# Oblique Bernstein Mode Generation Near the Upper-hybrid Frequency in Solar Pre-flare Plasmas

- 547 Downloads
- 2 Citations

## Abstract

We study analytically the generation process of the first harmonics of the pure electron weakly oblique Bernstein modes. This mode can appear as a result of the rise and development of a corresponding instability in a solar active region. We assume that this wave mode is modified by the influence of pair Coulomb collisions and a weak large-scale sub-Dreicer electric field in the pre-flare chromosphere near the footpoints of a flare loop. To describe the pre-flare plasma we used the model of the solar atmosphere developed by Fontenla, Avrett, and Loeser (*Astrophys. J.* **406**, 319, 1993). We show that the generated first harmonic is close to the upper-hybrid frequency. This generation process begins at the very low threshold values of the sub-Dreicer electric field and well before the beginning of the preheating phase of a flare. We investigate the necessary conditions for the existence of non-damped first harmonics of oblique Bernstein waves with small amplitudes in the flare area.

## Keywords

Pre-flare chromosphere Plasma instabilities Microwave emission## 1 Introduction

The understanding of the physical connection between the solar flare process and microwave emission from an active region (AR) has been an interesting and important problem of modern solar physics for several decades. Based on the electro-magnetic (EM) radiation in the frequency range 1 – 100 GHz generated at the footpoint of a magnetic loop, we consider the possibility of predicting in a short time interval the flare appearance in an AR. We analyse the potential mechanisms of plasma turbulence generation through plasma instabilities that appear before solar flare eruptions. We have made a few important assumptions. First, we assume a weak and quasi-static electric field in the magnetic loop. The existence of such a field has been confirmed by the additional Stark broadening of Balmer \(\mathrm{H}_{\upbeta}\) lines with principal quantum numbers \(N>8\) (see *e.g.* Foukal and Hinata, 1991). Furthermore, we also assume that energetic particle beams are not present in the lower and middle chromosphere, as this allows us to investigate the pre-flare stage in regions where the first energy release is not observed in general (see *e.g.* Hudson, 2007; Melnikov, Shibasaki, and Reznikova, 2002). We note that the findings presented here can be directly compared with previous observational results in a limited number of cases (see *e.g.* Bogod and Yasnov, 2009; Zharkova *et al.*, 2011; Kashapova, Meshalkina, and Kisil, 2012). In contrast, the majority of studies of microwave radiation from ARs consider either impulsive or gradual processes: flare or post-flare conditions with beams of energetic particles and without large-scale, quasi-static, sub-Dreicer (see *e.g.* Miller *et al.*, 1997) electric fields.

To explain a burst of microwave emission from solar magnetic loop structures, Holman, Eichler, and Kundu (1980) proposed the gyrosynchrotron masering mechanism. The authors pointed out that the observed GHz frequency of the gyrosynchrotron emission requires a magnetic field with a strength of a few kilogauss. Vlahos (1987) mentioned, among other characteristics of electron-cyclotron maser emission (ECME), that the frequency of emitted radiation is present around the first or second harmonics of the cyclotron frequency. For solar atmospheric parameters, the frequency of emitted radiation is equal to 2 – 3 GHz. The properties of the ECME at different harmonics of the electron-cyclotron frequency, \(\Omega_{\mathrm{e}}\), in the range \(\omega =1.16\,\mbox{--}\,1.69~\mbox{GHz}\) have been studied by Krucker and Benz (1994). Between 0.3 and 3 GHz, the microwave emission has been detected at frequencies, which are close enough, but do not coincide with integer values of \(\Omega_{\mathrm{e}}\). A possible explanation of this has been proposed by Willes and Robinson (1996). These authors assumed that several adjacent Bernstein modes can be excited by the cyclotron maser mechanism and radiation can escape from the solar atmosphere as a result of non-linear wave–wave interactions. Bogod *et al.* (2000) suggested the presence of emission in a close-frequency range, such as thermal cyclotron radiation at the third harmonics of \(\Omega_{\mathrm{e}}\) from a compact source in an solar AR. This mechanism can be considered as an alternative to ECME. Melnikov, Shibasaki, and Reznikova (2002) have analysed the microwave sources in extended solar flaring loops at 17 and 34 GHz. The authors studied the origin of enhanced losses of trapped particles in the lower part of a magnetic loop and proposed that this process can be explained by two possible mechanisms: (i) Coulomb collisions in a growing plasma density or (ii) scattering on locally (near footpoint) enhanced wave turbulence. This confirms that the overwhelming majority of the observational flare data in magnetic loops correspond to the impulsive and gradual phases of this process. Exceptions are very rare, but exist. For example, Bogod and Yasnov (see *e.g.* 2009) reported on spikes of microwave emission from NOAA AR 9077 in its pre-flare stage during four days before the Bastille Day flare, which occurred on 14 July 2000. The observations had been carried out in the frequency band from 4 to 16 GHz. Calculations and estimates have shown that the radiating region was probably surrounded by a magnetic field with \(|\mathbf{B}_{0}|<10\,\mbox{--}\,40~\mbox{G}\) (see *e.g.* Bogod and Yasnov, 2009). Kryshtal, Gerasimenko, and Voitsekhovska (2012) pointed out that values of the electron-cyclotron frequency in the range 1 – 40 GHz correspond to magnetic fields in the kilogauss range (in S. Solanki’s terminology, see *e.g.* Solanki, 1993). Hudson (2007) proposed using 10 G and 1000 G as representative values for the magnetic field strength of chromospheric flares. In this article, we have considered magnetic field strengths of the order of kilogauss (see *e.g.* Solanki, 1993). The presence of a sub-Dreicer field at the early stage of the flaring process (*i.e.* pre-flare phase) can initiate a number of plasma wave instabilities (see *e.g.* Kryshtal and Gerasimenko, 2004; Kryshtal, Gerasimenko, and Voitsekhovska, 2012; Kryshtal *et al.*, 2013; Kryshtal, Gerasimenko, and Voitsekhovska, 2014). The instabilities with extremely low threshold of excitation are most important (Kryshtal, Gerasimenko, and Voitsekhovska, 2012). We note that electromagnetic-wave emission during the linear stage of the instability development, assuming a small growth rate, can be generated by nonlinear parametric decay or wave coalescence.

## 2 Wave Sources and Three-wave Interactions

*i.e.,*

*e.g.*Alexandrov, Bogdankevich, and Rukhadze, 1984). Yukhimuk

*et al.*(1998) have shown that the parametric decay of the upper-hybrid pump wave (UHW) into a kinetic Alfvén wave (KAW) and an EMW is possible in the solar atmosphere,

*i.e.*,

*e.g.*Alexandrov, Bogdankevich, and Rukhadze, 1984; Krall and Trivelpiece, 1973). Under additional conditions (see

*e.g.*Chen, 1984), the generated EMW could be leaky,

*i.e.*the generated waves can leave the generation area and, as a result, can be detected. Therefore, the identification of the necessary conditions for the development of low-threshold instabilities becomes an important problem for short-term flare prediction. There are two different types of short-term flare forecast in ARs. Conventionally, we can call them synoptic and causal forecast. The first approach is well developed and could be applied for most cases. The synoptic approach is based on evidence observed in the AR before the flare, such as (i) the maximum horizontal gradient of the magnetic field, (ii) the length of the neutral line as an indicator of flare productivity, and (iii) the number of singular points (see

*e.g.*Yu

*et al.*, 2010; Li and Zhu, 2013). The causal forecast is based on a model of the flaring process (see

*e.g.*Willes and Robinson, 1996; Miller

*et al.*, 1997; Bogod

*et al.*, 2000; Kryshtal, Gerasimenko, and Voitsekhovska, 2012). The most realistic forecast should include both approaches (see

*e.g.*Núñez

*et al.*, 2005). However, this requires more accurate high-resolution measurements. The instability parameters, theoretically obtained in this article, and the observational results form other authors can only be directly compared when the microwave radiation has been registered during the pre-flare stage in the AR (see

*e.g.*Bogod and Yasnov, 2009; Zharkova

*et al.*, 2011; Kashapova, Meshalkina, and Kisil, 2012).

In comparison with the generation of second harmonics (see *e.g.* Kryshtal, 1998; Kryshtal, Gerasimenko, and Voitsekhovska, 2012), the excitation of the first harmonic is more likely because of its higher probability. To confirm this, it is necessary to obtain the instability threshold value in the vicinity of upper-hybrid frequency and to show that this value is extremely low. In this article, we obtain the boundary values of the main characteristics of pre-flare plasma and wave perturbation, and investigate the possibility of the generation of non-damped oscillations (waves) with small amplitudes. The comparison of the excitation threshold values for the first and second harmonics is also an important problem. For example, the beginning of EM radiation at the electron-cyclotron harmonics with non-integer numbers (Willes and Robinson, 1996) is possible if the threshold values of the first harmonic are of the same order as the second. On the other hand, when these threshold values are significantly different, the harmonic with a lower threshold value will be generated earlier with no influence of another harmonic.

In this article, we propose the necessary conditions for a causal short-term forecast, *i.e.* conditions for emergence of microwave radiation in the solar ARs before a flare. We investigate solely the linear stage of the perturbation development since it is the most important and relevant for forecasting.

## 3 Equations and Approximations

*e.g.*Alexandrov, Bogdankevich, and Rukhadze, 1984)

*e.g.*Chen, 1984)

*e.g.*Alexandrov, Bogdankevich, and Rukhadze, 1984),

*e.g.*Miller

*et al.*, 1997). According to the flare model proposed by Heyvaerts, Priest, and Rust (1977), the earliest (

*i.e.*pre-heating) stage of a flare process precedes the flash (or impulsive) phase. During this pre-heating phase the Buneman plasma instability (see

*e.g.*Alexandrov, Bogdankevich, and Rukhadze, 1984; Chen, 1984) develops if the stream velocity \(\mathbf{u}\) exceeds the electron thermal velocity \(v_{\mathrm{Te}}\). In this article we investigate the flare phase that precedes the pre-heating phase. This is the situation when a sub-Dreicer electric field exists in the region under study. The expression for the instability growth rate was first obtained by Kryshtal (1997). Here we apply its modified version. For high-frequency longitudinal waves, instead of the standard ion–electron collision frequency \(\nu_{\mathrm{ei}}\) (see Equation (4)), we used the effective frequency \(\nu^{*}_{\mathrm{ei}}\) of ion–electron collisions (see

*e.g.*Alexandrov, Bogdankevich, and Rukhadze, 1984):

*i.e.*

*e.g.*Fontenla, Avrett, and Loeser, 1993) of the solar atmosphere. These parameters are realistic enough for a magnetic loop footpoint in the interval of heights \(600\le H\le1400~\mbox{km}\). We assume that in this interval the condition \(\nu_{\mathrm{ei}}, \nu ^{*}_{\mathrm{ei}}\gg\nu_{\mathrm{0e}}, \nu_{\mathrm{0i}}\) is satisfied more strongly for the FAL model than for the MAVN (Machado

*et al.*, 1980) and VAL (Vernazza, Avrett, and Loeser, 1981) models, which have been studied previously (Kryshtal, 1997, 1998). Here \(\nu_{\mathrm{0e}}\) and \(\nu_{\mathrm{0i}}\) are the frequencies of collisions of neutral atoms with electrons and ions, respectively. Additionally, we assume that the inequality

*i.e.*is directed to the photosphere in our coordinate frame. The quasi-Bernstein modes discussed here are similar to the well-known neutralised Bernstein ion modes (Chen, 1984). In our case, \(\vert k_{*}\vert \) does not have such a limit because the main frequency \(\Omega_{\mathrm{e}}\gg\Omega_{\mathrm{i}}\) and the balance of charge separation is not rigid. But Equation (8) is very important to balance the Landau damping. We add one more condition

*e.g.*Chen, 1984; Krall and Trivelpiece, 1973),

*i.e.*

*i.e.*to calculate the resonant term in the series expansion of the dispersion relation for pure electron Bernstein modes (Krall and Trivelpiece, 1973; Chen, 1984), we apply the method described in Kryshtal (1997) and Kryshtal, Gerasimenko, and Voitsekhovska (2012). This approach allows us to take into account the small corrections that include \(\nu_{\mathrm{ei}}^{*}\ne0\), \(\varepsilon_{\mathrm{R}}\ne0\) and \(k_{\mathrm{*}}\ne0\) under the conditions given in Equations (5), (7), and (9). Obtaining a normalised growth rate for the first harmonic is difficult and tedious, even if the expression for \(\gamma\) is known for the second harmonic (Kryshtal, Gerasimenko, and Voitsekhovska, 2012). The calculations for each harmonic are independent and, therefore, have to be made separately. The free parameter \(\sigma\) takes into account the contribution of mutual collisions of all charged particles into the Bhatnagar–Gross–Krook (BGK) approximation of the collision integral (Alexandrov, Bogdankevich, and Rukhadze, 1984). The physical meaning of this integral and its use in calculations were described in detail before by Kryshtal and Kucherenko (1995, 1996) and Kryshtal, Gerasimenko, and Voitsekhovska (2012). The dispersion relation for pure electron Bernstein harmonics (with \(k_{\mathrm{z}}=0\), \(\nu=0\) and \(\varepsilon _{\mathrm{R}}=0\)) has the form (Krall and Trivelpiece, 1973)

*i.e.*

## 4 Results of the Calculations and Discussion

*e.g.*\(1\le\sigma\le6\), \(0.01 \le z_{\mathrm{e}} \le0.25\), \(0.001\le \vert k_{*}\vert \le0.2\) and \(5\times10^{-5}\le\varepsilon _{\mathrm{R}} \le1.5\times10^{-2}\). The calculated \(\Gamma\) sign change indicates waves with small constant amplitude,

*i.e.*oscillations at the level of the thermal noise. The boundary values of the perturbation parameters for five possible modifications of the FAL solar atmosphere model (see Table 1) are summarised in Table 2 for the first and in Table 3 for the second oblique Bernstein harmonics. These modifications include two physical scenarios A and P. A corresponds to the case when at the specific height H the chromospheric temperature and plasma density are lowest, and P corresponds to the highest values of these parameters at the same height H (

*see e.g.*Fontenla, Avrett, and Loeser, 1993). We note that the condition when the reduced growth rate \(\Gamma\) is lower than zero but extremely close to it corresponds to plasma processes with a large number of subcritical instabilities. To obtain the values of \(\Gamma\) we applied two additional conditions for \(z_{\mathrm{e}}\), \(k_{*}\) and \(\varepsilon_{\mathrm{R}}\). Specifically, (1) first positive value of \(\Gamma\) after \(\Gamma\) changes the sign from negative to positive has to be as low as possible, (2) if condition (1) is satisfied, the value of at least one of \(z_{\mathrm {e}}\), \(k_{*,}\) or \(\varepsilon_{\mathrm{R}}\) should be at minimum. For the calculation, we applied condition (2) to \(z_{\mathrm{e}}\). As a result of this procedure, we identify a single set of values wherein the limit values of \((\varepsilon_{\mathrm{R}} )_{\mathrm {bound}}\), \((k_{*} )_{\mathrm{bound}}\) and \((z_{\mathrm {e}} )_{\mathrm{bound}}\) are minimised. Formally, the condition \(\Gamma>0\) leads to small or very small changes in the limiting values of other parameters. However, when \(z > (z_{\mathrm{e}} )_{\mathrm{bound}}\) the instability is present, but in this case, conditions (1) and (2) are violated. We note that for all cases the limiting values are defined by taking the first values at which the negative reduced growth rate \(\Gamma\) becomes positive.

Main physical characteristics of the plasma from the FAL model of solar atmosphere. P1, P2, P3, A1, and A3 denote the five different sets of plasma parameters.

Modification | \(n_{\mathrm{e}}\) | \(T_{\mathrm{e}}=T_{\mathrm{i}}\) | \(B_{\mathrm{0}}\) | | \(\omega_{\mathrm{pe}}\) | \(\Omega_{\mathrm{e}}\) | \(\nu_{\mathrm{ei}}^{*}\) |
---|---|---|---|---|---|---|---|

\([10^{11}~\mbox{cm}^{-3}]\) | [K] | [mT] | [km] | \([10^{10}~\mbox{s}^{-1}]\) | \([10^{10}~\mbox{s}^{-1}]\) | \([10^{7}~\mbox{s}^{-1}]\) | |

P1 | 2.50 | 5220 | 321 | 650 | 2.81 | 5.64 | 2.56 |

P2 | 3.02 | 5480 | 321 | 700 | 3.10 | 5.64 | 2.89 |

P3 | 4.79 | 7420 | 145 | 1380 | 3.80 | 2.56 | 1.23 |

A1 | 0.714 | 4390 | 321 | 650 | 1.51 | 5.64 | 0.95 |

A3 | 0.31 | 6150 | 145 | 1375 | 0.97 | 2.56 | 0.093 |

The calculated values of the principal characteristics of the first oblique Bernstein harmonic instability for plasma parameters provided in Table 1.

Modification | \((\varepsilon_{\mathrm{R}})_{\mathrm{bound}}\times 10^{-4}\) | \((k_{*} )_{\mathrm{bound}}\times 10^{-3}\) | \((z_{\mathrm{e}} )_{\mathrm{bound}}\) | \(\Gamma_{(+)\mathrm{min}}\) or \(\Gamma_{(-)\mathrm{max}}\) |
---|---|---|---|---|

P1 | – | – | – | −0.002 |

P2 | – | – | – | −0.0023 |

P3 | 1.1 | 25.1 | 0.2 | 2.21 × 10 |

A1 | – | – | 0.17 | −8.8 × 10 |

A3 | 1.0 | 155.4 | 0.15 | 1.31 × 10 |

The calculated values of the principal characteristics of the second oblique Bernstein harmonic instability for plasma parameters provided in Table 1.

Modification | | \((\varepsilon_{\mathrm{R}}^{||})_{\mathrm{bound}}\times10^{-4}\) | \((k_{*}^{||} )_{\mathrm{bound}}\times10^{-3}\) | \((z^{||}_{\mathrm{e}} )_{\mathrm{bound}}\) | \(\Gamma^{||}_{1+}\) |
---|---|---|---|---|---|

P1 | – | 10 | 15.6 | 0.02 | 1.5 × 10 |

P2 | – | 0.95 | 1.3 | 0.022 | 1.1 × 10 |

P3 | 5 | 1.1 | 1.2 | 0.021 | 1.4 × 10 |

A1 | – | – | – | – | – |

A3 | 5 | 1.05 | 17.4 | 0.019 | 2.8 × 10 |

*i.e.*FAL P3 and FAL A3, respectively. The curve \(\Gamma (0.2,k_{*} )\) for FAL A3 corresponds to the subcritical instability. These instabilities are not marginal with respect to the parameters \(z_{\mathrm{e}}\) and \(k_{*}\) because they do not exist at the limit of the corresponding interval of variation of the parameters. The odd powers of \(k_{*}\) in the expression for the reduced growth rate \(\Gamma\) (see Equation (12)) lead to an interesting result: the process of the initial appearance and subsequent development of the instability is asymmetric with respect to the sign change of \(k_{*}\). Therefore, the behaviour of \(\Gamma\equiv\Gamma (z_{\mathrm{e}}, k_{*} )\) is very different for positive and negative values of \(k _{*}\) for the same and different solar atmospheric models. Figures 1 and 2 reflect this fact for FAL P3 and FAL A3 models, respectively.

*i.e.*\(\omega_{\mathrm{EMW}}\approx\omega_{1}\) (see Equation (15) for \(\omega_{1}\)). We note that the threshold values of \(\varepsilon_{\mathrm{R}}\) for the first and second harmonics are practically equal for FAL P3 and FAL A3 models (Kryshtal, Gerasimenko, and Voitsekhovska, 2012). Therefore, they can be simultaneously generated. The calculated frequencies of generated undamped waves are the following: \(f^{(1)}_{\mathrm{theor}} (\mathrm{FAL \: P3} )\approx\Omega^{\mathrm{(1)}}_{\mathrm{e}}/{2\pi}\sqrt {1+2\omega^{2}_{*}\exp(-z )}=8.72~\mbox{GHz}\) and \(f^{(1)}_{\mathrm{theor}} (\mathrm{FAL \: A3} )=4.52~\mbox{GHz}\). The superscripts (1) and (2) later in the text denote the first and second harmonics, correspondingly. These values are agree well with some observations in pre-flare region, for example in (i) the flare in NOAA AR 9077 (13 July 2000) (Bogod and Yasnov, 2009) with \(f^{(1)}_{\mathrm{obs}}\cong5.0~\mbox{GHz}\) (main peak), (ii) the flare in NOAA AR 10652 (25 July 2004) (Zharkova

*et al.*, 2011) with \(f^{(1)}_{\mathrm{obs}}\cong4.99~\mbox{GHz}\) (burst-like structure in microwave emission before the initial phase of the flare), (iii) the flare in AR 11081 (N22W45, 12 June 2010) (Kashapova, Meshalkina, and Kisil, 2012) with \(f^{(1)}_{\mathrm{obs^{*}}}\cong4.6~\mbox{GHz}\), \(f^{(1)}_{\mathrm {obs^{**}}}\cong6.4~\mbox{GHz}\) (main peak), \(f^{(1)}_{\mathrm{obs^{***}}}\cong 9.4~\mbox{GHz}\) (burst-like structures in microwave emission before the initial phase of the flare). In these examples the authors considered a model that includes energetic electron beams. In our analysis we investigated the non-beam model of the instability development. For FAL P1 the first harmonic is absent, but the second harmonic can appear. As a result of wave coalescence (see Equation (1)), the frequency of EMW can reach a value of \(f^{(2)}_{\mathrm{theor}} (\mathrm{FAL \: P1} )=4\Omega^{\mathrm{(1)}}_{\mathrm {e}}/{2\pi}\sqrt{1+2\omega^{2}_{*}\exp (-z )}=35.92~\mbox{GHz}\).

We also found that for FAL P1 model the instability of the first harmonic is absent and the second harmonic has an extremely low threshold value \((\varepsilon_{\mathrm{R}} )_{\mathrm {bound}}\approx10^{-6}\). Therefore, the instability of the second harmonic can develop well before the first harmonic is generated (see also Kryshtal, Gerasimenko, and Voitsekhovska, 2012), and the frequency of the EMW has to be approximately the same as twice the frequency of the second pure electron harmonics.

The possibility of simultaneous generation of the first and second harmonics for FAL P3 and FAL A3 models indicates that harmonics with non-integer number (Willes and Robinson, 1996) can be present at the footpoint of the loop. The threshold values of \(\varepsilon_{\mathrm{R}}\) for these harmonics are extremely low. Similar values, *i.e.* \(10^{-4}\le\varepsilon_{\mathrm{R}}\le10^{-3}\), were obtained before by Kryshtal and Gerasimenko (2004, 2005) for kinetic Alfvén and kinetic ion-acoustic waves. The threshold values of \(\varepsilon_{\mathrm{R}}\) for longitudinal waves are significantly higher, *i.e.* \(0.01\le\varepsilon_{\mathrm{R}}\le 0.1\) (Kryshtal *et al.*, 2013; Kryshtal, Gerasimenko, and Voitsekhovska, 2014). We note that the second harmonic of oblique Bernstein waves for the FAL P1 model (Kryshtal, Gerasimenko, and Voitsekhovska, 2012) has the lowest threshold value of \(\varepsilon _{\mathrm{R}}=10^{-6}\). The specific properties of the pre-flare plasma and wave perturbation in that region mean that the dispersion relations for the upper-hybrid wave and first harmonics of pure electron weakly oblique Bernstein modes might coincide. The high-quality factors of the investigated instabilities show that their development can be considered as a periodic wave process that corresponds to the generation of small amplitude (*e.g.* at the level of thermal noise) undamped waves.

## Notes

### Acknowledgements

The authors would like to thank colleagues from the Department of Space Plasma Physics of the Main Astronomical Observatory for continuing support and discussion at seminars. VF acknowledges the financial support received from the Science and Technology Facilities Council (STFC), UK.

## References

- Alexandrov, A., Bogdankevich, L., Rukhadze, A.: 1984,
*Principles of Plasma Electrodynamics*, Springer, Berlin. CrossRefGoogle Scholar - Bogod, V.M., Garaimov, V.I., Zheleznyakov, V.V., Zlotnik, E.Y.: 2000,
*Astron. Rep.***44**, 271. DOI. ADSCrossRefGoogle Scholar - Chen, F.F.: 1984,
*Introduction to Plasma Physics and Controlled Fusion, Volume 1: Plasma Physics*, Springer, Berlin. CrossRefGoogle Scholar - Fontenla, J.M., Avrett, E.H., Loeser, R.: 1993,
*Astrophys. J.***406**, 319. DOI. ADSCrossRefGoogle Scholar - Heyvaerts, J., Priest, E.R., Rust, D.M.: 1977,
*Astrophys. J.***216**, 123. DOI. ADSCrossRefGoogle Scholar - Holman, G.D., Eichler, D., Kundu, M.R.: 1980, In: Kundu, M.R., Gergely, T.E. (eds.)
*Proc. of the Symp. Radio Physics of the Sun*, 457. CrossRefGoogle Scholar - Hudson, H.S.: 2007, In: Heinzel, P., Dorotovič, I., Rutten, R.J. (eds.)
*The Physics of Chromospheric Plasmas***368**, Astronomical Society of the Pacific, San Francisco, 365. Google Scholar - Kashapova, L.K., Meshalkina, N.S., Kisil, M.S.: 2012,
*Solar Phys.***280**, 525. DOI. ADSCrossRefGoogle Scholar - Krall, N.A., Trivelpiece, A.W.: 1973,
*Principles of Plasma Physics*, McGraw-Hill, New York. Google Scholar - Kryshtal, A.N., Gerasimenko, S.V.: 2004,
*Astron. Astrophys.***420**, 1107. DOI. ADSCrossRefGoogle Scholar - Kryshtal, A.N., Gerasimenko, S.V., Voitsekhovska, A.D.: 2012,
*Adv. Space Res.***49**, 791. DOI. ADSCrossRefGoogle Scholar - Kryshtal, A.N., Gerasimenko, S., Voitsekhovska, A., Fedun, V.: 2013,
*Ann. Geophys.***31**, 2193. DOI. ADSCrossRefGoogle Scholar - Kryshtal, A.N., Gerasimenko, S.V., Voitsekhovska, A.D.: 2014,
*Astrophys. Space Sci.***349**, 637. DOI. ADSCrossRefGoogle Scholar - Machado, M.E., Avrett, E.H., Vernazza, J.E., Noyes, R.W.: 1980,
*Astrophys. J.***242**, 336. DOI. ADSCrossRefGoogle Scholar - Melnikov, V.F., Shibasaki, K., Reznikova, V.E.: 2002,
*Astrophys. J. Lett.***580**, L185. DOI. ADSCrossRefGoogle Scholar - Miller, J.A., Cargill, P.J., Emslie, A.G., Holman, G.D., Dennis, B.R., LaRosa, T.N., Winglee, R.M., Benka, S.G., Tsuneta, S.: 1997,
*J. Geophys. Res.***102**, 14631. DOI. ADSCrossRefGoogle Scholar - Núñez, M., Fidalgo, R., Baena, M., Morales, R.: 2005,
*Ann. Geophys.***23**, 3129. DOI. ADSCrossRefGoogle Scholar - Vernazza, J.E., Avrett, E.H., Loeser, R.: 1981,
*Astrophys. J. Suppl.***45**, 635. DOI. ADSCrossRefGoogle Scholar - Yukhimuk, V., Voitenko, Y., Fedun, V., Yukhimuk, A.: 1998,
*J. Plasma Phys.***60**, 485. DOI. ADSCrossRefGoogle Scholar - Yu, D., Huang, X., Hu, Q., Zhou, R., Wang, H., Cui, Y.: 2010,
*Astrophys. J.***709**, 321. DOI. ADSCrossRefGoogle Scholar - Zharkova, V.V., Kashapova, L.K., Chornogor, S.N., Andrienko, O.V.: 2011,
*Mon. Not. Roy. Astron. Soc.***411**, 1562. DOI. ADSCrossRefGoogle Scholar

## Copyright information

**Open Access** This article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution, and reproduction in any medium, provided you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made.