Currently available models of one of the most intriguing types of unsteady rf solar emission, millisecond solar radio spikes, are discussed. A comparative analysis of the models’ implications and of the body of existing data yields an outline of the most realistic radio spike model possible. The spikes are produced by the cyclotron maser mechanism. The cyclotron cone instability is caused by fast electrons distributed over energies according to a (piecewise) power law. The angular part of the distribution function (whose exact form is, as yet, undetermined) suffers fluctuations due to the magnetic field inhomogeneities that arise in the burst loop as a consequence of the original energy release. In some portions of the loop the distribution is not anisotropic enough to secure the development of a cyclotron instability; it is in these ’microtraps’ where individual spikes form. Key areas of future theoretical and experimental research are suggested with a view to verifying the adequacy and realizing the diagnostic potential of the model.

PACS: 96.60.−j DOI: 10.1070/PU1998v041n12ABEH000510 URL: https://ufn.ru/en/articles/1998/12/a/ 000078107700001 Citation: Fleishman G D, Mel’nikov V F "Millisecond solar radio spikes" Phys. Usp. 41 1157–1189 (1998) BibTexBibNote ® (generic)BibNote ® (RIS)Medline RefWorks RT Journal T1 Millisecond solar radio spikes A1 Fleishman,G.D. A1 Mel’nikov,V.F. PB Physics-Uspekhi PY 1998 FD 10 Dec, 1998 JF Physics-Uspekhi JO Phys. Usp. VO 41 IS 12 SP 1157-1189 DO 10.1070/PU1998v041n12ABEH000510 LK https://ufn.ru/en/articles/1998/12/a/ Оригинал: Флейшман Г Д, Мельников В Ф «Солнечные миллисекундные радиоспайки» УФН 168 1265–1301 (1998); DOI: 10.3367/UFNr.0168.199812a.1265