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• W2529307120 abstract "All radiation processes described can take place inthe solar corona, depending on different physical characters ofthe radiating electrons and the coronal plasma, such aselectron energy, electron pitch angle and the magnitude of the ratio f-2p/f-2H of the medium in the region where the radiatorsreside. On the other hand, the observed spectral features ofa solar radio emission are determined by both the mechanismresponsible for the emission and the propagation conditions ofelectromagnetic waves in the solar corona. Thus, the observeddynamic spectra of the solar radio emissions reveal essentiallythe physical conditions of the solar corona during the emission periods.The emissions of narrow bandwidth type III bursts anddrift pair bursts have been proposed as the consequence of plasmaradiation caused by electron streams in the isotropic corona,which is understood to refer to electromagnetic radiationextracted from Cerenkov plasma waves through scattering or wave-modecoupling (Ginzburg and Zheleznyakov, 1958; Roberts, 1958;Wild et al., 1963; Zheleznyakov, 1965). However, manyobserved spectral characteristics of the type III bursts and itsrelated U bursts, the drift pairs and the newly discovered hookbursts clearly indicate that it is necessary that the sunspotmagnetic field be taken into account in the theories. So farthe conditions of plasma radiation by electron streams in amagnetoactive plasma have not been investigated in detailand consequently, many characteristics of these emission eventsremain unexplained. In this thesis, we begin by formulatingthe theory of plasma radiation in a magnetoactive plasma(Chapter II and Chapter V). The theory is then applied to theinterpretation of the polarized type III burst and U burstemission event and the drift pair and hook burst emission eventin Chapter VI and Chapter VII respectively.The origins of various components of the complicated typeIV emission have been interpreted as the results of synchrotronradiation by relativistic electrons trapped in the sunspotmagnetic field configurations (Boischot and Denisse, 1957; Takakura and Kaip 1961; Kai, 1964; etc.). However, withouttaking into account the effects of the medium on the radiationprocess, previous theories encounter various difficulties andfail to account for the outstanding polarization characters ofthe type IV emission. In order to set up a satisfactorytheory of type IVA emission, we study, for the x-mode and theo-mode, the power spectra from single electrons, the process ofamplification of cyclotron radiation in a stream-plasma systemand the escape conditions in detail in Chapter III and ChapterVIII. Cyclotron radiation of electromagnetic waves in thex-mode and the o-mode and the Cerenkov excitation of plasmawaves by helical electron streams moving at the base of thesolar corona is proposed as the origin of the type IVAemission. It is found that most of the important characteristicsof the emission can be well accounted for by the theory.In Chapter IX, coherent synchrotron radiation from asystem of relativistic electrons is studied taking into accountthe effects of the ambient plasma. The origins of some broadband solar continuum emissions are also discussed.In the final chapter, a conclusion of the thesis is givenand further researches are suggested." @default.
• W2529307120 created "2016-10-14" @default.
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• W2529307120 title "Solar radio emissions." @default.
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