Issue 
A&A
Volume 598, February 2017



Article Number  A106  
Number of page(s)  6  
Section  The Sun  
DOI  https://doi.org/10.1051/00046361/201629717  
Published online  08 February 2017 
Temperature dependent growth rates of the upperhybrid waves and solar radio zebra patterns
^{1} Department of Theoretical Physics and Astrophysics, Masaryk University, Kotlářská 2, 611 37 Brno, Czech Republic
email: jbenacek@physics.muni.cz
^{2} Astronomical Institute of the Czech Academy of Sciences, Fričova 258, 251 65 Ondřejov, Czech Republic
^{3} St.Petersburg State University, 198504 St.Petersburg, Russia
Received: 14 September 2016
Accepted: 24 November 2016
Context. The zebra patterns observed in solar radio emission are very important for flare plasma diagnostics. The most promising model of these patterns is based on double plasma resonance instability, which generates upperhybrid waves, which can be then transformed into the zebra emission.
Aims. We aim to study in detail the double plasma resonance instability of hot electrons, together with a much denser thermal background plasma. In particular, we analyse how the growth rate of the instability depends on the temperature of both the hot plasma and background plasma components.
Methods. We numerically integrated the analysed model equations, using Python and Wolfram Mathematica.
Results. We found that the growthrate maxima of the upperhybrid waves for nonzero temperatures of both the hot and background plasma are shifted towards lower frequencies comparing to the zero temperature case. This shift increases with an increase of the harmonic number s of the electron cyclotron frequency and temperatures of both hot and background plasma components. We show how this shift changes values of the magnetic field strength estimated from observed zebras. We confirmed that for a relatively low hot electron temperature, the dependence of growth rate vs. both the ratio of the electron plasma and electron cyclotron frequencies expresse distinct peaks, and by increasing this temperature these peaks become smoothed. We found that in some cases, the values of wave number vector components for the upperhybrid wave for the maximal growth rate strongly deviate from their analytical estimations. We confirmed the validity of the assumptions used when deriving model equations.
Key words: Sun: radio radiation / instabilities / methods: analytical
© ESO, 2017
1. Introduction
Zebra patterns (zebras) are fine IV radioburst type structures, observed during solar flares in the dm and mwavelength ranges (Slottje 1972; Chernov et al. 2012). They are considered to be an important source of information about the plasma density and intensity of the magnetic field in their sources.
There are many zebra models (Rosenberg 1972; Kuijpers 1975; Zheleznyakov & Zlotnik 1975; Chernov 1976, 1990; LaBelle et al. 2003; Kuznetsov & Tsap 2007; Bárta & Karlický 2006; Ledenev et al. 2006; Laptukhov & Chernov 2009; Tan 2010; Karlický 2013). The most promising one is based on the double plasma resonance instability of the plasma, together with losscone type electron distribution function (Zheleznyakov & Zlotnik 1975; Zlotnik 2013). In this model, the upperhybrid waves are first generated, then transformed to electromagnetic (radio) waves with the same (fundamental branch) or double frequency (harmonic branch) as the upperhybrid waves. This model has the simple resonance condition(1)where is the upperhybrid frequency of the background plasma, ω_{p} and ω_{B} are electronplasma and electroncyclotron frequencies and s is a integer harmonic number, is used for estimations of the magnetic field strength and electron plasma density in zebra radio sources (Ledenev et al. 2001; Zlotnik 2013; Karlický & Yasnov 2015). However, this resonance condition is only valid in the zerotemperature limit. If we want to analyse effects of temperatures on the zebra generation processes, we need to take the resonance condition in its general form, see relation 3.
In this paper we study these temperature effects in detail. It is shown that these effects require a correction in the method used to estimate magnetic field strength in zebra radio sources, especially for zebra stripes at high harmonics.
The paper is structured as follows: in Sect. 2 we present model equations describing the double plasma resonance instability and methods of their solution. Results are summarized in Sect. 3. Finally, the paper is completed by discussions and conclusions in Sects. 4 and 5.
2. Model
Similarly to Winglee & Dulk (1986), Yasnov & Karlický (2004), for the hot electron component we consider the DGH distribution function with the parameter j = 1 (Dory et al. 1965) (2)where u_{⊥} = p_{⊥}/m_{e} and u_{∥} = p_{∥}/m_{e} are electron velocities and p_{⊥} and p_{∥} are components of the electron momentum perpendicular and parallel to the magnetic field, and m_{e} is the electron mass. For simplification and in agreement with Winglee & Dulk (1986), we call v_{t} here the thermal velocity of hot electrons and we use the term the temperature of hot electrons, although the distribution function in relation 2 is not Maxwellian.
Unlike Winglee & Dulk (1986), we included the background plasma with nonzero temperature. Its density n_{b} is assumed to be much greater than the density of the hot electrons n_{h}.
In agreement with the approach by Melrose & Dulk (1982), Winglee & Dulk (1986), Yasnov & Karlický (2004), we use the condition for double plasma resonance instability in the form (3)where is the upperhybrid frequency of the background plasma, where the temperature effect is included, v_{tb} is the thermal velocity of the background plasma, is the Lorentz factor, k is the absolute value of the wave number vector. Its componets k_{∥} and k_{⊥} are in parallel and perpendicular directions to the magnetic field.
Then, starting from the basic equations presented in Winglee & Dulk (1986), Yasnov & Karlický (2004), we derived the relation for the growth rate Γ_{UH} of the upperhybrid waves as
where n_{h} is the hot electron density, e is the electron charge, r_{pB} is the ratio ω_{p}/ω_{B}, J_{s}(x) is the Bessel function of first kind of sth order and λ,σ are dimensionless parameters (9)and G^{±} are functions
The term comes from original relation of derivation distribution function of hot electrons (k_{∥}u_{⊥}∂f/∂u_{∥}) /γ (Winglee & Dulk 1986, Eq. (A8)). As shown below, this term is negligible, and thus in our computations we use G^{±} = g_{1}.
The sum h^{+} + h^{−} expresses a simultaneous effect of the both operators h^{+},h^{−} on one upperhybrid wave described by the specific kvector. In our computations we used both operators, but we found that term h^{−} was always at least two orders lower than h^{+} and the typical difference was ten orders.
Equations (4)–(8)are valid for k_{⊥} ≫ k_{∥}, see Winglee & Dulk (1986). We note that comparing these relations with those in the paper by Yasnov & Karlický (2004) the growth rate (relation 5, G^{±} = g_{1}) is proportional to s^{3}, not to s^{2}.
The integration is done for velocities up to their maxima (13)from which we get the followning conditions for maximal and minimal value of λ and σ (expressions under root in previous equations equal zero):
For the comparison below, we add values of σ and λ for the maximal growth rate as follows from analytical estimations made by Winglee & Dulk (1986)
2.1. Methods
We used Python SympPy^{1} library for analytical application and Python SciPy^{2} library for numerical computations of growth rate Eqs. (4)–(8), (13)–(16).
Generally, the analytical expressions for the growth rate (relations 4–8) depend on v_{t}, v_{tb}, λ, σ, s and r_{pB}. Their numerical solutions are made in several steps as described below.
First of all is the choice of thermal velocities v_{t}, v_{tb}. Then we selected the r_{pB} interval in which computations are made and steps in this interval. We usually use the interval r_{pB} = 3−20 with the step as Δr_{pB} = 0.03.
For each value of r_{pB} we searched for s which fulfill s = s_{0}−m,...,s_{0} + n, where s_{0} = Round(r_{pB}) is the round value of r_{pB}. Numbers m,n ∈N creates the interval of s for which the growth rate can be computed. However, we limited this interval only for s, maximal values of the growth rate of this interval are at least one hundredth of the maximal growth rate for s_{0}.
Next, values of v_{t}, v_{tb}, r_{pB} and s were chosen, and values of remaining variables λ and σ, which correspond to the kvector components of the upperhybrid waves, need to be specified. We chose these values in the intervals σ ∈ (σ_{min},σ_{max}) and λ ∈ (λ_{min},λ_{max}) on equidistant lattice. If the maximal values of σ_{max} and λ_{max} are too large or not defined, the upper boundaries are chosen as ten times of their minimal values. It was found to be sufficient in all cases.
Only then it is possible to compute the growth rate given by relations between four and eight for parameters v_{t}, v_{tb} and r_{pB} for each s and in all points of the map λ−σ. In following step we summed the maps in each specific (λ−σ)point over s. Finally, in the resulting map we searched for the point (λ_{Γmax},σ_{Γmax}), where is the highest value of the growth rate, which is then that determined for chosen r_{pB}. The wave number components of the upperhybrid wave with the maximal growth rate is then determined by Eq. (9).
3. Results
We solved the above described equations for the parameters shown in Table 1, for r_{pB} = 3−20 and B = 100 G. In Models 1−3, we changed background temperature while temperature of the hot electrons remains constant. Models 4 and 5 consider higher temperatures of the hot electrons comparing with Model 1, while the temperature of the background plasma is fixed.
Computation parameters.
Fig. 1 Example of the comparison of the growth rates computed with and without the term (Eq. (5)), for Model 1 and s = 6. We note that the growth rate at this and following figures are normalized by the term n_{h}ω_{B}. 

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First, we tested an importance of the correction term in Eq. (10)for computation of the growth rate. An example of such comparison is shown in Fig. 1. We found that in all models differences in values of the growth rate in models with and without this term is less than 5%, and at their maxima even smaller. Thus, we consider the effect of this term negligible and in all following computations we suppose .
Fig. 2 Growth rates in the λ−σ space: Model 1 (top), Model 4 (middle), Model 5 (bottom); all computed for s = 6 and r_{pb}, for which the growth rate is maximal. In Model 1 r_{pb} = 5.8, compare with Fig. 3. Black diamonds show positions of maximal values of the growth rate. 

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Fig. 3 Values of σ (top) and λ (bottom) for Model 1 and s = 6, where the growth rate has the maximal value depending on r_{pB}. Solid lines show values of the maximal growth rate, dashdotted lines are boundaries of the σ−λ space. Where dashdotted lines are not shown, the boundaries are outside the presented region. 

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In computations of the growth rate in all models (see Table 1) we followed steps described in Methods. Thus, we obtained many maps in the λ−σ space, corresponding to the kvector space. We note that the relations between the λ−σ and kvector space is given by relation 9.
Examples of such maps for s = 6 at their maxima are shown in Fig. 2. In each of these maps the maximal growth rate is indicated. Then we summed the maps over s and in the resulting map we searched for the maximal growth rate. This growth rate then corresponds to one point of the curve in Fig. 4.
To compare the computed and analytically estimated (relations 17–18) kvectors, which correspond to the maximal growth rate for the cases presented in Fig. 2, these are shown in Table 2. Thus, the assumption (k_{⊥} ≫ k_{∥}) used in derivation of the growthrate relations was fulfilled in all studied Models. All computed kvectors are smaller than that analytically predicted. Their computed perpendicular components are systematically two times less than analytical ones. This is due to assumptions and simplifications made in analytical estimations of these values. Computed values of k_{∥} decrease with increasing temperature in contradiction with analytical predictions.
Examples of values σ_{Γ,max},λ_{Γ,max} for v_{t} = 0.1 c (Model 1), where the growth rate has the maximal value depending on r_{pb}, are presented in Fig. 3. Values of σ_{Γ,max} for r_{pB} ~ 5 and r_{pB} > 6 are close to the lower boundary (given by Eq. (15)). However, in the region around the growthrate maximum they deviate from the lower boundary. Values of λ_{Γ,max} are changing only slightly. The steps in curves are due to discretisation of the λ−σ space. Note that the value λ_{Γ,max} ≈ 5 (Fig. 3, bottom) is less then predicted value s^{2}/ 2 = 18.
Fig. 4 Growth rates in Models shown in Table 1 in dependence on r_{pB} = ω_{p}/ω_{B}. Upper part: growth rates for Models 1, 4 and 5 with the fixed background temperature v_{tb} = 0.018c. Bottom part: growth rates for Models 1–3 with the fixed temperature of hot electrons v_{t} = 0.1c; detailed view. 

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Based on many such λ−σ maps the growthrate in dependence on the r_{pB} = ω_{p}/ω_{B} were computed for all Models according to Table 1. These growth rates are shown in Fig. 4. The upper part of this figure shows an effect of the temperature increase of the hot electrons for fixed temperature of the background plasma electrons, and its bottom part an effect of the temperature increase of the background plasma electrons for fixed temperature of hot electrons.
As seen in the upper part of this figure, Model 1 with the lower velocity of hot electrons have higher growth rates than those in Models 4 and 5 for all r_{pB} = ω_{p}/ω_{B}. Furthermore, the temperature increase of hot electrons smooths peak maxima in the growth rate. While Model 1 shows distinct maxima, in Model 5 the maxima for s> 5 are hardly recognisable.
On the other hand, the change of the thermal velocity of background electrons in Models 1–3 for fixed temperature of hot electrons (see the bottom part of the Fig. 4) do not change values of the growth rate, but the temperature increase shifts the maxima slightly to lower r_{pB}. The values of maxima generally decrease with an increase of r_{pB}.
Fig. 5 Ratio between maxima and minima of growth rate depending on s for Models 1, 4 and 5. 

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Fig. 6 Relative frequency shift Δω of growthrate maxima between predicted values by ω_{UH} = sω_{B} and its computed position (see Fig. 4). Top: Models 1, 4 and 5 with changing hot electrons temperature; bottom: Models 1–3 with changing background temperature. 

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As already mentioned, maxima of the growth rates are more distinct for lower temperatures of the hot electrons. Therefore in Fig. 5 we present ratios of these maxima and neighbouring minima of the growth rate in dependence on s. We note that there is a simple relation between s and r_{pB}; . As seen in Fig. 5, the ratios decrease with increasing s. It does not depend on the temperature of background electrons.
There is another interesting effect of temperatures of the both hot and background plasma electrons. Namely, by increasing these temperatures, the growthrate maxima are shifted to lower frequencies as shown in Fig. 6.
In Fig. 7 we present this effect in a way that is more appropriate for zebra pattern analysis. Here we show growthrate dependence on the ratio ω_{UH}/ω_{B} = s for Model 1, meaning that, with the magnetic field intensity B = 100 G (f_{B} = ω_{B}/ 2π= 280 MHz) and for the model with similar parameters as in Model 1, except that the magnetic field intensity is B = 10 G (f_{B} = ω_{B}/ 2π= 28 MHz). At the horizontal axis of this figure we used the ratio ω_{UH}/ω_{B}, because ω_{UH} can be directly determined from frequencies of the observed zebra stripes. As shown here, the growthrate maxima do not correspond to a simple resonance conditions (relation 1), which is used in estimations of the magnetic field and plasma density in the zebra radio sources from observed zebras. The maxima are shifted to lower frequencies, and this shift increases with the increase of s. Moreover, as seen in Fig. 7, the relative bandwidth of the growthrate maxima also increases with the increase of s.
Fig. 7 Growth rate for Model 1 (B = 100 G, f_{B} = ω_{B}/ 2π= 280 MHz) (blue line) and the model with similar parameters to Model 1, except the magnetic field intensity B = 10 G (f_{B} = ω_{B}/ 2π= 28 MHz) in dependence on ω_{UH}/ω_{B}. Numbers close the growthrate maxima designate s from computations. We note that the growth rate at this figure is normalized by the term n_{h}ω_{B}. 

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Fig. 8 Comparison of the growth rates with summation over s and for s with the maximal growth rate, for Model 1 (blue line) and Model 5 (green line). Dashed lines show summation over s and solid lines correspond to s with the maximal growth rate. 

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We also analyzed an effect of summation over s in relation 4 in comparison with the case for s with the maximal growth rate, see Fig. 8 made for Models 1 and 5. As seen here, for lower temperatures v_{t} the summation increases values of the growthrate minima and for higher temperatures the growth rate is enhanced in the whole range. We found that if for a given s the growth rate decreases steeply from its maximum (the case with lower v_{t}), the summation is important at places where the individual orders overlap. But if the decrease of the growth rate from its maximum is gradual (the case with higher v_{t}), the summation influences the growth rate in a broad range of r_{pB}.
4. Discussion
In the present paper we studied effects of nonzero temperatures of the both hot and background plasma on the growth rate. We showed that including effects of nonzero temperatures leads to shifts in the growthrate maxima to lower frequencies, comparing frequencies derived from the simple resonance condition ω_{UH} = sω_{B}. We found that these shifts are greater for higher values of the cyclotron harmonic number s. Because the simple resonance condition is used in estimations of the magnetic field and plasma density in the zebra radio sources, these shifts influence such estimations.
Therefore, let us estimate an error in the magnetic field determination from some zebra stripes using the simple resonance condition. For this purpose, let us assume the zebra stripe on the frequency f = f_{UH} = ω_{UH}/ 2π= 504 MHz (assuming the emission on the fundamental frequency) with s= 18. If we use the simple resonance condition then for such high s the ratio of r_{pB} = ω_{p}/ω_{B}≈s, and thus f_{B} = ω_{B}/ 2π= 28 MHz, which gives the magnetic field B= 10 G, see also Fig. 7. But, for modified Model 1 with B= 10 G we found that the emission maximum for s= 18 is shifted to ω_{UH}/ω_{B}= 17.3. From observations, we have f_{UH} = ω_{UH}/ 2π= 504 MHz, thus f_{B} = 504/17.3≈ 29.1 MHz, which gives the magnetic field B= 10.4 G. This example shows a 4% error in magnetic field estimation. As shown in Fig. 6, the shift of the growth rates grows linearly with s. However, the relative error of determining the magnetic field does not depend on s. For higher temperatures of hot electrons errors in magnetic field estimations are larger. For example, for Model 4 (recognisable maxima only for s< 11) this error is ≈16%.
The growth rate is proportional to the density of the hot plasma n_{h} and inversely proportional to the magnetic field. If we multiply the growth rate for Model 3 (with zero temperature of the background plasma), expressed in our paper as Γ_{UH}/ (ω_{B}n_{h}) by the density n_{h} = 10^{8} cm^{3} we obtain the growth rate, which agrees with that by (Winglee & Dulk 1986).
In agreement with the results by Yasnov & Karlický (2004) we found that for a relatively low temperature of the hot electrons (Model 1) the dependence of the growth rate vs. the ratio of the electron plasma and electron cyclotron frequencies expresses distinct peaks and increasing this temperature (Models 4 and 5) these peaks are smoothed, especially for high s. This growthrate behaviour differs from those in previous studies (Zheleznyakov & Zlotnik 1975; Winglee & Dulk 1986). The difference is caused by relativistic corrections used in the present
paper in both resonance terms in Eq. (3)and in selection of maximal growth rates in kmaps. We note that a similar effect in growthrate behaviour was found by Kuznetsov & Tsap (2007). Namely, considering the powerlaw and losscone distribution function of hot electrons, they showed that stripes of a zebra pattern become more pronounced with an increase of the losscone opening angle and the powerlaw spectral index.
We also studied effects of the neglected term in the growth rate with (Winglee & Dulk 1986, Eq. (A8)). We found that these effects are negligible.
5. Conclusions
We found that the growthrate maxima of the upperhybrid waves for nonzero temperatures of the both hot and background plasma are shifted towards lower frequencies comparing to the zero temperature case. It was found that this shift increases with an increase of the harmonic number s of the electron cyclotron frequency and temperatures of the both hot and background plasma components.
We showed that this shift of the growthrate maxima influences estimations of the magnetic field strength in sources of observed zebras. In agreement with previous studies we found that for a relatively low temperature of the hot electrons the dependence of the growth rate vs. the ratio of the electron plasma and electron cyclotron frequencies expresses distinct peaks and increasing this temperature these peaks are smoothed.
We found that in some cases the values of components of the wave number vector of the upperhybrid wave for the maximal growth rate strongly deviate from their analytical estimations. Validity of the assumptions used in derivation of the model equations was confirmed.
Acknowledgments
The authors thank G. P. Chernov for useful comments. We acknowledge support from Grants P209/12/0103. Access to computing and storage facilities owned by parties and projects contributing to the National Grid Infrastructure MetaCentrum provided under the programme “Projects of Projects of Large Research, Development, and Innovations Infrastructures” (CESNET LM2015042), is greatly appreciated. L.Y. acknowledges support by the RFBR grant (No. 160200254).
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All Tables
All Figures
Fig. 1 Example of the comparison of the growth rates computed with and without the term (Eq. (5)), for Model 1 and s = 6. We note that the growth rate at this and following figures are normalized by the term n_{h}ω_{B}. 

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In the text 
Fig. 2 Growth rates in the λ−σ space: Model 1 (top), Model 4 (middle), Model 5 (bottom); all computed for s = 6 and r_{pb}, for which the growth rate is maximal. In Model 1 r_{pb} = 5.8, compare with Fig. 3. Black diamonds show positions of maximal values of the growth rate. 

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In the text 
Fig. 3 Values of σ (top) and λ (bottom) for Model 1 and s = 6, where the growth rate has the maximal value depending on r_{pB}. Solid lines show values of the maximal growth rate, dashdotted lines are boundaries of the σ−λ space. Where dashdotted lines are not shown, the boundaries are outside the presented region. 

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In the text 
Fig. 4 Growth rates in Models shown in Table 1 in dependence on r_{pB} = ω_{p}/ω_{B}. Upper part: growth rates for Models 1, 4 and 5 with the fixed background temperature v_{tb} = 0.018c. Bottom part: growth rates for Models 1–3 with the fixed temperature of hot electrons v_{t} = 0.1c; detailed view. 

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In the text 
Fig. 5 Ratio between maxima and minima of growth rate depending on s for Models 1, 4 and 5. 

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In the text 
Fig. 6 Relative frequency shift Δω of growthrate maxima between predicted values by ω_{UH} = sω_{B} and its computed position (see Fig. 4). Top: Models 1, 4 and 5 with changing hot electrons temperature; bottom: Models 1–3 with changing background temperature. 

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In the text 
Fig. 7 Growth rate for Model 1 (B = 100 G, f_{B} = ω_{B}/ 2π= 280 MHz) (blue line) and the model with similar parameters to Model 1, except the magnetic field intensity B = 10 G (f_{B} = ω_{B}/ 2π= 28 MHz) in dependence on ω_{UH}/ω_{B}. Numbers close the growthrate maxima designate s from computations. We note that the growth rate at this figure is normalized by the term n_{h}ω_{B}. 

Open with DEXTER  
In the text 
Fig. 8 Comparison of the growth rates with summation over s and for s with the maximal growth rate, for Model 1 (blue line) and Model 5 (green line). Dashed lines show summation over s and solid lines correspond to s with the maximal growth rate. 

Open with DEXTER  
In the text 
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