scholarly journals The Mechanism Responsible for 'Shadow' Type III Solar Radio Bursts. II. Absorption due to Ion Sound Turbulence

1974 ◽  
Vol 27 (2) ◽  
pp. 271 ◽  
Author(s):  
DB Melrose
Keyword(s):  
Energy Density ◽  
Solar Radio ◽  
Plasma Frequency ◽  
Radio Bursts ◽  
Sound Waves ◽  
Solar Radio Bursts ◽  
Langmuir Waves ◽  
Transverse Waves ◽  
Type Iii ◽  
Ion Plasma

The hypothesis is explored that ion sound turbulence generated by the exciting agency for type III bursts is responsible for shadow type III events. The possible absorption mechanisms are listed: the most favourable are the coalescence of transverse waves and ion sound waves into Langmuir waves or the decay of transverse waves into Langmuir waves and ion sound waves. These mechanisms can operate only if the background source emits at the fundamental plasma frequency and the absorbing region is directly above it (;$ 3 x 104 km). It is found that the event discussed by Kai (1973) can be explained in terms of such absorption with reasonable parameters, e.g. with an energy density in ion sound turbulence W' ~ 10-12 ergcm- 3 at frequencies co' ~ O�3cop! (where cop! is the ion plasma frequency).

Nonlinear Langmuir waves during Type III solar radio bursts

1978 ◽  
Vol 223 ◽  
pp. 605 ◽  
Author(s):  
D. R. Nicholson ◽  
M. V. Goldman ◽  
P. Hoyng ◽  
J. C. Weatherall
Keyword(s):  
Solar Radio ◽  
Radio Bursts ◽  
Solar Radio Bursts ◽  
Langmuir Waves ◽  
Type Iii

scholarly journals High Resolution Studies of Type III Solar Radio Bursts

1974 ◽  
Vol 57 ◽  
pp. 225-226
Author(s):  
C. Chiuderi ◽  
R. Giachetti ◽  
C. Mercier ◽  
H. Rosenberg ◽  
C. Slottje
Keyword(s):  
Solar Radio ◽  
Plasma Frequency ◽  
Solar Radius ◽  
Average Height ◽  
Radio Bursts ◽  
General Shape ◽  
Solar Radio Bursts ◽  
Type Iii ◽  
Temporal And Spatial ◽  
East West

(Solar Phys.). High spectral, temporal and spatial resolution observations were obtained with the 60-channel Utrecht solar radio spectrograph (160–320 MHz) and the 169 MHz Nançay solar radioheliograph. From a large number of type III bursts the average height was found to be 0.37 solar radius above the photosphere, corresponding to approximately the Newkirk streamer density, if the bursts are emitted at the harmonic of the local plasma frequency. No center-to-limb variation, nor east-west asymmetry was observed. All double bursts, double humped bursts, precursor-type III had exactly the same position and general shape for both members of the pair. From this it was concluded that fundamental-harmonic pairs are very rare at frequencies above 160 MHz (Mercier and Rosenberg, 1974).

On the Fundamental and Harmonic Components of Low-Frequency Type III Solar Radio Bursts

1982 ◽  
Vol 4 (4) ◽  
pp. 382-386 ◽  
Author(s):  
S. Suzuki ◽  
K.V. Sheridan
Keyword(s):  
Solar Radio ◽  
Plasma Frequency ◽  
Low Frequency ◽  
Radio Bursts ◽  
Solar Radio Bursts ◽  
Type Iii ◽  
Field Lines ◽  
Harmonic Components ◽  
Electro Magnetic ◽  
Open Magnetic Field

Ground-based observations of Type III bursts made with spectrographs and spectro-polarimeters, at frequencies above the ionospheric cut-off, reveal that most bursts (excluding storm Type IIIs) have fundamental (F) and harmonic (H) structure (Wild et al. 1959; Dulk and Suzuki 1980). An example of F-H bursts is given by Sheridan (1978). Such bursts are produced by streams of electrons travelling along open magnetic field lines and exciting plasma oscillations which are converted to electro-magnetic waves at both the F and H frequencies of the local plasma frequency in the corona.

Can Spontaneously Emitted Langmuir Waves Account for Type III Solar Radio Bursts?

1976 ◽  
Vol 3 (1) ◽  
pp. 43-45 ◽  
Author(s):  
D. B. Melrose
Keyword(s):  
Solar Radio ◽  
The Other ◽  
Radio Bursts ◽  
Solar Radio Bursts ◽  
Langmuir Waves ◽  
Type Iii ◽  
Other Hand ◽  
The One ◽  
Stream Instability

One of the major problems in the theory of type III solar radio bursts concerns the development of the two-stream instability. On the one hand, Sturrock (1964) argued that one expects the instability to develop rapidly, and if it does it should prevent the stream from propagating through the corona, contrary to observation. On the other hand, one appears to require that the instability develop partially, in the sense that there is some significant amplified emission of Langmuir waves, in order to account for the observed emission.

Emission of type III solar radio bursts by two oppositely propagating langmuir waves

2001 ◽  
Author(s):  
M. Virgı́nia Alves ◽  
M. A. E. de Moraes ◽  
J. R. Abalde ◽  
A. C.-L. Chian ◽  
F. B. Rizzato
Keyword(s):  
Solar Radio ◽  
Radio Bursts ◽  
Solar Radio Bursts ◽  
Langmuir Waves ◽  
Type Iii

Electron Exciter Speeds Associated with Interplanetary Type III Solar Radio Bursts

Solar Physics ◽  
2015 ◽  
Vol 290 (10) ◽  
pp. 2975-3004 ◽  
Author(s):  
M. J. Reiner ◽  
R. J. MacDowall
Keyword(s):  
Solar Radio ◽  
Radio Bursts ◽  
Solar Radio Bursts ◽  
Type Iii

A Theory of Type III Solar Radio Bursts

1974 ◽  
pp. 283-283
Author(s):  
V. V. Zaitsev ◽  
N. A. Mityakov ◽  
V. O. Rapoport
Keyword(s):  
Solar Radio ◽  
Radio Bursts ◽  
Solar Radio Bursts ◽  
Type Iii

scholarly journals The Polarization Structure of Type III Solar Radio Bursts

1965 ◽  
Vol 18 (3) ◽  
pp. 283 ◽  
Author(s):  
UV Gopala Rao
Keyword(s):  
Solar Radio ◽  
Great Majority ◽  
Radio Bursts ◽  
Solar Radio Bursts ◽  
Polarization Structure ◽  
Type Iii ◽  
Double Structure ◽  
Strong Polarization ◽  
Diffuse Background

The polarization of type III bursts was measured, using a swept.phase technique, at 40 and 60 Mc/s. The great majority of type III bursts show slight to moderate polarization. The results indicate a double structure for the type III burst-a sharp, intense, drifting feature with relatively strong polarization, and a diffuse background of longer duration with relatively weak or zero polarization.

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