The Solar Corona in Active Regions and the Thermal Origin of the Slowly Varying Component of Solar Radio Radiation.

1961 ◽  
Vol 133 ◽  
pp. 983 ◽  
Author(s):  
Gordon, Jr. Newkirk
Keyword(s):  
Solar Corona ◽  
Solar Radio ◽  
Active Regions ◽  
Radio Radiation ◽  
Thermal Origin ◽  
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 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.

Stepwise Emergence and Development of Microwave Emission of Active Regions – A Fundamental Property of Active Solar Corona

1994 ◽  
Vol 144 ◽  
pp. 509-512
Author(s):  
G. Ya. Smolkov ◽  
V. P. Nefedyev ◽  
A. M. Uralov ◽  
N. N. Kardapolova
Keyword(s):  
Solar Corona ◽  
Radio Telescope ◽  
Solar Radio ◽  
Fundamental Property ◽  
Active Regions ◽  
Space Mission ◽  
Microwave Emission ◽  
Ground Support ◽  
Siberian Solar Radio Telescope

AbstractThis paper has two goals: to report the informative merits of the Siberian solar radio telescope (SSRT) for ground-support of the SOHO or some other space mission, and provide a generalized presentation of one of the original results obtained at SSRT that indicates, we believe, a fundamental property of the emission from solar corona active regions (AR).

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 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 70. Some properties of solar radio-transients on fast 200 Mc./s. records

1957 ◽  
Vol 4 ◽  
pp. 366-370 ◽  
Author(s):  
C. De Jager ◽  
F. Van 'T Veer
Keyword(s):  
Response Time ◽  
High Speed ◽  
Solar Radio ◽  
Radio Radiation ◽  
Cornell University ◽  
Solar Radio Radiation ◽  
Radio Transients

Some 6 km. of high-speed (Brush) records of the solar radio radiation at 200 Mc./s. made at Cornell University by Ch. L. Seeger in 1949 and 1950 have been kindly put at our disposal. They were made with a paper speed of 0·5 cm./sec., sometimes with 2·5 cm./sec. The response time of the recording pen was 0s·02. Some records have been made simultaneously at 205 Mc./s. and at 200 Mc./s. This paper gives some results of a discussion of these records. The properties that were studied are: the clustering tendencies among the radio-pips, their band-widths, the echo-phenomena and the duration of the pips.

Sign in / Sign up

Export Citation Format

Share Document