Abstract
We studied the properties of fine structures in 23 type II bursts recorded at the Trieste Astronomical Observatory at frequencies above 200 MHz.
The lifetime of a single fine structure is a fraction of a second. The ratio of fine structures intensity vs bulk flux density is different in different type II bursts and it changes during the evolution of a single event; the reported maximum ratio is 3. The polarization of fine structures is nearly the same during the lifetime of an event. There is also no essential difference in polarization between fine structures and bulk emission; this holds also for an example of high-polarization (about 80%) event.
At frequencies lower than 200 MHz the analogy between herringbone structure and type III bursts is frequently mentioned in the literature. From the observations we studied, it results, however, that the time profile of single fine-structure elements and their polarization are substantially different from the morphology of type III bursts.
The observed fine structures and their characteristics are discussed in the framework of the model by Holman and Pesses (1983).
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References
Abrami, A., Messerotti, M., Zlobec, P., and Karlický, M.: 1990,Solar Phys. 130, 131.
Aurass, H.: 1992,Ann. Geophys. 10, 359.
Bakunin, L. M., Ledenev, V. G., Kosugi, T., and McLean, D. J.: 1990,Solar Phys. 129, 379.
Benz, A. O. and Thejappa, G.: 1988,Astron. Astrophys. 202, 267.
Benz, A. O. and Zlobec, P.: 1978,Astron. Astrophys. 63, 137.
Blandford, R. D. and Ostriker, F. R.: 1978,Astrophys. J. 221, L29.
Cairns, I. H. and Robinson, R. D.: 1987,Solar Phys. 111, 365.
Cane, H. V. and White, S. M.: 1989,Solar Phys. 120, 137.
Fomichev, V. V. and Chertok, I. M.: 1968,Soviet Astron. 12, 21.
Holman, G. D. and Pesses, M. E.: 1983,Astrophys. J. 267, 837.
Krüger, A.: 1979,Introduction to Solar Radio Astronomy and Radio Physics, D. Reidel Publ. Co., Dordrecht, Holland.
Kundu, M. R.: 1965,Solar Radioastronomy, Interscience, New York.
McLean, D. J.: 1974, in G. Newkirk (ed.), ‘Coronal Disturbances’,IAU Symp. 57, 301.
Melrose, D. B.: 1990,Australian J. Phys. 43, 703.
Nakajima, H., Kawashima, S., Shinohara, N., Shiomi, Y., and Enome, S.: 1990,Astrophys. J. Suppl. Series 73, 177.
Nelson, G. J. and Melrose, D. B.: 1985, in D. J. McLean and N. R. Labrum (eds.),Solar Radiophysics, Cambridge University Press, Cambridge, p. 333.
Pesses, M. E.: 1981,J. Geophys. Res. 86, 150.
Riddle, A. C.: 1974,Solar Phys. 34, 181.
Roberts, J. A.: 1959,Australian J. Phys. 12, 327.
Slottje, C.: 1981,Atlas of Fine Structures of Dynamic Spectra of Solar Type IV-dm and Some Type II Radio Bursts, Publ. of the Netherlands Fundation for Radio Astronomy, Dwingeloo.
Stewart, R. T.: 1966,Australian J. Phys. 19, 209.
Stewart, R. T. and Magun, A.: 1980,Proc. Astron. Soc. Australia 4(1), 53.
Suzuki, S., Stewart, R. T., and Magun, A.: 1980, in M. R. Kundu and T. E. Gergely (eds.), ‘Radio Physics of the Sun’,Proc. IAU Symp. 86, 241.
Toptyghin, I. N.: 1980,Space Sci. Rev. 26, 157.
Urbarz, H. W.: 1990,Type II Solar Radio Bursts Recorded at Weissenau 1966–1987, Rep. UAG-98, Publ. World Data Center A, Boulder, Colorado.
Urbarz, H. W., Fomichev, V. V., and Chertok, I. M.: 1977,Soviet Astron. 21, 77.
Zlobec, P. and Thejappa, G.: 1987,Hvar Obs. Bull. 11, 111.
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Zlobec, P., Messerotti, M., Karlický, M. et al. Fine structures in time profiles of type II bursts at frequencies above 200 MHz. Sol Phys 144, 373–384 (1993). https://doi.org/10.1007/BF00627601
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DOI: https://doi.org/10.1007/BF00627601