Homology of solar radio events

Symposium - International Astronomical Union ◽

10.1017/s0074180900022002 ◽

1968 ◽

Vol 35 ◽

pp. 551-555

Author(s):

A. D. Fokker

Keyword(s):

Solar Radio ◽

Microwave Bursts

Successive flares within the same centre of activity sometimes produce radio events that are remarkably similar. The occurrence of such homologous radio events is commonly restricted to periods of less than 48 hours.Typical for certain centres of activity is their tendency to give rise to impulsive microwave bursts. Such bursts may occur repeatedly during a period of more than a week. The distributions of the lengths of periods during which series of homologous bursts and of impulsive microwave bursts occur are compared.

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An Attempt to Classify Solar Microwave-Bursts by Source Localization Characteristics and Dynamics of Flare-Energy Release

Symposium - International Astronomical Union ◽

10.1017/s0074180900114767 ◽

1998 ◽

Vol 188 ◽

pp. 205-206

Author(s):

A. Krüger ◽

B. Kliem ◽

J. Hildebrandt ◽

V.P. Nefedev ◽

B.V. Agalakov ◽

...

Keyword(s):

Source Localization ◽

Solar Radio ◽

Spectral Characteristics ◽

Solar Radio Bursts ◽

Spatially Resolved ◽

Siberian Solar Radio Telescope ◽

Solar Microwave ◽

Magnetic Origin ◽

Flare Process ◽

Microwave Bursts

An overview of spatially resolved observations of solar radio bursts obtained by the Siberian Solar Radio Telescope at 5.8 GHz during the last ten years reveals the occurrence of different classes of burst emission defined by their source localization characteristics. Four major classes of bursts according to the source position relative to sunspots, the source size and structure, and the source height, could be tentatively distinguished and compared with burst spectral characteristics as well as with soft X-ray emission oberved by YOHKOH. These findings are in favour of a magnetic origin of the underlying flare process.

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Type II Solar Radio Bursts over Solar Cycle 21

International Astronomical Union Colloquium ◽

10.1017/s025292110002546x ◽

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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The Heights of Solar Radio Sources at 1424 MHz and 696 MHz

Publications of the Astronomical Society of Australia ◽

10.1017/s1323358000011401 ◽

1969 ◽

Vol 1 (5) ◽

pp. 192-194 ◽

Cited By ~ 4

Author(s):

D. G. Cole ◽

R. F. Mullaly

Keyword(s):

Solar Activity ◽

High Resolution ◽

Solar Disk ◽

Previous Investigation ◽

Solar Radio ◽

Radio Sources ◽

Grating Interferometer ◽

Maximum Solar Activity

The heights of solar radio sources at 1424 MHz and 696 MHz have been measured during the years 1965 and 1966. Solar activity at this time was near minimum. The number of radio sources appearing on the solar disk rarely exceeded three at any time and it thus was possible to resolve the majority of these with a high resolution grating interferometer. Many of the previous height measurements at these frequencies have been made near times of maximum solar activity and the confusion of sources within the beam has limited their accuracy. The number of sources studied here is quite considerably higher than in any previous investigation at these frequencies, and the period of observation has been continuous.

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