supersonic zones
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2007 ◽  
Vol 42 (5) ◽  
pp. 844-850
Author(s):  
A. N. Kraiko ◽  
K. S. P’yankov
Keyword(s):  

1986 ◽  
Vol 89 ◽  
pp. 75-87 ◽  
Author(s):  
L.B. Lucy

In this review, attention will be focussed exclusively on the winds of hot stars, concentrating for the most part on spectral types 0 and B. For these stars, a clear consensus has emerged that it is the gradient of selective radiation pressure - i.e., line-driving - that explains the high terminal velocities, typically ~ 2000 km s−1, of their winds. Accordingly, few would now doubt that the supersonic zones of these winds present us with rather clean examples of line-driven flow, whose investigation therefore properly belongs under the heading “Radiation Hydrodynamics”. Moreover, in marked contrast with other astronomical environments where line-driven winds may exist, the stellar case is geometrically and parametrically well defined and is thus by far the best natural example from which to learn about such flows.


1970 ◽  
Vol 2 (1) ◽  
pp. 13-16 ◽  
Author(s):  
D. M. Voitenko ◽  
A. I. Zubkov ◽  
Yu. A. Panov

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