scholarly journals Chains Of Type I Solar Radio Bursts

1966 ◽  
Vol 19 (5) ◽  
pp. 635 ◽  
Keyword(s):  
Solar Radio ◽  
Frequency Drift ◽  
Type I ◽  
Radio Bursts ◽  
Solar Radio Bursts ◽  
Frequency Rate

This paper reports statistical investigations of "chains" of type I bursts recorded with the Dapto radio spectrograph. Various characteristics of chains have been investigated, including their distribution with mid frequency, rate of frequency drift, posi

scholarly journals Satellite Observations of Solar Radio Bursts

1980 ◽  
Vol 86 ◽  
pp. 387-400
Author(s):  
J.L. Steinberg
Keyword(s):  
Solar Radio ◽  
Source Size ◽  
Type I ◽  
Radio Bursts ◽  
Solar Radio Bursts ◽  
Burst Source ◽  
Radiation Mechanism ◽  
3 Dimensional ◽  
Type Iii ◽  
Group Delays

Space observations of solar radio bursts have provided the following information:– From a single spacecraft:Measurements within the burst source or close to it: fundamental and harmonic type III radio emission, the corresponding plasma waves and spectra of the exciting electrons.– From a spacecraft and the earth or from two spacecrafts:A better evaluation of the influence of the ionosphere on some ground-based observations.Measurements of the beaming of the emission which yield constraints on the radiation mechanism and/or the role of coronal propagation in determining the source size and directivity (type I and III's).Measurements of the differential time delay which yield for type III:At short (m- and dam-) wavelengths, some evidence of group delays,At long (hm- and km-) wavelengths one coordinate of the source.Complete (3-dimensional) localization of the source at long wavelengths and therefore maps of the heliosphere magnetic field and electron density as well as the source size and, in the future, its polarization.The results of these observations and their interpretation are reviewed and discussed.

scholarly journals Fine Structure in the Spectra of Solar Radio Bursts

1969 ◽  
Vol 22 (2) ◽  
pp. 177 ◽  
Author(s):  
GRA Ellis
Keyword(s):  
Fine Structure ◽  
Radio Burst ◽  
Solar Radio ◽  
Type I ◽  
Radio Bursts ◽  
Frequency Range ◽  
Solar Radio Bursts ◽  
Mean Frequency ◽  
Addition Chains ◽  
Fast Drift

Observations are described of solar radio burst spectra in the frequency range 25-100 MHz with a time resolution of 0�02 sec. The types of bursts that were observed included (1) fast drift storm bursts with a mean frequency-time slope of 1�9 MHzsec-1, a mean bandwidth !!.f'"-' 0�03 MHz, and a mean duration !!.T of 0�6sec; (2) drift pair bursts with dffdt = 1�2MHzsec-1 and !!.f= 0�45 MHz; and (3) split pair bursts with dffdt = 0�08 MHzsec-1, !!.f = 0�05 MHz, and !!.T = 1�4 sec. In addition, chains of split pa.ir bursts were frequently observed, the chain resembling a type I burst with fine structure.

Positional drift within groups of Type I solar radio bursts

Solar Physics ◽  
1986 ◽  
Vol 103 (1) ◽  
pp. 129-140 ◽  
Author(s):  
J. Van Nieuwkoop
Keyword(s):  
Solar Radio ◽  
Type I ◽  
Radio Bursts ◽  
Solar Radio Bursts

scholarly journals EUV and Magnetic Activities Associated with Type-I Solar Radio Bursts

Solar Physics ◽  
2017 ◽  
Vol 292 (6) ◽  
Author(s):  
C. Y. Li ◽  
Y. Chen ◽  
B. Wang ◽  
G. P. Ruan ◽  
S. W. Feng ◽  
...  
Keyword(s):  
Solar Radio ◽  
Type I ◽  
Radio Bursts ◽  
Solar Radio Bursts

scholarly journals The Nature and Velocity of the Sources of Type II Solar Radio Bursts

1965 ◽  
Vol 18 (2) ◽  
pp. 167 ◽  
Author(s):  
The Late AA Weiss
Keyword(s):  
Magnetic Field ◽  
Speed Of Sound ◽  
Solar Radio ◽  
Frequency Drift ◽  
Radio Bursts ◽  
Type Ii ◽  
Solar Radio Bursts ◽  
Harmonic Emission ◽  
Band Splitting ◽  
Standard Density

Velocities of the sources of type II bursts are derived from rates of frequency drift using standard density models, both statistically for 21 bursts, and individually for 5 bursts extending over wide frequency ranges. The derived velocities exceed the speed of sound in the magnetic-field.free corona: on the average the velocity decreases with increasing height to a minimum of ,....., 750 kmjs at a little below I Ro' and j,hereafter slowly increases with height. The nature of the type II source is discussed in relation to these velocities, and also in relation to detailed measurements of harmonic ratios and band splitting for the five individual bursts. It is suggested that the type II source is either a strong parallel shock (direction of propagation of shock parallel to magnetic field) or a perpendicular shock. Magnetic field strengths of 2-20 G at 0�5 R 0 above the photosphere, decreasing to 1-10 G at 2 Ro, are derived. Finally, it is shown that theories by which fundamental emission arises in front of the shock, whilst harmonic emission originates in the interior of the shock, are untenable.

Type II Solar Radio Bursts over Solar Cycle 21

1994 ◽  
Vol 144 ◽  
pp. 283-284
Author(s):  
G. Maris ◽  
E. Tifrea
Keyword(s):  
Solar Radio ◽  
Interplanetary Space ◽  
Impulsive Phase ◽  
Radio Bursts ◽  
Type Ii ◽  
Solar Radio Bursts ◽  
Strong Energy ◽  
Mass Ejection ◽  
Geophysical Effect ◽  
Radio Event

The type II solar radio bursts produced by a shock wave passing through the solar corona are one of the most frequently studied solar activity phenomena. The scientific interest in this type of phenomenon is due to the fact that the presence of this radio event in a solar flare is an almost certain indicator of a future geophysical effect. The origin of the shock waves which produce these bursts is not at all simple; besides the shocks which are generated as a result of a strong energy release during the impulsive phase of a flare, there are also the shocks generated by a coronal mass ejection or the shocks which appear in the interplanetary space due to the supplementary acceleration of the solar particles.

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