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.

scholarly journals The correlation of solar radio bursts by magnetic activity and cosmic rays

1959 ◽  
Vol 9 ◽  
pp. 210-213
Author(s):  
A. R. Thompson
Keyword(s):  
Cosmic Rays ◽  
Radio Astronomy ◽  
Solar Radio ◽  
Magnetic Activity ◽  
Radio Bursts ◽  
Type Ii ◽  
Frequency Range ◽  
Sweep Frequency ◽  
Solar Radio Bursts ◽  
Auroral Particles

The sweep-frequency equipment at the Harvard Radio Astronomy Station, Fort Davis, Texas, has now been running continuously since 1956 September, recording solar radio activity in the frequency range from 100 to 580 Mc/s. The following contribution describes preliminary investigations of the correlation of the radio data with solar corpuscular emissions. This work was initiated to examine the well-known suggestions that the origins of the type II and type III radio bursts are associated with the ejection of auroral particles and cosmic rays respectively.

scholarly journals Solar Radio Bursts of Spectral Type V

1965 ◽  
Vol 18 (2) ◽  
pp. 143 ◽  
Author(s):  
The Late AA Weiss ◽  
RT Stewart
Keyword(s):  
Spectral Type ◽  
Solar Radio ◽  
Radio Bursts ◽  
Frequency Range ◽  
Solar Radio Bursts ◽  
Wave Type ◽  
Type V

The properties of the metre-wave type V burst have been-observed by interferometry in the frequency range 40-70 Mc/s, and by dynamic spectroscopy in the frequency range 5-210 Mc/s. Our investigations cover positions, movements, and angular sizes of the sources, and the spectrum and polarization of the emission.

A Preliminary Study of the Dynamic Spectra of Solar Radio Bursts in the Frequency Range 500-950 Mc/s.

1961 ◽  
Vol 133 ◽  
pp. 243 ◽  
Author(s):  
C. W. Young ◽  
C. L. Spencer ◽  
G. E. Moreton ◽  
J. A. Roberts
Keyword(s):  
Solar Radio ◽  
Radio Bursts ◽  
Frequency Range ◽  
Solar Radio Bursts ◽  
Dynamic Spectra ◽  
Preliminary Study

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 Interferometric imaging with LOFAR remote baselines of the fine structures of a solar type-IIIb radio burst

2020 ◽  
Vol 639 ◽  
pp. A115
Author(s):  
PeiJin Zhang ◽  
Pietro Zucca ◽  
Sarrvesh Seethapuram Sridhar ◽  
ChuanBing Wang ◽  
Mario M. Bisi ◽  
...  
Keyword(s):  
Radio Burst ◽  
Solar Radio ◽  
Source Size ◽  
Radio Bursts ◽  
Solar Radio Bursts ◽  
Harmonic Emission ◽  
Apparent Source ◽  
Solar Type ◽  
Fine Structures ◽  
Source Motion

Context. Solar radio bursts originate mainly from high energy electrons accelerated in solar eruptions like solar flares, jets, and coronal mass ejections. A sub-category of solar radio bursts with short time duration may be used as a proxy to understand wave generation and propagation within the corona. Aims. Complete case studies of the source size, position, and kinematics of short term bursts are very rare due to instrumental limitations. A comprehensive multi-frequency spectroscopic and imaging study was carried out of a clear example of a solar type IIIb-III pair. Methods. In this work, the source of the radio burst was imaged with the interferometric mode, using the remote baselines of the LOw Frequency ARray (LOFAR). A detailed analysis of the fine structures in the spectrum and of the radio source motion with imaging was conducted. Results. The study shows how the fundamental and harmonic components have a significantly different source motion. The apparent source of the fundamental emission at 26.56 MHz displaces away from the solar disk center at about four times the speed of light, while the apparent source of the harmonic emission at the same frequency shows a speed of < 0.02 c. The source size of the harmonic emission observed in this case is smaller than that in previous studies, indicating the importance of the use of remote baselines.

Fine Structure of Solar Radio Bursts Observed at Decametric and Hectometric Waves

Solar Physics ◽  
2007 ◽  
Vol 241 (1) ◽  
pp. 145-169 ◽  
Author(s):  
G. P. Chernov ◽  
M. L. Kaiser ◽  
J.-L. Bougeret ◽  
V. V. Fomichev ◽  
R. V. Gorgutsa
Keyword(s):  
Fine Structure ◽  
Solar Radio ◽  
Radio Bursts ◽  
Solar Radio Bursts
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