Interferometer observation of pulsating sources associated with a type IV solar radio burst

Solar Physics ◽  
1973 ◽  
Vol 29 (2) ◽  
pp. 461-475 ◽  
Author(s):  
Keizo Kai ◽  
Akio Takayanagi
Keyword(s):  
Radio Burst ◽  
Solar Radio ◽  
Solar Radio Burst ◽  
Type Iv ◽  
Interferometer Observation

scholarly journals The Type IV Solar Radio Burst at Metre Wavelengths

1963 ◽  
Vol 16 (4) ◽  
pp. 526 ◽  
Author(s):  
AA Weiss
Keyword(s):  
Radio Burst ◽  
Solar Radio ◽  
Solar Radio Burst ◽  
Frequency Range ◽  
Type Iv

Properties of 24 sources of type IV emission at metre wavelengths (including the long-lived continuum storms) have been observed by interferometry in the frequency range 40-70 Mc/s and by dynamic spectroscopy in the frequency range 15-210 Mc/s. The characteristics investigated are the positions, movements, and angular sizes of the sources, and the spectrum and polarization of the emission.

scholarly journals AN ERUPTIVE HOT-CHANNEL STRUCTURE OBSERVED AT METRIC WAVELENGTH AS A MOVING TYPE-IV SOLAR RADIO BURST

2016 ◽  
Vol 830 (1) ◽  
pp. L2 ◽  
Author(s):  
V. Vasanth ◽  
Yao Chen ◽  
Shiwei Feng ◽  
Suli Ma ◽  
Guohui Du ◽  
...  
Keyword(s):  
Radio Burst ◽  
Solar Radio ◽  
Channel Structure ◽  
Solar Radio Burst ◽  
Type Iv

scholarly journals Evidence for the Transfer of Corpuscles to Distant Parts of the Sun Following a Solar Radio Burst

1961 ◽  
Vol 14 (4) ◽  
pp. 540 ◽  
Author(s):  
RF Mullaly
Keyword(s):  
Radio Burst ◽  
Solar Radio ◽  
Brightness Distribution ◽  
Solar Radio Burst ◽  
The Sun ◽  
Time Intervals ◽  
The Past ◽  
Grating Interferometer ◽  
Half Power ◽  
East West

The brightness distribution of 21-cm radiation over the Sun's surface has been studied for the past four years with the Christiansen crossed-grating interferometer (Christiansen et al. 1961) at Fleurs near Sydney. The observations described here were made using one arm of this cross as a simple grating interferometer, providing a transit instrument with a fan beam of about 2' of arc resolution to half-power points in the east-west direction and very low resolution north-south. The Sun was scanned repeatedly from east to west at time intervals of approximately 4 min.

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