Slowly varying component of extreme ultraviolet solar radiation and its relation to solar radio radiation

1974 ◽  
Vol 79 (28) ◽  
pp. 4138-4148 ◽  
Author(s):  
Robert D. Chapman ◽  
Werner M. Neupert
Keyword(s):  
Solar Radiation ◽  
Solar Radio ◽  
Extreme Ultraviolet ◽  
Radio Radiation ◽  
Solar Radio Radiation ◽  
Ultraviolet Solar Radiation

scholarly journals Solar Radio Radiation Bursts on 1998 April 15

2000 ◽  
Vol 52 (5) ◽  
pp. 919-924 ◽  
Author(s):  
Zongjun Ning ◽  
Qijun Fu ◽  
Quankang Lu
Keyword(s):  
Solar Radio ◽  
Radio Radiation ◽  
Solar Radio Radiation

scholarly journals Mode Coupling in the Solar Corona. I. Coupling Near the Plasma Level

1974 ◽  
Vol 27 (1) ◽  
pp. 31 ◽  
Author(s):  
DB Melrose
Keyword(s):  
Plasma Level ◽  
Solar Corona ◽  
Mode Coupling ◽  
Solar Radio ◽  
Plasma Frequency ◽  
Type I ◽  
Radio Radiation ◽  
Coupling Ratio ◽  
Solar Radio Radiation ◽  
Solar Type

The theory of mode coupling in the radiation from solar type I storms is extended to treat coupling when the frequency! is near the plasma frequency!p. It is found that Cohen's coupling ratio Q = U/It)4, where It is the transition frequency (f'P It for strong coupling), is to be multiplied by a factor (1-!~/ J2)5/2 for QT regions, i.e. coupling is relatively suppressed close to the plasma level. The implications on the handedness of solar radio radiation are discussed. The possibility of depolarization due to mode coupling is considered briefly.

scholarly journals Solar radio bright spots at 88-cm wavelength

1959 ◽  
Vol 9 ◽  
pp. 136-139 ◽  
Author(s):  
J. Firor
Keyword(s):  
Solar Radio ◽  
Wavelength Region ◽  
Bright Spot ◽  
Radio Radiation ◽  
Noise Storm ◽  
Bright Spots ◽  
Solar Radio Radiation

During 1957 we studied the solar radio radiation at a wavelength intermediate between the centimeter region with its slowly varying bright spots and the meter-wavelength region with its noise storms. At this intermediate wavelength (88 cm) the slowly varying bright-spot and the noise-storm producing regions merge into two aspects of the same persistent, bright, solar radio regions.

scholarly journals The Quiet Sun at cm- and mm-Wavelengths

1980 ◽  
Vol 86 ◽  
pp. 25-39 ◽  
Author(s):  
E. Fürst
Keyword(s):  
Solar Atmosphere ◽  
Solar Radio ◽  
Theoretical Estimate ◽  
Sunspot Cycle ◽  
Active Regions ◽  
Spectral Lines ◽  
Radio Radiation ◽  
Quiet Sun ◽  
Solar Radio Radiation ◽  
Active Centres

Soon after the first detection of radio emission from the sun two components of the solar radio radiation were identified: The emission related to active centres on the disk and the radiation of the undisturbed, static solar atmosphere, in which the active regions are embedded. The undisturbed component is observed to vary only slightly during the solar sunspot cycle, it is called the emission of the quiet sun. A theoretical estimate of this component was first given by Martyn (1946) and subsequently developed in more detail by many other authors. The basic observations were performed with poor angular resolution. Still at present most experimental data are taken with angular resolutions of about 1 to 4 arc min, too low to discriminate between the different solar atmospheric fine structures, clearly seen in various spectral lines. The quiet component of the solar radio radiation therefore represents the average emission of an inhomogenous solar atmosphere.

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