽ annihilation in the surroundings of the coalescing neutron stars. The corresponding energy deposition prior to and during merging turned out to be 2–3 orders of magnitude too small to power a typical γ-ray burst (GRB) with an energy output of ~ (1051/4π) erg/sterad at cosmological distances. Analytical estimates of the subsequent evolution of the disk which possibly surrounds the central black hole showed that even under the most favorable conditions the energy provided by v⊽ → e−e+ → γγ falls short by at least an order of magnitude. We discuss the implications of our results and speculate about possibilities how v⊽ annihilation might still be a viable energy source for GRBs.

Gamma-Ray Energy Deposition Measurements in the Fast Breeder Blanket Facility

1986 ◽  
Vol 92 (4) ◽  
pp. 596-605 ◽  
Author(s):  
K. R. Koch ◽  
F. M. Clikeman ◽  
R. H. Johnson
Keyword(s):  
Energy Deposition ◽  
Gamma Ray

Gamma-Ray Energy Deposition in Silicon Detectors

1975 ◽  
Vol 22 (6) ◽  
pp. 2582-2585 ◽  
Author(s):  
N. A. Lurie ◽  
D. K. Steinman ◽  
L. Harris ◽  
J. P. Wondra
Keyword(s):  
Energy Deposition ◽  
Gamma Ray ◽  
Silicon Detectors
Sign in / Sign up

Export Citation Format

Share Document