Introduction

c with a narrow dispersion (for the speed ~ 0.2 c the increment sharply decreases and the maxima are washed out in the continuum for several cyclotron harmonics s). Thus these calculations show the inefficiency of the DPR mechanism. It is also important to note that the zebra stripes in this case still reveal the superfine structure of millisecond duration.

The August 1, 2010 event is an obvious case to understand all the difficulties in explaining the complex structure of the zebra pattern. Figure 1 gives dynamic spectrum in the decimeter range of Yunan observatory during the first maximum of this phenomenon. The event was discussed in connection with two complex CMEs. Separate spectra of Ondřejov observatory were used by Marian Karlicky and co-authors in several works under the DPR model, but no one tried to adequately explain the diversity of ZS in this case (see Figure 1).

Figure 1. Zebra- structure in the pulsating regime in the event on August 1, 2010 in the decimeter range 1000 – 1500 MHz observed by the spectropolarimeter of Yunan observatory (YNAO,   Kunming, China). The radio emission is weakly polarized. (Courtesy Guannan Gao).

Figure 2. An enlarged fragment of the spectrum shown in Figure 1, of 8 s duration, compared with the spectrum of Ondřejov observatory. All the components of the stripes coincide in two observatories, divided into 8000 km that confirms the solar origin of ZS (the time scale of obs. Ynao is late on 1.6 s). The time resolution of the spectrum of Ondřejov is an order of magnitude higher, and we see therein the superfine structure of the stripes of millisecond duration (Ondřejov spectrum is courtesy Marian Karlicky).

Figure 3. Zebra- structure, limited by fiber bursts from HF edge in the microwave range 2600– 3800 MHz of Huairou observatory, Beijing.

Brief discussion and conclusion

So, any model should explain:

• Radio fibers are sometimes imposed on ZS, or limit the stripes at the LF edge in the decimeter range (or from the HF edge in microwave);
• ZS appear in the pulsing mode as chaotic instantaneous columns (almost without their drift) with random duration from 0.1 s to 6 s;
• A wavelike or saw-tooth frequency drift of stripes of ZS in columns;
• The frequency separation grows with the frequency (as usual);
• Superfine structure of stripes of ZS and continuum.

In other events we have observed many examples of frequency splitting of ZS and, perhaps this was the main property, there was a synchronous change in the frequency drift of ZS stripes with space drift of their radio source.

In the DPR model all the changes of ZS stripes are usually associated with changes of the magnetic field and with propagating fast magneto-acoustic waves. In a very complicated case the simultaneous presence of fast particles in a radio source with several different distribution functions was proposed (Zheleznyakov et al. 2016).

At the same time, in the whistler model all the aforementioned properties of ZS stripes mentioned above were explained by real physical processes occurring during the coalescence of Langmuir waves with whistler waves (Chernov, 2006).

First of all, a radio source of ZS is usually located in magnetic islands after CME ejections. Therefore the close connection of ZS with fiber bursts is simply explained by the acceleration of fast particles in magnetic reconnection regions in the lower part (as in Figure 3) and in the upper part (as in Figure 1) of magnetic islands.

A wavelike or saw-tooth frequency drift of stripes was explained by the switching of whistler instability from the normal Doppler cyclotron resonance into the anomalous one (see Figure 2b in Chernov, 1990). Such switching should lead to a synchronous change of the frequency drift of stripes and spatial drift of the radio source, since whistlers generated at normal and anomalous resonance move in opposite directions. New injections of fast particles cause sharp change in frequency drift of stripes in instantaneous ZS columns. Low frequency absorptions (black stripes of ZS) are explained by weakening of the plasma wave instability due to the diffusion of fast particles by whistlers.

The superfine structure is generated by a pulsating regime of whistler instability with ion-sound waves (Chernov et al. 2003). Rope-like chains of fiber bursts are explained by a periodic whistler instability between two fast shock fronts in a magnetic reconnection region (Chernov, 2006). In the whistler model zebra-stripes can be converted into fiber bursts and back as it is shown in Figure 1.

For a comprehensive discussion of comparative analysis of observations of ZS and fiber bursts and different theoretical models we refer the reader to the reviews of Chernov (2012; 2016) (freely available at http://www.izmiran.ru/~gchernov/).

Acknowledgements

The authors are grateful to the Chinese colleagues in the National Astronomical Observatories of China Chenming Tan and Guannan Gao. The work was supported by the Russian Foundation for Basic Research (Grant N 17-02-00308).

Oral report at the conference: XII Solar System Plasma Conference, February 6–10, 2017, Space Research Institute of RAS.

The full paper was submitted to Astronomy Letter Journal:
G. P. Chernov, V. V. Fomichev, & R. A. Sych (2017). Comparison of alternative zebra-structure models in solar radio emission submitted to Astronomy Letter Journal arXiv: 1704.02528v1

*Full list of authors: Chernov G.P.¹, Fomichev V.V.¹, Sych R.A.² 

¹Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation, Russian Academy of Sciences (IZMIRAN), Troitsk, Moscow 108840, Russia e-mail:[email protected]

²Institute of Solar-Terrestrial Physics of Siberian Branch of Russian Academy of Sciences, 126a Lermontov Street, 664033 Irkutsk, Russia