Results 261 to 270 of about 250,180 (275)

Low-Temperature Neutron Moderation

Physical Review Letters, 1960
Measurements on an energy level in the microwave spectrum of water are discussed. The inelastic cross section for scattering of 0.005 ev neutrons from HO/sub 1/2/ at room temperature was estimated to be 8 barns. (C.J.G.)
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Neutron temperature measurements with 176Lu

Journal of Nuclear Energy. Part A. Reactor Science, 1959
A relative calibration of the Lu/sup 176/(n, gamma y) reaction is reported. It was found that the Lu/sup 176/(n, gamma ) reaction is potentially capable of measuring neutron temperature in the 0 to 110 deg C range to about 5 deg C. (C.J.G.)
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On the growth of temperature within neutron stars [PDF]

Astrophysics, 1979
Analytic expressions are obtained that describe the variation of the temperature in the degenerate layers of the shell of a neutron star with electron heat conduction. The relativistic expression is used for the coefficient of thermal conductivity, and a possible crystallization of the ions is taken into account. For a neutron star with solar mass of 1
D. G. Yakovlev, V. A. Urpin
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Neutron Diffraction Study of Water At High Temperature

Europhysics Letters (EPL), 1992
Neutron diffraction measurements on water at T = 523 K are presented. The comparison with room temperature data shows an evident weakening of the tetrahedral coordination. This effect has been accurately simulated by an ensemble of polarizable water molecules, interacting via the NEMO (Non Empirical Molecular Orbital) potential model.
U. Buontempo, POSTORINO, Paolo, M. A. Ricci, A. K. Soper   +3 more
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Neutron scattering at nK temperatures

Neutron News, 1991
Abstract The study of nuclear magnetic order in Copper is the most ambitious and difficult neutron scattering experiment ever performed at Ris⊘. Beside expensive hardware, approximately 50man-months of scientific work, 24 months of beam time and 10000 litres of liquid He had to be invested before we could even expect to discover whether the experiment ...
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Internal Neutronics-Temperature Coupling in Serpent 2

Nuclear Science and Engineering, 2014
This paper describes the built-in calculation routines in the reactor physics code Serpent 2 that provide a novel method for solving the coupled problem of the power distribution, temperature distribution, and material property distributions in nuclear fuel elements.
Jaakko Leppänen, Tuomas Viitanen, Ville Valtavirta   +2 more
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Effects of temperature on the structure of neutron stars at high temperature

General Relativity and Gravitation, 2017
In Newtonian physics, higher temperature leads to higher thermal pressure, which provides stronger support against the gravitational contraction of stars. However, in the temperature range of tens of MeV involved in the evolution of a proto-neutron star or a higher massive neutron star, the effects of temperature are richer.
Liang-gui Zhu, Jun-Li Lu, Li Wang
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Low temperature neutron irradiation of niobium

Scripta Metallurgica, 1976
A study was made to determine the effect of low temperature neutron irradiation and post-irradiation annealing on the yield stress of low and intermediate oxygen content niobium. The results are compared with previous results to determine the type of neutron-produced defect that causes the changes in the yield stress. 12 references. (JFP)
F Vanoni, R.J. Arsenault
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A low-temperature Weissenberg camera for neutrons

Journal of Applied Crystallography, 1981
The construction and performance of a neutron Weissenberg camera for temperatures down to 4 K is described. Exposure times are similar to the X-ray case. The background from the cryostat walls can be eliminated. Examples of applications in the fields of magnetic structures which are incommensurate with their chemical unit cells, crystallographic phase ...
D. Hohlwein, A. F. Wright
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Neutron Capture Data at Stellar Temperatures

Reviews of Modern Physics, 1965
Neutron capture cross sections are averaged over Maxwell-Boltzmann neutron distributions for temperatures pertinent to slow nucleosynthesis ($s$ process) in red giant stars. Such cross sections, together with isotopic abundances, provide the major quantitative experimental tests of the theory.
J. H. Gibbons, R. L. Macklin
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