Fine Structure on the Sun at 2.8 cm.

1976 ◽  
Author(s):  
C. John Grebenkemper
Keyword(s):  
Fine Structure ◽  
The Sun

Salyut-4 Observations of Active Regions on the Sun

1977 ◽  
Vol 36 ◽  
pp. 333-367 ◽  
Author(s):  
A.V. Bruns ◽  
G.M. Grechko ◽  
A.A. Gubarev ◽  
P.I. Klimuk ◽  
V.I. Sevastyanov ◽  
...  
Keyword(s):  
Fine Structure ◽  
Spatial Resolution ◽  
Physical State ◽  
High Spatial Resolution ◽  
Solar Spectrum ◽  
Active Regions ◽  
Spectral Lines ◽  
The Sun ◽  
Solar Image ◽  
Solar Plasma

We believe that the examination of the ultraviolet solar spectrum is the most informative tool for the diagnostic of the physical state of the solar plasma. But the well known phenomenon of fine structure of active regions (A.R.), as well as of quiet ones, making spectral lines to be wavy and patchy (across dispersion) demandsa) high spatial resolution on the solar image and b) stigmatic spectra.

Fine Structure of the Sun at Centimeter Wavelengths

1974 ◽  
pp. 65-68 ◽  
Author(s):  
M. R. Kundu ◽  
T. Velusamy ◽  
R. H. Becker
Keyword(s):  
Fine Structure ◽  
The Sun

Fine structure on the Sun

Nature ◽  
1990 ◽  
Vol 344 (6269) ◽  
pp. 815-816
Author(s):  
Nigel Weiss
Keyword(s):  
Fine Structure ◽  
The Sun

On the Reality of Magnetic Fine Structure

1971 ◽  
Vol 43 ◽  
pp. 316-322 ◽  
Author(s):  
Constance Sawyer
Keyword(s):  
Magnetic Field ◽  
Fine Structure ◽  
Solar Observatory ◽  
The Sun ◽  
Magnetic Elements ◽  
Cast Doubt ◽  
The Many ◽  
Salt And Pepper

On filter magnetograms of the Sun made at Lockheed Solar Observatory, small mottles create a salt-and-pepper appearance. Outside plages, the surface seems to be sprinkled with little magnetic elements, with opposite polarities intermingled. The many steps of the photographic subtraction process required to make these elements visible tend to cast doubt on their reality. Independent and stronger evidence for the quantization of magnetic field, recently presented by Livingston and Harvey (1969), stimulates an effort to define more carefully the characteristics of the elements seen on filter magnetograms. The purpose of this contribution is to show that these characteristics are compatible with those of the elements observed at Kitt Peak.

Fine Structure of the Sun at Centimeter Wavelengths

1974 ◽  
Vol 56 ◽  
pp. 65-68
Author(s):  
M. R. Kundu ◽  
T. Velusamy ◽  
R. H. Becker
Keyword(s):  
Fine Structure ◽  
Brightness Temperature ◽  
Angular Size ◽  
Gradual Decrease ◽  
Peak Amplitude ◽  
The Sun ◽  
Quiet Sun

The Hat Creek Observatory's two-element interferometer and the NRAO 3–element interferometer have been used at 1.3, 3.7– and 11.1–cm wavelengths respectively, to study the fine structure of the radio emissive regions on the Sun. Observations of the quiet Sun at 1.3 cm show sudden increases followed by a gradual decrease in the fringe amplitude lasting for typically about 5–8 min. Assuming these events are identical in nature, a plot of peak amplitude against the projected baseline at the time of the event suggests emission from a region of angular size of about 10″. The corresponding brightness temperature is 50000 K. It is possible that these events may be related to the appearance and disappearance of groups of spicules or mottles.

scholarly journals 13. The processes in active regions on the sun and electromagnetics

1958 ◽  
Vol 6 ◽  
pp. 114-122
Author(s):  
A. B. Severny
Keyword(s):  
Fine Structure ◽  
Shock Waves ◽  
Observational Data ◽  
Spectroscopic Data ◽  
Active Regions ◽  
The Sun ◽  
Continuous Emission ◽  
And Shock Waves ◽  
Observational Aspect

1. Brief summary of the dynamics of flare development, based on the analysis of moving picture and spectroscopic data. Some new spectroscopic data on the fine structure of emission in active regions, evidencing the peculiar character of motions in them: outbursts of corpuscules, ascending grains of continuous emission, explosive processes and shock-waves.2. Summary of the observational data on the motions in prominences. Regular electromagnetic and turbulent motions, ‘explosive’ motions and their admissible interpretation. Some data on the coronal forms above active regions and on the possible role of hydromagnetics in their formation.3. Some remarks on the role of hydromagnetics, admissible, from the observational aspect.

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