Relationship of Solar Radio Emission at λ=1.43m and Optical Processes in the Sun

During the period 1966 July 12 to August 5 observations were made of the Sun at three radio observatories. The instruments used were the east-west arm of the Mills cross at Molonglo (408 MHz) and the Christiansen cross at Fleurs (696 MHz and 1424 MHz). The aim of these observations was to study the discrete sources of the slowly varying component of solar radio emission, while activity was comparatively quiet. The three frequencies enabled the variation of source structure with height of solar atmosphere to be studied. It has been pointed out by Swarup et al., and Christiansen et al. that the determination of the frequency dependence of these discrete sources is important for defining the physical mechanisms causing the radio emission.

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67. Solar radio emission and the acceleration of magnetic-storm particles

Symposium - International Astronomical Union ◽

10.1017/s0074180900049421 ◽

1957 ◽

Vol 4 ◽

pp. 356-357 ◽

Cited By ~ 9

Author(s):

A. Schlüter

Keyword(s):

Gravitational Field ◽

Radio Emission ◽

Solar Corona ◽

Magnetic Storm ◽

Solar Radio ◽

Plasma Frequency ◽

Solar Radio Emission ◽

The Sun ◽

Lower Frequencies

The shift of the emitted frequencies towards lower frequencies during a solar outburst is usually interpreted as due to a progressive rarefaction of the emitting gas. If one assumes that the emitted frequency is identical with the plasma frequency and furthermore that the density of the emitting plasma is similar to the density of the solar corona at the location of the radiating material, then it follows that this material is subject to an acceleration throughout the solar corona which compensates or exceeds the effect of the gravitational field of the sun.

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69. Disturbed radio emission from the sun as a sum of small monochromatic peaks

Symposium - International Astronomical Union ◽

10.1017/s0074180900049445 ◽

1957 ◽

Vol 4 ◽

pp. 363-365 ◽

Cited By ~ 1

Author(s):

V. V. Vitkevitch

Keyword(s):

Radio Emission ◽

Solar Radio ◽

Solar Radio Emission ◽

The Sun ◽

General Increase ◽

Quiet Sun ◽

Small Areas ◽

Physical Institute ◽

Academy Of Sciences

Observations of the radio emission from the sun carried out during recent years at the Crimean Station of the Physical Institute of the U.S.S.R. Academy of Sciences showed that the occurrence of spots appreciably increases the intensity of the solar radio emission in the range of metre wave-lengths. This increase of intensity has two components. The first (S-component) changes comparatively slowly with time. The second (P-component) consists of individual brief bursts (of the order of a second and less) of small amplitudes (10–100 % of the intensity of the quiet sun). The P-component is manifested most clearly in the emission connected with spots of small areas, when the general increase of the intensity is insignificant. Such a situation has been utilized for the study of the spectrum of individual small peaks.

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Measuring the polarization of solar radio emission due to the total magnetic field of the sun

Radiophysics and Quantum Electronics ◽

10.1007/bf01038621 ◽

1966 ◽

Vol 8 (2) ◽

pp. 286-287

Author(s):

I. F. Belov

Keyword(s):

Magnetic Field ◽

Radio Emission ◽

Solar Radio ◽

Solar Radio Emission ◽

The Sun ◽

Total Magnetic Field

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71. A peculiar type of scintillation of solar radio radiation

Symposium - International Astronomical Union ◽

10.1017/s0074180900049469 ◽

1957 ◽

Vol 4 ◽

pp. 371-372

Author(s):

A. D. Fokker

Keyword(s):

The Netherlands ◽

Radio Emission ◽

Radio Astronomy ◽

Solar Radio ◽

Solar Radio Emission ◽

The Sun ◽

Radio Radiation ◽

Selective Fading ◽

Continuous Survey ◽

Solar Radio Radiation

Some authors (Payne-Scott and Little (1952) [1]; Owren (1952) [2]) have mentioned a phenomenon in the enhanced solar radio emission which they call ‘non-selective fading’. The present paper is meant to call attention to another, rather peculiar, type of scintillation in the radio emission of the sun, which differs from the non-selective fading in some important respects. This scintillation has been observed since 1952 by the division ‘Ionosphere and Radio Astronomy’ of the Netherlands Telecommunications Service in the course of a continuous survey of solar radio radiation. It has been found at the radio frequencies 140, 200 and 545 Mc./s.

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