scholarly journals Parameters of the luminous region surrounding deuterium pellets in the PLT tokamak

1985 ◽  
Author(s):  
D.H. McNeill ◽  
G.J. Greene ◽  
D.D. Schuresko
Keyword(s):  
1985 ◽  
Vol 55 (13) ◽  
pp. 1398-1401 ◽  
Author(s):  
D. H. McNeill ◽  
G. J. Greene ◽  
D. D. Schuresko
Keyword(s):  

1861 ◽  
Vol 22 (1) ◽  
pp. 21-32
Author(s):  
William Swan

If we examine the flame arising from the combustion of any of the hydrocarbons, such as that of coal-gas, or of a common candle, it will be found to consist of several portions easily distinguishable by the eye, and in which the matter composing the flame exists in very different conditions. There is, first, a central non-luminous region, in which the gases are not yet ignited; secondly, a blue conoidal envelope, extending from the wick or burner, and gradually thinning out towards the top of the flame; thirdly, a more or less luminous conoid, thin towards the bottom of the flame, where it is enveloped by the blue conoid, but thicker towards the top. And fourthly, a faintly luminous outer envelope, completely surrounding the other portions of the flame, and greatly developed towards the top.


2003 ◽  
Vol 93 (1) ◽  
pp. 274-277 ◽  
Author(s):  
Y. Y. Kim ◽  
K. W. Lee ◽  
E. J. Ahn ◽  
S. Shim

1968 ◽  
Vol 46 (24) ◽  
pp. 2753-2754 ◽  
Author(s):  
D. D. Wallis ◽  
C. D. Anger

Measurements of a luminous region following two Black Brant II rockets are presented. This luminous region or wake appears as a circular cone of half angle 4° and length less than 1 km lying along the trajectory of the rocket, with vertex near the rocket. The wake was observed between 80 and 115 km at 4278 Å, but was not observed at 5577 Å.


Author(s):  
M Samadi ◽  
S Zanganeh ◽  
S Abbassi

Abstract The classical Bondi model is adopted to study accretion onto the finite luminous region around the central massive black hole (MBH) in an elliptical galaxy. Unlike Bondi (1952), we define the boundary conditions at a certain finite radius (rf) instead of at the infinity and examine the variation of solutions for a simple case. In the following, we consider the special case of a MBH at the center of a Hernquist galaxy and involve the gravity and luminosity of its own galaxy. Our results in the first part show that kinitic energy at the final radius is ignorable even for not so far away from the center. Moreover, the mass accretion rate will be approximately equal to its Bondi value if the final radius (rf) becomes about 2-3 orders of magnitude larger than semi-Bondi radius, i.e. $GM/c_{sf}^2$ (where M and csf are the mass of the central object and the sound speed at rf). In the second part, adding the two extra forces of gravity and radiation in the momentum equation let us know that the maximum possible of accretion rate increases with greater characteristic linear density of galaxy and lower radiation.


1998 ◽  
Vol 103 (D12) ◽  
pp. 14131-14134 ◽  
Author(s):  
N. Takagi ◽  
D. Wang ◽  
T. Watanabe ◽  
I. Arima ◽  
T. Takeuchi ◽  
...  

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