An expeditionary solar radiotelescope

Belov, I. F.; Lebedev, E. I.; Pivovarov, V. F.; Timofeev, B. V.; Fridman, V. M.; Khrulev, V. P.

doi:10.1007/bf01037402

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“…The observations on March 1970 were carried out using a radio telescope with a 2-m paraboloid antenna. The flux (F), polarization (FR-L), and the slope of the spectrum (zlF) of the solar radio emission were measured at A = 3 cm (Belov et al, 1974). Analysing the averaged per 5 min records taken on March 5 and 6, 1970 ( Figure 5a Observations, including the moment of the onset of the proton flare on Sepgember 1, 1971 were made using a 2-m radio telescope .…”

Section: Flares On August 2 4 and 7 1972 In The Active Region Mcmatmentioning

confidence: 99%

Manifestation of pulsation instability in solar radio emission preceding proton flares

et al. 1978

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The investigation of solar radio emission fluctuations at the wavelength ~t = 3 cm led to the discovery of a visible increase in pulsations with periods of about 30-120 min prior to proton flares. These pulsations were observed before all (seven) proton flares included in our cycle of observations from 1969 to 1974. The phenomenon was not found to occur before non-proton flares. The assumption is made that the observed pulsations are a manifestation of pre-flare instability in coronal structures. Estimations have been made for fluctuations of the gyro-resonance radiation from the regions above spots associated with the magnetic field variations when a groove instability of a coronal condensation is developed. They are in good agreement with the observational data. The discovered manifestation of the pre-flare instability in fluctuations of the solar radio emission open new ways to study the flare development and to predict geo-effective phenomena on the Sun.

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Section: Flares On August 2 4 and 7 1972 In The Active Region Mcmatmentioning

confidence: 99%