The Frequency Splitting of Transient Solar Radio Bursts

1969 ◽  
Vol 1 (6) ◽  
pp. 273-274 ◽  
Author(s):  
G. R. A. Ellis
Keyword(s):  
Solar Radio ◽  
Narrow Band ◽  
Common Type ◽  
Radio Bursts ◽  
Frequency Range ◽  
Solar Radio Bursts ◽  
Radio Emissions ◽  
Frequency Splitting ◽  
Solar Radio Emissions

Observations of transient solar radio emissions lasting 0.2 to 2 s in the frequency range 25-50 MHz have demonstrated the existence of a characteristic and relatively common type of burst (the split pair) made up of two narrow band components separated in frequency by about 0.1 MHz.

scholarly journals Nonlinear analysis of decimetric solar bursts

2009 ◽  
Vol 5 (S264) ◽  
pp. 279-281
Author(s):  
Reinaldo R. Rosa ◽  
Mauricio J. A. Bolzan ◽  
Francisco C. R. Fernandes ◽  
H. S. Sawant ◽  
Marian Karlický
Keyword(s):  
Solar Radio ◽  
Inhomogeneous Plasma ◽  
Active Regions ◽  
Singularity Spectrum ◽  
Frequency Range ◽  
Radio Emissions ◽  
Magnetic Structures ◽  
Fine Structures ◽  
Solar Bursts ◽  
Solar Radio Emissions

AbstractThe solar radio emissions in the decimetric frequency range (above 1 GHz) are very rich in temporal and spectral fine structures due to nonlinear processes occurring in the magnetic structures on the corresponding active regions. In this paper we characterize the singularity spectrum, f(α), for solar bursts observed at 1.6, 2.0 and 3 GHz. We interpret our findings as evidence of inhomogeneous plasma turbulence driving the underlying plasma emission process and discuss the nonlinear multifractal approach into the context of geoeffective solar active regions.

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 Numerical Simulation of Type III Bursts

1980 ◽  
Vol 86 ◽  
pp. 299-302
Author(s):  
T. Takakura
Keyword(s):  
Numerical Simulation ◽  
Analytical Method ◽  
Solar Radio ◽  
Plasma Waves ◽  
Radio Bursts ◽  
Emission Mechanism ◽  
Normal Type ◽  
Solar Radio Bursts ◽  
Radio Emissions ◽  
Type Iii

By the use of semi-analytical method, modeling of three kinds of type III solar radio bursts have been made. Many basic problems about the type III bursts and associated solar electrons have been solved showing some striking or unexpected results. If the fundamental radio emissions should be really observed as the normal type III bursts, the emission mechanism would not be the currently accepted one, i.e. the scattering of plasma waves by ions.

The transverse motions of the sources of solar radio bursts

1959 ◽  
Vol 9 ◽  
pp. 176-185 ◽  
Author(s):  
J. P. Wild ◽  
K. V. Sheridan ◽  
G. H. Trent
Keyword(s):  
Automatic System ◽  
Solar Radio ◽  
Complex Data ◽  
Radio Bursts ◽  
Frequency Range ◽  
Solar Radio Bursts ◽  
Time Intervals ◽  
Initial Form ◽  
Phase Calibration ◽  
East West

Observations of the spectrum of solar radio bursts at meter wavelengths have indicated the desirability of measuring positions on the sun's disk not only as a function of time but also as a function of frequency. With this objective in view, we are now using a swept-frequency interferometer to determine the east-west disk coordinate of the transient solar sources at time intervals of ½ second and freqency intervals of about 5 Mc/s within the frequency range 40 to 70 Mc/s. The accuracy to which the centroid of the source is located is about ±1 minute of arc. In its initial form [1], the interferometer contained two aerials separated by a distance of 1 km. As a result of preliminary tests, two major additions have been made: (1) a second interferometer of much smaller spacing (¼ km) has been added to resolve the usual ambiguities associated with two-aerial interferometry, and (2) an automatic system of lobe-switching and phase-calibration has been incorporated to facilitate the reduction of the complex data recorded.

Possible reasons for the frequency splitting of the harmonics of type II solar radio bursts

2016 ◽  
Vol 60 (1) ◽  
pp. 163-173 ◽  
Author(s):  
V. G. Eselevich ◽  
M. V. Eselevich ◽  
I. V. Zimovets
Keyword(s):  
Solar Radio ◽  
Radio Bursts ◽  
Type Ii ◽  
Solar Radio Bursts ◽  
Frequency Splitting

scholarly journals The Positions and Movements of the Sources of Solar Radio Bursts of Spectral Type II

1963 ◽  
Vol 16 (2) ◽  
pp. 240 ◽  
Author(s):  
AA Weiss
Keyword(s):  
Spectral Type ◽  
Solar Radio ◽  
Radio Bursts ◽  
Type Ii ◽  
Frequency Range ◽  
Solar Radio Bursts ◽  
Dynamic Spectra ◽  
Type Ii Radio Bursts ◽  
Optical Flare ◽  
East West

The east-west position coordinates of the sources of 22 type II radio bursts, measured in the range 40-70 Mc/s using a swept-frequency interferometer, are analysed and discussed, in conjunction with dynamic spectra obtained in the frequency range 15-210 Mc/s. Many bursts are multiple and consist of a number of separate bursts excited by disturbances ejected in different directions from the vicinity of an optical flare, which may be equally complex.

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 Estimation of Shock Thickness from Dynamic Spectra of Type II Bursts

1980 ◽  
Vol 91 ◽  
pp. 257-259
Author(s):  
H. S. Sawant ◽  
S. S. Degaonkar ◽  
S. K. Alurkar ◽  
R. V. Bhonsle
Keyword(s):  
Solar Radio ◽  
Narrow Band ◽  
Radio Bursts ◽  
Type Ii ◽  
Solar Radio Bursts ◽  
Fast Electrons ◽  
Dynamic Spectra ◽  
Type Ii Bursts ◽  
Shock Thickness

Twenty type II solar radio bursts were observed during the period 1968 to 1972 by a solar radio spectroscope (240-40 MHz) at Ahmadebad. Intensity variations in type II bursts as a function of frequency and time are sometimes observed in their dynamic spectra. This fine structure enables determination of the shock thickness of the order of a few hundred to a few thousand kilometers. In a few cases, an interaction between streams of fast electrons and propagating shocks is clearly evidenced by simultaneous observations of short duration narrow band structures in type III bursts and type II bursts.

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