Solar radio bursts of spectral type II, coronal shocks, and optical coronal transients

Solar Physics ◽  
1981 ◽  
Vol 73 (2) ◽  
pp. 313-329 ◽  
Author(s):  
Alan Maxwell ◽  
Murray Dryer
Keyword(s):  
Spectral Type ◽  
Solar Radio ◽  
Radio Bursts ◽  
Type Ii ◽  
Solar Radio Bursts

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 Solar Radio Bursts of Spectral Type II

1959 ◽  
Vol 12 (4) ◽  
pp. 327 ◽  
Author(s):  
JA Roberts
Keyword(s):  
Spectral Type ◽  
Solar Radio ◽  
Bone Structure ◽  
Second Harmonic ◽  
Radio Bursts ◽  
Type Ii ◽  
Harmonic Structure ◽  
Solar Radio Bursts ◽  
Band Splitting ◽  
Compound Type

The characteristics of bursts of spectral type II are studied in a sample of 65 bursts. Approximately half the bursts show harmonic structure and about half are compound type III-type II events. Band splitting, the doubling of both the fundamental and second harmonic bands, is also relatively common. A rather less common feature is the appearance of herring-bone structure in which the slowly drifting band of the type II burst appears to be a source from which rapidly drifting elements diverge towards lower and higher frequencies.

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.

Higher Harmonic Plasma Radiation in Type II Solar Radio Bursts

1990 ◽  
pp. 517-518
Author(s):  
V. V. Fomichev ◽  
I. M. Chertok ◽  
R. V. Gorgutsa ◽  
A. K. Markeev ◽  
B. Kliem ◽  
...  
Keyword(s):  
Solar Radio ◽  
Plasma Radiation ◽  
Radio Bursts ◽  
Type Ii ◽  
Solar Radio Bursts ◽  
Higher Harmonic

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 Recent Results of Meter-decameter Wave Observations of Solar Flares

1989 ◽  
Vol 104 (2) ◽  
pp. 185-189
Author(s):  
N. Copalswamy ◽  
M. R. Kundu
Keyword(s):  
Solar Flares ◽  
Solar Radio ◽  
Radio Bursts ◽  
Type Ii ◽  
Solar Radio Bursts ◽  
Type Iii ◽  
Type Iv

AbstractWe present recent results from meter-decameter imaging of several classes of solar radio bursts: Preflare activity in the form of type III bursts, correlated type IIIs from distant sources, and type II and moving type IV bursts associated with flares and CMEs.

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.

scholarly journals Type II solar radio bursts: 2. Detailed comparison of theory with observations

2012 ◽  
Vol 117 (A6) ◽  
pp. n/a-n/a ◽  
Author(s):  
D. S. Hillan ◽  
Iver H. Cairns ◽  
P. A. Robinson
Keyword(s):  
Solar Radio ◽  
Detailed Comparison ◽  
Radio Bursts ◽  
Type Ii ◽  
Solar Radio Bursts

The Positions of Associated Type II and Type III Solar Radio Bursts

1974 ◽  
Vol 2 (5) ◽  
pp. 255-258 ◽  
Author(s):  
R. A. Duncan
Keyword(s):  
Solar Radio ◽  
Radio Bursts ◽  
Type Ii ◽  
Solar Radio Bursts ◽  
Type Iii ◽  
Intense Burst ◽  
Lower Frequencies

Large solar radio outbursts at metre wavelengths often consist of a group of type III bursts followed a few minutes later by a type II burst; in both spectral types the intense burst radiation drifts towards lower frequencies with time (Figure 1).

Sign in / Sign up

Export Citation Format

Share Document