Radio Bursts from the Solar Corona

Wild, J. P.; Smerd, S. F.

doi:10.1146/annurev.aa.10.090172.001111

Cited by 272 publications

(91 citation statements)

References 3 publications

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“…These two aspects of band-splitting indicate that LFB and HFB are emitted from the upstream and downstream region of the shock, as ad hoc presumed by various authors (see, e.g., Wild & Smerd 1972;Smerd et al 1974Smerd et al , 1975Mann et al 1995;Vršnak et al 2001; and references therein). Pre-examining a larger set of long wavelength IP t-II bursts we found in a number of non-band-split bursts that the emission lane points to the base of the associated jump in the local plasma frequency (indicative of the upstream emission) and sometimes (see Fig.…”

Section: Discussionmentioning

confidence: 72%

Band-splitting of coronal and interplanetary type II bursts

Vršnak¹,

Auraß²,

Magdalenić³

et al. 2001

A&A

141

113

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Abstract. Patterns analogous to the band-splitting of metric type II bursts are found in a number of type II bursts observed in the dekameter-kilometer wavelength range. A similarity of morphological and frequency-time characteristics of two emission components are indicative of a common source. Relative frequency splits span in the range ∆f/f = 0.05−0.6. At radial distances between 2 and 4 R only small splits around 0.1 can be found. In the interplanetary space the relative split on average increases with the radial distance, whereas the inferred shock velocity decreases. In three events extrapolations of the split components point to the base and the peak of the jump in the local plasma frequency caused by the associated shock passage at 1 AU. This is suggestive of the plasma radiation from the regions upstream and downstream of the shock. Adopting this interpretation, one finds that the drop of ∆f/f at 2-4 R is congruent with the Alfvén velocity maximum expected there. The split increase and the velocity decrease at larger distances can be explained as a consequence of declining Alfvén speed in the interplanetary space.

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Section: Discussionmentioning

confidence: 72%

Band-splitting of coronal and interplanetary type II bursts

Vršnak¹,

Auraß²,

Magdalenić³

et al. 2001

A&A

141

113

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“…There is no evidence against shorter period (for example, ~ 1 s) waves being important, and there is radio evidence for their presence (see e.g. the review by Wild and Smerd 1972). Frisch's (1964) coupling ratio for waves with a period of around a second (implying A of order several hundred kilometres) would require a very inhomogeneous corona for the coupling to be effective.…”

Section: Discussionmentioning

confidence: 99%

Mode Coupling in the Solar Corona. III. Alfvén and Magnetoacoustic Waves

Melrose¹

1977

Aust. J. Phys.

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Coupling between Alfven waves and fast mode waves obliquely incident on a stratified medium is treated using the method of Clemmow and Heading (1954) within the framework of the cold plasma approximation. A result due to Frisch (1964) is rederived in the special case of vertical incidence. The coupling is strongest for nearly parallel (to the magnetic field lines) propagation, and the coupling ratio may be approximated by Q = (00 /0)" where 0 is the angle between the wave vector and the magnetic field lines, while og = A/L, with A the wavelength and L the scalelength of the inhomogeneity. This result may be of significance in connection with the heating of the solar corona by the dissipation of waves generated initially as acoustic waves in the photosphere, and perhaps with the propagation of hydromagnetic waves in the interplanetary medium.

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“…Of the five different types of solar radio bursts that have been identified to date, type-III radio bursts are perhaps the best studied and understood. For historical and recent reviews, see, e.g., Ginzburg & Zheleznyakov (1958), Wild et al (1963), Kundu (1965), Tsytovich (1967), Zheleznyakov (1970), Wild & Smerd (1972), Stewart (1974), Fainberg & Stone (1974), Lin (1974), Smerd (1976), Rosenberg (1976), Melrose (1980aMelrose ( , 1980bMelrose ( , 1986, Goldman (1983), Suzuki & Dulk (1985), Dulk (1985), Reiner et al (1992Reiner et al ( , 2009, Robinson & Cairns (1998a, 1998b, 1998c, Cane et al (2002), Reid & Ratcliffe (2014), Ziebell et al (2014Ziebell et al ( , 2015.…”

Section: Introductionmentioning

confidence: 99%

Plasma Emission by Counter-Streaming Electron Beams

Ziebell¹,

Petruzzellis²,

Yoon³

et al. 2016

ApJ

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The radiation emission mechanism responsible for both type-II and type-III solar radio bursts is commonly accepted as plasma emission. Recently Ganse et al. suggested that type-II radio bursts may be enhanced when the electron foreshock geometry of a coronal mass ejection contains a double hump structure. They reasoned that the counter-streaming electron beams that exist between the double shocks may enhance the nonlinear coalescence interaction, thereby giving rise to more efficient generation of radiation. Ganse et al. employed a particle-in-cell simulation to study such a scenario. The present paper revisits the same problem with EM weak turbulence theory, and show that the fundamental (F) emission is not greatly affected by the presence of counter-streaming beams, but the harmonic (H) emission becomes somewhat more effective when the two beams are present. The present finding is thus complementary to the work by Ganse et al.

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Radio Bursts from the Solar Corona

Cited by 272 publications

References 3 publications

Band-splitting of coronal and interplanetary type II bursts

Band-splitting of coronal and interplanetary type II bursts

Mode Coupling in the Solar Corona. III. Alfvén and Magnetoacoustic Waves

Plasma Emission by Counter-Streaming Electron Beams

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