Fine structure of the skin of the amphibious fishes,Boleophthalmus pectinirostris andPeriophthalmus cantonensis, with special reference to the location of blood vessels

1992 ◽  
Vol 214 (3) ◽  
pp. 287-297 ◽  
Author(s):  
Sachihiko Yokoya ◽  
Osamu S. Tamura
Keyword(s):  
Fine Structure ◽  
Special Reference ◽  
Blood Vessels ◽  
Boleophthalmus Pectinirostris ◽  
Amphibious Fishes

The fine structure of blood vessels in chromophobe adenoma

1972 ◽  
Vol 22 (3) ◽  
pp. 200-207 ◽  
Author(s):  
Asao Hirano ◽  
Uwamie Tomiyasu ◽  
H. M. Zimmerman
Keyword(s):  
Fine Structure ◽  
Blood Vessels ◽  
Chromophobe Adenoma

Fine structure of prolactin pituitary adenoma with special reference to annulate lamellae

1979 ◽  
Vol 46 (1-2) ◽  
pp. 163-166 ◽  
Author(s):  
M. Scanarini ◽  
R. Giordano ◽  
S. Mingrino ◽  
N. Pennelli
Keyword(s):  
Fine Structure ◽  
Pituitary Adenoma ◽  
Special Reference ◽  
Annulate Lamellae

A Discussion on solar studies with special reference to space observations - The manifold structure of the chromosphere and corona

1971 ◽  
Vol 270 (1202) ◽  
pp. 77-80 ◽  
Keyword(s):  
Magnetic Field ◽  
Fine Structure ◽  
High Resolution ◽  
Field Strength ◽  
Special Reference ◽  
Velocity Fields ◽  
Field Patterns ◽  
Uniform Region ◽  
Determining Factor ◽  
The Magnetic Field

Although the photosphere is a uniform region for scales greater than the granulation, the fact that the magnetic field strength falls off less sharply than the gas pressure leads to strong magnetic influence at greater heights in the solar atmosphere. This magnetic influence leads to non-uniformity and fine structure in the chromosphere and corona. The existence of such structure has been deduced mostly from measurements of photospheric phenomena; in particular, from measurements of photospheric velocity fields (Leighton, Noyes & Simon 1962) and of photospheric magnetic fields (Bumba & Howard 1965). The determining factor would thus appear to be in the photosphere; but visible effects only are produced in the chromosphere and corona. In recent years, high resolution filter photography has enabled us to recognize different regions of the chromosphere, where qualitatively different structure is associated with distinct magnetic field patterns. This progress has been possible because of better Lyot filters, better films and better observing sites; the spectroheliograph has always been limited for high resolution work by the finite slit width and the difficulty of accurate guiding during the long exposures.

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