Proposed Experimental Investigation of Uncertainty Relations by Measuring the Velocity Dispersion of Localized Neutrons

1986 ◽  
Vol 480 (1 New Technique) ◽  
pp. 607-610
Author(s):  
J. SCHEER ◽  
M. SCHMIDT
2016 ◽  
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Xiang Zhan ◽  
Zhihao Bian ◽  
Jian Li ◽  
Yongsheng Zhang ◽  
...  

2019 ◽  
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Jun-Li Li ◽  
Shuang Wang ◽  
Qiu-Cheng Song ◽  
Cong-Feng Qiao

2017 ◽  
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Jun-Li Li ◽  
Qiu-Cheng Song ◽  
Hui Wang ◽  
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...  

2020 ◽  
Vol 101 (3) ◽  
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Huan Yang ◽  
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2020 ◽  
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...  

1967 ◽  
Vol 31 ◽  
pp. 265-278 ◽  
Author(s):  
A. Blaauw ◽  
I. Fejes ◽  
C. R. Tolbert ◽  
A. N. M. Hulsbosch ◽  
E. Raimond

Earlier investigations have shown that there is a preponderance of negative velocities in the hydrogen gas at high latitudes, and that in certain areas very little low-velocity gas occurs. In the region 100° <l< 250°, + 40° <b< + 85°, there appears to be a disturbance, with velocities between - 30 and - 80 km/sec. This ‘streaming’ involves about 3000 (r/100)2solar masses (rin pc). In the same region there is a low surface density at low velocities (|V| < 30 km/sec). About 40% of the gas in the disturbance is in the form of separate concentrations superimposed on a relatively smooth background. The number of these concentrations as a function of velocity remains constant from - 30 to - 60 km/sec but drops rapidly at higher negative velocities. The velocity dispersion in the concentrations varies little about 6·2 km/sec. Concentrations at positive velocities are much less abundant.


1967 ◽  
Vol 31 ◽  
pp. 45-46
Author(s):  
Carl Heiles

High-resolution 21-cm line observations in a region aroundlII= 120°,b11= +15°, have revealed four types of structure in the interstellar hydrogen: a smooth background, large sheets of density 2 atoms cm-3, clouds occurring mostly in groups, and ‘Cloudlets’ of a few solar masses and a few parsecs in size; the velocity dispersion in the Cloudlets is only 1 km/sec. Strong temperature variations in the gas are in evidence.


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