Abstract
From solar maps at 8.6 mm wavelength and total flux measurements at wavelengths of 1.7 cm to 122 cm, various spectra of the slowly varying component have been studied. The main distinction between these various types of spectra is the slope of the spectra toward wavelengths of less than 2 cm.
It has been shown that the probability of flare occurrence is correlated with the type of the source spectra. It is proposed that enhanced flare production occurs from a source of SVC whose spectrum has a peak around 6–10 cm wavelength but whose slope is flatter around λ ≃ 8 mm, but steeper toward longer centimeter wavelengths, than in the case of ‘normal’ SVC-spectra attributed to gyro resonance radiation. The implications of such spectra in terms of changes in magnetic field structure before the occurrence of a flare are discussed.
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References
Christiansen, W. N. and Mathewson, D. S.: 1959, in R. N. Bracewell (ed.), Paris Symposium on Radioastronomy, Stanford University Press, Stanford, p. 108.
Efanov, V. A., Kislyakov, A. G., and Moiseev, I. G.: 1972, Solar Phys. 24, 142.
Enger, I. and Reilly, E. R.: 1967, ‘The Influence of Radio Brightness Temperature on Solar Flare Prediction’, AFCRL-Report-67-0670.
Hobbs, R. W., Jordan, S. D., and Webster, W. J.: 1973, Nature 243, 48.
Kakinuma, T. and Swarup, G.: 1962, Astrophys. J. 136, 975.
Kundu, M. R.: 1965, Solar Radio Astronomy, Interscience Publishers, New York, London, Sydney, pp. 169, 178, and 186.
Kundu, M. R.: 1959, in R. N. Bracewell (ed.), Paris Symposium on Radio Astronomy, Stanford University Press, Stanford, p. 222.
Kundu, M. R., Becker, R. H., and Velusamy, T.: 1974, Solar Phys. 34, 185.
Kuseski, R. A. and Swanson, P. N.: 1976, Solar Phys. 48, 41.
Shimabukuro, F. I., Chapman, G. A., Mayfield, E. B., and Edelson, S.: 1973, Solar Phys. 30, 163.
Smerd, S. F.: 1964, in H. Odishaw (ed.), Research in Geophysics, M.I.T. Press, Cambridge, Mass., Vol. 1, p. 77.
Solar-Geophysical Data: 1972–1975, Boulder, Colo.
Swarup, G., Kakinuma, T., Covington, A. E., Harvey, G. A., Mullaly, R. F., and Rome, J.: 1963, Astrophys. J. 137, 1251.
Tanaka, H. and Kakinuma, T.: 1958, Rep. Ionosph. Res. Japan 12, 3.
Tanaka, H., Castelli, J. P., Covington, A. E., Krüger, A., Landecker, T. L., and Tlamicha, A.: 1973, Solar Phys. 29, 243.
Tlamicha, A.: 1968, Solar Phys. 5, 377.
Tsuchiya, A. and Takahashi, K.: 1968, Solar Phys. 3, 346.
Waldmeier, M.: 1940, Astrophys. 20, 195.
Zheleznyakov, V. V.: 1962, Soviet Astron.-AJ 6.1, 3.
Zheleznyakov, V. V.: 1964, Radio Emission of the Sun and Planets, Pergamon Press, p. 111.
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Steffen, P. On the type of spectra of S-component sources and their correlation with flare occurrence. Sol Phys 67, 89–100 (1980). https://doi.org/10.1007/BF00146685
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DOI: https://doi.org/10.1007/BF00146685