Issue 
A&A
Volume 534, October 2011



Article Number  A116  
Number of page(s)  8  
Section  The Sun  
DOI  https://doi.org/10.1051/00046361/201116982  
Published online  18 October 2011 
Proton firehose instability in biKappa distributed plasmas
^{1}
Center for Plasma Astrophysics, Celestijnenlaan 200B,
3001
Leuven,
Belgium
email: marian.lazar@wis.kuleuven.be
^{2}
Institut für Theoretische Physik, Lehrstuhl IV: Weltraum und
Astrophysik, RuhrUniversität Bochum, 44780
Bochum,
Germany
Received:
30
March
2011
Accepted:
21
June
2011
Context. Protons or heavier ions with anisotropic velocity distributions and nonthermal departure from Maxwellian, are frequently reported in the magnetosphere and at different altitudes in the solar wind. These observations are sustained by an extended number of mechanisms of acceleration in any direction with respect to the interplanetary magnetic field. However, the observed anisotropy is not large and most probably constrained by the kinetic instabilities.
Aims. An excess of parallel kinetic energy, T_{∥}/T_{⊥} > 1 (where ∥ and ⊥ denote directions relative to the background magnetic field) drives a proton firehose mode to grow, limiting any further increase in the anisotropy according to the observations. The effects of suprathermal populations on the principal characteristics of the proton firehose instability are investigated.
Methods. For lowcollisional plasmas, the dispersion approach is based on the fundamental kinetic VlasovMaxwell equations. The anisotropy of plasma distributions including suprathermal populations is modeled by biKappa functions, and the new dispersion relations are derived in terms of the modified plasma dispersion function (for Kappa distributions), and analytical approximations of this function.
Results. Growth rates of the proton firehose solutions and threshold conditions are provided in analytical forms for different plasma regimes. The proton firehose instability needs a larger anisotropy and a larger parameter β_{∥} to occur in a Kappadistributed plasma. A precise numerical evaluation shows that the growth rates are, in general, lower and the wave frequency is only slightly affected, but the influence of suprathermal populations is essentially dependent on both the proton and electron anisotropies. Departures from the standard dispersion of a Maxwellian plasma can eventually be used to evaluate the presence of suprathermal populations in solar flares and the magnetosphere.
Key words: Sun: flares / plasmas / solar wind / instabilities / Sun: coronal mass ejections (CMEs)
© ESO, 2011
1. Introduction
Kinetic instabilities prevail in the solar wind (Cairns et al. 2000; Bale et al. 2009) as it is a dilute plasma that contains ample free energy, localized in flows, and a nonuniform heating (Marsch 2006; Bougeret & Pick 2007). In a poorcollisional plasma, these instabilities provide a plausible mechanism to prevent the development of excessive anisotropies and ensure a more fluidlike behavior (Hellinger et al. 2006; Stverak et al. 2008). Moreover, the electromagnetic wave turbulence leads to acceleration and pitchangle scattering and diffusion, and must therefore play an important role in the evolution of plasma particles in the solar wind and the magnetosphere (Dröge 2003; Schlickeiser et al. 2010; Pierrard et al. 2011)
Measurements of the plasma parameters at high altitudes in the solar wind (≲ 1 AU) closely agree with theoretical and numerical predictions (Gary et al. 1976; Quest & Shapiro 1996; Gary et al. 1998; Hellinger & Matsumoto 2000; Matteini et al. 2006) showing that any increase in the parallel proton temperature is constrained by the proton firehose instability (PFHI) (Kasper et al. 2002; Hellinger et al. 2006; Bale et al. 2009). This instability is driven by an excess of the parallel kinetic energy, i.e. temperature T_{p,∥} > T_{p,⊥} or pressure p_{∥} > p_{⊥}, and develops from a righthanded (RH) circularly polarized mode with a maximum growth rate at parallel propagation, i.e., k × B_{0} = 0. The mechanism that converts the kinetic energy of the protons and excites the firehose instability is essentially nonresonant, or fluidlike (Parker 1958; Pilipp & Völk 1971; Yoon 1995; Wang & Hau 2003). For a finite thermal spread, it has already been shown that resonant particles can also play an important role enhancing or suppressing the instability (Pilipp & Völk 1971; Gary et al. 1998), and shaping the proton distribution function to depart from the biMaxwellian form (Matteini et al. 2006). Resonant terms can, therefore, be considered whenever their contribution is expected to be significant.
Protons or heavier ions with suprathermal distributions have frequently been observed in the solar wind (Collier et al. 1996; Chotoo et al. 2000), the magnetosphere (Gloeckler & Hamilton 1987), or further in the heliosphere towards the termination shock (Decker et al. 2005; Fisk & Gloeckler 2007). There is abundant observational evidence indicating that particle energization and the occurrence of suprathermal populations are correlated with an enhanced activity of the waves and instabilities in space plasma. A brief description of these mechanisms of acceleration can be found in the review (referred to in Sect. 3) by Pierrard & Lazar (2010). Populations with suprathermal highenergy tails are most accurately modeled by the family of Kappa functions (Vasyliunas 1968; Summers & Thorne 1991), and may exhibit different wave dispersion and stability properties from a Maxwellian (Pierrard & Lazar 2010). Electrons with a surplus of parallel kinetic energy, T_{e,∥} > T_{e,⊥}, initiate the electron firehose instability (EFHI) of the lowfrequency lefthanded (LH) circularly polarized modes propagating parallel to the magnetic field. Modeling the anisotropy of suprathermal electrons with a biKappa distribution, Lazar & Poedts (2009) demonstrated that, compared to a biMawellian, the threshold of the EFHI increases, the maximum growth rates are slightly diminished, and the instability extends to large wave numbers.
The PFHI is also a lowfrequency growing mode but with a RH circular polarization, and is driven by the nonresonant protons with T_{p,∥} > T_{p,⊥}. Under the usual convention, protons resonate more easily with LH modes driving a proton cyclotron instability if T_{p,∥} < T_{p,⊥}. However, for an intense magnetization in lowβ plasmas, the same resonant protons can also cause the instability of the RH modes to grow. In this case, the growth rates are usually much lower than the proton gyrofrequency, but they can increase (by a few orders of magnitude), approaching the proton gyrofrequency as the abundance of the suprathermal protons increases (Xue et al. 1993; Dasso et al. 2003). In addition, we consider largeβ plasmas where deviations of the protons from an isotropic Maxwellian equilibrium can easily develop and drive the PFHI.
2. Parallel RH transverse modes in biKappa plasmas
We start from the general dispersion relation of the transverse modes propagating along the regular magnetic field with a RH circular polarization, e.g., Eq. (2) from Lazar & Poedts (2009), hereafter called Paper I, (1)where ω and k denote the frequency and the wave number of the plasma modes, respectively, c is the speed of light in a vacuum, Ω_{a} = q_{a}B_{0}/(m_{a}c) is the (nonrelativistic) gyrofrequency, and ω_{p,a} = (4πn_{a}e^{2}/m_{a})^{1/2} is the plasma frequency for the particles of species a. We use polar coordinates in the particle velocity space (2)The initial unperturbed plasma anisotropy is modeled with a biKappa velocity distribution function of plasma particles (3)which is normalized by . Here, (4)with (5)and (6)denote the perpendicular and parallel thermal velocities, respectively. The biKappa distribution function given in Eq. (4) was introduced by Summers & Thorne (1991) to describe anisotropies of suprathermal populations, and it approaches a biMaxwellian as the spectral index κ (<3/2) reaches very large values κ → ∞.
Now we insert the distribution function in Eq. (3) into Eq. (1) and obtain the general dispersion relation of the RH transverse modes in a biKappa distributed plasma (7)We use the modified plasma dispersion function (Lazar et al. 2008a) (8)with the argument (a = e,p) (9)and the temperature anisotropy (10)In the limit of very large values of κ → ∞, the modified plasma dispersion function given in Eq. (8) converges to the standard dispersion function of Fried & Conte (1961), and the dispersion relation in Eq. (7) agrees exactly with the dispersion relation derived for a Maxwellian plasma (Gary 1993).
The newly modified dispersion function was introduced by Lazar et al. (2008a) to simplify the description of the dispersion properties of the transverse modes and instabilities in Kappa distributed plasmas. This function relates to the modified dispersion function Z_{κ} introduced by Summers & Thorne (1991) (11)We simply use the small and large argument expansions of Z_{κ} (Summers & Thorne 1991) to find for (12)(13)Each of the approximative forms given in Eqs. (12) and (13) of the modified dispersion function in Eq. (8) contains a principal part with an important contribution from the nonresonant particles, and an imaginary part given by the analytical continuation for the resonant particles with velocities satisfying cyclotron resonance conditions (of the first dominant order), i.e., g_{a} ≃ 1, a = e,p. Because the mechanism that excites the firehose instability is essentially nonresonant, we can describe the EFHI/PFHI only by considering a finite nonresonant contribution of the electrons/protons in the analytical approximations.
We can explicitly characterize the conditions for large or small arguments of by restricting ourselves to the lowest frequencies, ω_{r} < Ω_{p} ≪ Ω_{e}, corresponding to modes excited by the proton firehose instability, and further simplifying by considering two distinct cases:

(a)
ω_{i} < ω_{r} (<Ω_{p} ≪ Ω_{e}) when g_{e} ≷ 1 implies that kc/ω_{p,p} ≶ (1/α_{κe}) [m_{p}/(m_{e}β_{e,∥})] ^{1/2}, and g_{p} ≷ 1 implies . In the limit of a small ω_{r} < Ω_{p}, both arguments are large, g_{e} > 1 and g_{p} > 1, only for small wave numbers . Here, we introduced , a = e,p;

(b)
ω_{r} < ω_{i} (<Ω_{p} ≪ Ω_{e}), when g_{e} ≷ 1 implies the same kc/ω_{p,p} ≶ (1/α_{κe}) [m_{p}/(m_{e}β_{e,∥})] ^{1/2}, and g_{p} ≷ 1 implies . In the limit of a small ω_{i} < Ω_{p}, both arguments are large, g_{e} > 1 and g_{p} > 1, only for small wave numbers
The spectral domains where the approximations given in Eqs. (12) and (13) apply are displayed in Fig. 1a and b, in a dispersion frequency versus wave number diagram. Four regions are delimited by the resonance curves shown with dashed lines for protons and dotted lines for electrons: region R1 for g_{p,e} > 1, region R2 for g_{e} > 1 and g_{p} < 1, region R3 for g_{e,p} < 1, and, finally, region R4 for g_{e} < 1 and g_{p} > 1.
Fig. 1
Spectral domains R1–R4, where the approximations given in Eqs. (12) and (13) of the modified plasma dispersion function (8) can be used. For a dominance of suprathermal populations, indices κ_{a} → 1/2, and α_{κa} → 0 increasing (m_{e}α_{κe}β_{e,∥}/m_{p})^{−1/2} and (α_{κp}β_{p,∥})^{−1/2} to very large values, and also enlarging the area where the arguments g_{a} > 1 are large enough to apply the approximation in Eq. (13) for both species a = e,p, (W_{r,i} = ω_{r,i}/Ω_{p}, K = kc/ω_{p,p}). 

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The suprathermal populations are in general described by small values of the index κ → 3/2 in the distribution function in Eq. (3). In this case, α_{κa} → 0 also becomes very small causing the cutoffs of the resonance conditions and to reach very large values. The region R1, where g_{a} > 1 for both species a = e,p, can extend considerably to dominate the other regions, where the arguments are smaller ( g_{a} < 1). This is the first important result of the present paper proving that in Kappadistributed plasmas, the arguments of the modified dispersion function become sufficiently large, g_{a} > 1, for a large variety of plasma parameters, wave numbers, and frequencies, and that the approximation derived in Eq. (13) enables a simple analytical description of the unstable modes.
3. Proton firehose instability
Additional analytical derivations of the dispersion Eq. (7) can be easily undertaken to provide a detailed characterization of the PFHI for specific plasma regimes. Thus, it is obvious to consider either the limit of small temperatures (or small wavenumbers) when the argument of is large enough ( g_{a} ≫ 1) for the approximation in Eq. (13) to be applicable, or the opposite limit of large temperatures (or large wavenumbers) when the argument becomes small ( g_{a} ≪ 1) and the approximation in Eq. (12) applies.
3.1. Cold fluidlike plasma (small wave numbers)
In this limit, both arguments are supposed to be very large, i.e. g_{a} ≫ 1 (with a = e,p), and if we neglect the contribution of resonant particles, the modified plasma dispersion function in the approximative form given in Eq. (13) does not depend explicitly on the spectral index κ (cf. Paper I), and the dispersion relation (7) reduces to (14)We have assumed that for small wave numbers (real or imaginary) the frequencies are also sufficiently small, ω^{2} ≪ k^{2}c^{2} and ω ≪ Ω_{p} ≪ Ω_{e}. With β_{e,∥} = (T_{e,∥}/T_{p,∥})β_{p,∥}, we simply find that in the limit of very large κ → ∞ (when α_{κ} → 1), the dispersion relation in Eq. (14) agrees exactly with that derived by Pilipp & Völk (1971, see Eq. (3.3)) for a biMaxwellian plasma.
An instability is expected to occur for (15)i.e. when the dispersion relation in Eq. (14) admits purely growing solutions. This is the threshold condition of the firehose instability in the limit of small wave numbers or a sufficiently cold, fluidlike plasma model. In this limit, the two branches of LH and RH modes overlap, both being described by the same dispersion relation given in Eq. (14) and the same threshold condition in Eq. (15), and where the nonresonant character of this instability is most clearly revealed by cumulating the effects of both anisotropic components, electrons, and ions. Otherwise, if an instability is resonantly growing because of the kinetic anisotropies of the plasma particles (see, for instance, the cyclotron instabilities), the resonant enhancing effects from both species cannot cumulate. Parker (1958) demonstrated for the first time the existence of the firehose instability by considering a (onecomponent) fluid model of anisotropic plasma with an excess of pressure parallel to the magnetization field, and neglecting any resonances with plasma particles.
However, minimizing the role of collisions and assuming electrons and ions distributed after power laws of biKappa type, here we find that both the growth rate and the threshold condition are sensitive to the shape of the distribution function exhibiting a strong dependence on the spectral index κ. The standard fluidlike model of the firehose instability is, therefore, recovered only in the Maxwellian limit of κ → ∞, when the plasma must be collisional and less tenuous. The growth rates are displayed in Fig. 2 for different values of the κ index, the temperature contrast, T_{e,∥}/T_{p,∥}, and the plasmaβ parameter.
Fig. 2
Growth rates of the firehose instability as provided by Eq. (14) for κ_{e} = 2, κ_{p} = 3 (dotted line), κ_{e,p} = 4 (dashed line), κ_{e,p} → ∞ (solid line), and plasma parameters: T_{e,∥}/T_{e,⊥} = T_{p,∥}/T_{p,⊥} = 4, a) T_{e,∥}/T_{p,∥} = 3, β_{e,∥} = 18; and b) T_{e,∥}/T_{p,∥} = 2, β_{e,∥} = 8. For a given wavenumber value K = 0.03, the growth rate variation with κ_{e} and κ_{p} is shown in panel c). (W_{i} = ω_{i}/Ω_{p}, K = kc/ω_{p,p}). 

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When we compare the contributions of each species, electrons and protons, we find that the mass contrast m_{e}/m_{p} (or ) does not intervene (minimizing the contribution of the protons). It is, however, the temperature contrast T_{e,∥}/T_{p,∥} (<1, in the solar wind often in the favor of electrons) that can lower the effect of protons, e.g., through β_{p,∥} = (T_{p,∥}/T_{e,∥})β_{e, ∥} < β_{e,∥}. However, an important observation is that, in this limit (small wavenumbers), the effects of both species, electrons and protons, are diminished in the presence of suprathermal populations (small values of κ_{e,p}).
If the electrons are isotropic, i.e. A_{e} = 0, from the general condition in Eq. (15) we find the threshold condition for the PFHI (16)where must be sufficiently large. Alternatively, for isotropic protons, we substitute A_{p} = 0 in Eq. (15) and find the threshold condition for the EFHI (17)assuming this time a sufficiently large (for instance, Eq. (5) provides for κ = 2, and for κ = 4). We note that the reproduction of Eq. (17) here corrects a typographical error in Paper I, Eq. (22), where the threshold condition for the EFHI was derived for the first time. Both of these conditions in Eqs. (16) and (17) illustrate the need for a larger kinetic anisotropy and a larger β_{∥} to produce the instability in plasma with suprathermal populations. For comparison, the threshold conditions for a Maxwellian plasma (κ → ∞) and different lowκ plasmas are displayed in Fig. 3. We also note that in Fig. 2b no instability grows for small values of κ_{e} = 1.8 and κ_{p} = 2 because, for the given values of the plasma parameters, the instability condition imposes a minimum limit value for the spectral index κ (see Eq. (23) in Paper I).
When both species are anisotropic, i.e. A_{e,p} ≠ 0, and exhibit suprathermal tails of different shapes, (κ_{e} ≠ κ_{p}), the general condition in Eq. (15) can be rewritten in the same form as (18)assuming this time a sufficiently large .
Fig. 3
Threshold conditions for the EFHI (or the PFHI) as provided by Eq. (16) (or in Eq. (17)) for different values κ. The instability occurs below the threshold lines for , i.e., β_{∥} > 8 for κ = 2, β_{∥} > 3.2 for κ = 4, β_{∥} > 2.5 for κ = 8, and β_{∥} > 2 for κ → ∞. 

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3.2. Hot electrons – isotropic distribution, A_{e} = 0
Considering a plasma with anisotropic protons, T_{p,∥} > T_{p,⊥}, and isotropic electrons, T_{e,⊥} = T_{e,∥}, the dispersion relation in Eq. (7) simplifies to
(19)For Maxwellian distributions with the same assumption of anisotropic protons and isotropic electrons, the dispersion relation in Eq. (19) transforms, in the limit of κ → ∞, to (20)where Z(f) is the standard plasma dispersion function (Fried & Conte 1961) with the argument (21)If protons are still assumed to be cold (and nonresonant), the argument in Eq. (9) of the plasma dispersion function will be large, g_{p} > 1. Here, we assume that the electrons are hot so that the argument is g_{e} < 1, and they can resonate with RH modes. (The nonresonant effects of the electrons are discussed in the other sections and in Paper I). Limiting to the first order approximation of the modified plasma dispersion function in Eqs. (12) and (13), we obtain from Eq. (19) (22)where from Eq. (12) (23)Assuming ω^{2} ≪ k^{2}c^{2} and ω < Ω_{p} the dispersion Eq. (22) reduces further to (24)which admits unstable solutions of frequency (25)and growth rate (26)when the same threshold condition in Eq. (16) for the existence of the PFHI is fulfilled.
3.3. Hot electrons – anisotropic distribution, A_{e} ≠ 0
Two distinct cases are found here. First, if the electrons are anisotropic with a finite but sufficiently small anisotropy to describe an excess of parallel or perpendicular temperature, 0 < A_{e} < 1, the instability occurs for the same condition in Eq. (16) and has the same growth rate in Eq. (26), but only the frequency changes to (27)Second, if the electron anisotropy is larger, T_{e,∥} ≫ T_{e,⊥} but still in the limit of A_{e} ≲ 1, or if it is provided by a surplus of perpendicular temperature, T_{e,∥} ≪ T_{e,⊥} (A_{e} < 0), the wave solution will be described (in the same limit of a small ω < Ω_{p}) by the real frequency (28)and the imaginary frequency (29)The instability occurs only for A_{e} > 0, otherwise the wave is damped by the resonant electrons with T_{e,⊥} ≫ T_{e,∥} (A_{e} < 0). As expected in this case, if the instability occurs, it is exclusively driven by electrons (with a large excess of the parallel temperature, T_{e,⊥} ≪ T_{e,∥}), and it can change into an EFHI mode if the A_{p} is small enough to switch the wave polarization, i.e. the sign of the wave frequency in Eq. (28). Thus, Eq. (29) describes analytically the negativeslope branch of the EFHI growth rate displayed in Paper I, Fig. 1b: after a maximum at the saturation, the growth rate decreases and does not vanish completely, but decreases asymptotically to zero.
The instability of the RH modes can also be enhanced by the resonant protons (i.e. with a contribution from the imaginary residual part of the approximations in Eqs. (12) or (13)) producing ion (proton) cyclotron modes (Xue et al. 1993; Dasso et al. 2003), but this is possible only in smallβ plasmas, and is not considered here.
3.4. Hot plasma (large wave numbers)
If both components, electrons and protons, are sufficiently hot, both arguments are small enough, i.e. g_{e,p} ≪ 1 (region R3 in Fig. 1), and we use the approximation given in Eq. (12) for the modified plasma dispersion function. Keeping only the principal part in Eq. (12), we found no instability driven by the nonresonant particles. Some possible contribution from the resonant electrons in this case, is irrelevant for the firehose instability. The conclusion is that in this limit, the number of the nonresonant protons is not large enough to produce an instability of the firehose type. For electrons colder than protons, which is not the case in the solar wind plasma, the RH mode is damped (ω_{i} < 0).
4. The exact numerical solutions of Eq. (7)
Fig. 4
The exact numerical solutions, the real frequency a) and the growth rate b), c), d) for the PFHI as provided by Eq. (7) for κ_{p} = 3 (dotted line), κ_{p} = 4 (dashed line), κ_{p} = 8 (longdashed line), and κ_{p} → ∞ (solid line), and typical solar wind plasma parameters T_{e,∥}/T_{p,∥} = 2, β_{e,∥} = 8, (β_{p,∥} = 4), T_{e,⊥} = T_{e,∥} ≃ 10^{6} K and different values of the proton anisotropy T_{p,⊥}/T_{p,∥} = 0.25 a), b), 0.6 c), 0.8 d). Electrons are assumed to be isotropic and Maxwellian (κ_{e} → ∞). (W_{r} = ω_{r}/Ω_{p}, W_{i} = ω_{i}/Ω_{p}, K = kc/ω_{p,p}). 

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In Figs. 4–6 we plot the exact numerical solutions of Eq. (7), the real frequency W_{r} = ω_{r}/Ω_{p}, and the growth rate W_{i} = ω_{i}/Ω_{p}, and examine the influence that the Kappa index value can have on the evolution of the PFHI in different plasma regimes. Values of the plasma parameters including temperature anisotropy, are chosen from the insitu measurements of the solar wind missions.
The three distinct cases displayed in Fig. 4 correspond to different proton anisotropies T_{p,⊥}/T_{p,∥} = 0.25 (in panels a and b), 0.6 (c), 0.8 (d). The electrons are assumed to be isotropic (A_{e} = 0), and Maxwellian (κ_{e} → ∞). For comparison, the growth rates are calculated for different values of the spectral index, and their evolution depends markedly on the value of the proton anisotropy. At large anisotropies (panel b), the growth rate increases with κ_{p} reaching its maximum for Maxwellian (κ_{p} → ∞), but this tendency is restrained by decreasing the anisotropy, and for small anisotropies the growth rates show an opposite trend of variation, decreasing with κ_{p} index. If the instability suppression for small values of κ_{p} was anticipated by the more stringent threshold conditions found in Eq. (16) (and displayed in Fig. 3), the enhancement of the instability in the presence of Kappa populations with small anisotropies was unexpected. This new evolution seems to correspond to different threshold conditions that can eventually be obtained for an argument of the plasma dispersion function close to unity ( g ~ 1). However, in the observations there is no constraint for such small anisotropies, and they are probably irrelevant. The real (oscillatory) frequency (panel a) does not change significantly with κ_{p} index in the range of unstable wave numbers. Comparing to the growth rates of the EFHI in Paper I, the maxima reached by the growth rate of the PFHI are in general lower. This also remains true for larger proton anisotropies, e.g. T_{p,∥}/T_{p,⊥} = 20, similar to that used for electrons in Paper I. However, when assuming both components, electrons and protons, to be anisotropic, the evolution of the PFHI changes significantly.
Thus, an excess of the electron temperature perpendicular to the magnetic field, T_{e,⊥}/T_{e,∥} > 1, is expected to enhance the RH polarized mode. This indeed happens, as shown in Fig. 5, but only for large wave numbers when the instability turns into the whistler instability, which is driven by electrons and is, in general, inhibited by the Kappa distributions (Lazar et al. 2008b). At small wave numbers, the PFHI is suppressed by the same anisotropy of electrons, and both the growth rate and the unstable wave numbers interval are reduced. In Kappa distributed plasmas, growth rates are further reduced (at small values of the κ index) if the electron anisotropy is sufficiently small (Fig. 5a). However, for a somewhat larger anisotropy, e.g., T_{e,⊥}/T_{e,∥} = 1.5 (Fig. 5b), the evolution with κ changes again and the instability is enhanced at small values of κ. In this case, the enhancement of the PFHI occurs instead, for common values of the proton temperature anisotropy, e.g., T_{p,⊥}/T_{p,∥} = 0.25, where the instability seems to be very effective in the observations. Moreover, the enhanced growth rates of the PFHI evolve smoothly into the whistler instability, clearly illustrating that these anisotropic distributions of biKappa type tend to be highly unstable for a broadband of electromagnetic excitations.
Fig. 5
Growth rates for the PFHI and the whistler instability (WI) as provided by Eq. (7) for T_{e,∥}/T_{p,∥} = 2, β_{e,∥} = 8, (β_{p,∥} = 4), T_{e,∥} ≃ 10^{6} K, T_{p,⊥}/T_{p,∥} = 0.25, and electrons with a small anisotropy T_{e,⊥}/T_{e,∥} = 1.2 a), 1.5 b). (W_{i} = ω_{i}/Ω_{p}, K = kc/ω_{p,p}). 

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In the opposite case, when the electrons are hotter along the magnetic field direction, the EFHI is also expected to grow and compete with the PFHI (see Fig. 6). These instabilities interplay with each other and produce two maxima in the wave spectrum (see Fig. 6, panels b, c, and d)^{1}. The PFHI grows at smaller wave numbers, and because the two peaks lie within a narrow wavenumber interval they can overlap if plasma conditions are favorable to only one of these instabilities. Three situations displayed in Fig. 6 are representative of the case where these growing modes produce two distinct maxima. We keep the electron anisotropy fixed (T_{e,⊥}/T_{e,∥} = 0.5) and vary the proton anisotropy. At small deviations from isotropy (T_{p,⊥}/T_{p,∥} = 0.8), the EFHI instability is usually much faster than the PFHI (panel c). Large anisotropies enhance the PFHI that becomes competitive (panel b), or even faster than the EFHI (panel d). In Kappadistributed plasma, the tendency is the same, and the growth rates are diminished and restrained to small wave numbers because, in this case, the EFHI is suppressed much faster for decreasing values of κ_{e,p}. Towards the smallest values of κ_{e,p}, as illustrated, for instance, for the growth rates corresponding to κ_{e} = 2 and κ_{p} = 3 in panels b, c, and d, the EFHI is absent and the PFHI is only slightly inhibited.
These two instabilities have magnetic helicity of opposite sign (RH for the PFHI and LH for the EFHI) and this can help us to discriminate between the peaks, or to decide on their nature when they overlap. Changing of the sign of the oscillatory frequency (and the polarization) occurs exactly at the local minimum of the growth rate, when the PFHI mode shifts to the EFHI mode. This is clearly shown in Fig. 3, panels a and b. At small values of κ_{e,p} (e.g., κ_{e} = 2 and κ_{p} = 3), the frequency does not change sign because the PFHI is dominant and the EFHI is suppressed.
Fig. 6
The exact numerical solutions, the real frequency a), and the growth rate b), c), d) for the PFHI (small wavenumbers) and the EFHI (large wavenumbers) as provided by Eq. (7) for different indices κ_{e,p}, and typical solar wind plasma parameters T_{e,∥}/T_{p,∥} = 2, β_{e,∥} = 4, (β_{p,∥} = 2), T_{e,∥} ≃ 10^{6} K and different anisotropies T_{e,⊥}/T_{e,∥} = 0.5, T_{p,⊥}/T_{p,∥} = 0.8 a), b), 0.4 c), 0.2 d). (W_{r} = ω_{r}/Ω_{p}, W_{i} = ω_{i}/Ω_{p}, K = kc/ω_{p,p}). 

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5. Conclusions
We have studied the influence of suprathermal populations on the dispersion properties of the PFHI. The excess of parallel kinetic energy (T_{p,∥} > T_{p,⊥}) has been modeled with an anisotropic power law distribution of biKappatype.
In Sect. 2, we have derived the general dispersion relation of the RH transverse modes in terms of the modified plasma dispersion function for Kappa distributions. In the limits of both large or small arguments, this function admits approximative analytical forms, that allows us to identify the resonant and nonresonant contributions of the plasma particles. These limits have been explicitly described showing that in a Kappadistributed plasma, the argument of the new plasma dispersion function becomes larger than unity for a large variety of plasma parameters, wave numbers, and frequencies. Thus, the approximation of the modified dispersion function given in Eq. (13) enables a simple analytical description of the unstable solutions.
Different plasma conditions favorable to an analytical description of the PFHI have been identified in Sect. 3. First, we have derived the threshold conditions, which become more stringent in Kappadistributed plasmas: the PFHI requires a larger anisotropy and a larger plasmaβ parameter to grow. To shape suprathermal distribution functions susceptible of producing the unstable fluctuations measured in solar wind, we have to determine values of the κ_{e,p} index satisfying the same condition in Eq. (15). Secondly, we have shown that even in the limit of small wave numbers the growth rates are sensitive to the form of the distribution function: growth rates decrease for low values of the κ index. The standard fluidlike model of the firehose instability is, therefore, recovered only in the Maxwellian limit of κ → ∞.
In Sect. 4, we have examined the exact numerical solutions of the PFHI. If the electrons are isotropic their effect is unimportant, but the influence of suprathermal populations depends on how large the proton anisotropy is. Thus, at large anisotropies the instability is enhanced with κ_{p} reaching a maximum for a Maxwellian (κ_{p} → ∞), but this tendency is restrained by decreasing the anisotropy, and for small anisotropies the growth rates decrease with κ_{p}.
The influence of suprathermal populations also depends on the electron anisotropy. If the electrons exhibit an excess of perpendicular temperature (T_{e,⊥} > T_{e,∥}), the PFHI growth rates are enhanced by the suprathermal populations (at small values of κ_{e,p}) leading to a smooth transition into the whistler instability at high growth rates. In the opposite case, when the electrons are hotter along the magnetic field direction (T_{e,⊥} < T_{e,∥}), both plasma components drive the firehose instability, the PFHI instability at small wave numbers and the EFHI at larger wave numbers. The growth rate dispersion curve exhibits two peaks of maximum, that can be distinct (Fig. 6), or can overlap when the conditions are favorable to only one of these instabilities. The advantage is that these two instabilities have magnetic helicity of opposite sign that can eventually discriminate the origin of the peaks. Within Kappa distributions, the tendency is the same, the growth rates being reduced and restrained to small wave numbers because the EFHI is suppressed much faster with decreasing κ_{e,p}.
The new properties of the PFHI presented here are expected to provide closer agreement with measured data in the solar flares dominated by the suprathermal populations. If we consider the magnetic fluctuations measured near 1 AU in the solar wind (Bale et al. 2009), the data distribution corresponding to the magnetic fluctuation power is sharply peaked in a bandwith kρ_{p} ≃ 0.56 ± 0.32, where ρ_{p} = v_{p,th, ⊥ }/Ω_{p} is the thermal proton gyroradius. Relating to our wave number scaled by the proton inertial length (30)and assuming the solar wind plasma conditions adopted in Fig. 4, e.g., A_{p} = 3/4 and β_{p,∥} = 4, the measured fluctuations eventually generated by the PFHI must fall into a bandwith K = 0.24−0.88 that seems to be relevant for the branch of increasing (positive slope) growth rates displayed in Figs. 4–6. We should, however, remember that these magnetic fluctuations are frequently attributed to the oblique firehose instability that develops in the same conditions (T_{∥} > T_{⊥}), and seems to be faster (Hellinger et al. 2006) than the parallel firehose. Because a kinetic analytical treatment in two (or three) dimensions is still a difficult task, here we have limited the study by considering only the parallel propagation that must, however, retain the new features of this instability in Kappadistributed plasmas. Thus, the general trend of the instability thresholds moving to larger values of β_{∥} (in Fig. 3) seems to agree with observations in the solar wind.
Acknowledgments
We are grateful to the anonymous referee for his insightful comments and suggestions. The authors acknowledge financial support from the Research Foundation Flanders – FWO Belgium, the Katholieke Universiteit Leuven, and by the Deutsche Forschungsgemeinschaft (DFG), grant Schl 201/211. These results were obtained in the framework of the projects GOA/2009009 (K.U. Leuven), G.0729.11 (FWOVlaanderen) and C 90205 (ESA Prodex 10). Financial support by the European Commission through the SOLAIRE Network (MTRNCT2006035484) is gratefully acknowledged. The numerical results were obtained on the HPC cluster VIC of the K.U. Leuven.
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All Figures
Fig. 1
Spectral domains R1–R4, where the approximations given in Eqs. (12) and (13) of the modified plasma dispersion function (8) can be used. For a dominance of suprathermal populations, indices κ_{a} → 1/2, and α_{κa} → 0 increasing (m_{e}α_{κe}β_{e,∥}/m_{p})^{−1/2} and (α_{κp}β_{p,∥})^{−1/2} to very large values, and also enlarging the area where the arguments g_{a} > 1 are large enough to apply the approximation in Eq. (13) for both species a = e,p, (W_{r,i} = ω_{r,i}/Ω_{p}, K = kc/ω_{p,p}). 

Open with DEXTER  
In the text 
Fig. 2
Growth rates of the firehose instability as provided by Eq. (14) for κ_{e} = 2, κ_{p} = 3 (dotted line), κ_{e,p} = 4 (dashed line), κ_{e,p} → ∞ (solid line), and plasma parameters: T_{e,∥}/T_{e,⊥} = T_{p,∥}/T_{p,⊥} = 4, a) T_{e,∥}/T_{p,∥} = 3, β_{e,∥} = 18; and b) T_{e,∥}/T_{p,∥} = 2, β_{e,∥} = 8. For a given wavenumber value K = 0.03, the growth rate variation with κ_{e} and κ_{p} is shown in panel c). (W_{i} = ω_{i}/Ω_{p}, K = kc/ω_{p,p}). 

Open with DEXTER  
In the text 
Fig. 3
Threshold conditions for the EFHI (or the PFHI) as provided by Eq. (16) (or in Eq. (17)) for different values κ. The instability occurs below the threshold lines for , i.e., β_{∥} > 8 for κ = 2, β_{∥} > 3.2 for κ = 4, β_{∥} > 2.5 for κ = 8, and β_{∥} > 2 for κ → ∞. 

Open with DEXTER  
In the text 
Fig. 4
The exact numerical solutions, the real frequency a) and the growth rate b), c), d) for the PFHI as provided by Eq. (7) for κ_{p} = 3 (dotted line), κ_{p} = 4 (dashed line), κ_{p} = 8 (longdashed line), and κ_{p} → ∞ (solid line), and typical solar wind plasma parameters T_{e,∥}/T_{p,∥} = 2, β_{e,∥} = 8, (β_{p,∥} = 4), T_{e,⊥} = T_{e,∥} ≃ 10^{6} K and different values of the proton anisotropy T_{p,⊥}/T_{p,∥} = 0.25 a), b), 0.6 c), 0.8 d). Electrons are assumed to be isotropic and Maxwellian (κ_{e} → ∞). (W_{r} = ω_{r}/Ω_{p}, W_{i} = ω_{i}/Ω_{p}, K = kc/ω_{p,p}). 

Open with DEXTER  
In the text 
Fig. 5
Growth rates for the PFHI and the whistler instability (WI) as provided by Eq. (7) for T_{e,∥}/T_{p,∥} = 2, β_{e,∥} = 8, (β_{p,∥} = 4), T_{e,∥} ≃ 10^{6} K, T_{p,⊥}/T_{p,∥} = 0.25, and electrons with a small anisotropy T_{e,⊥}/T_{e,∥} = 1.2 a), 1.5 b). (W_{i} = ω_{i}/Ω_{p}, K = kc/ω_{p,p}). 

Open with DEXTER  
In the text 
Fig. 6
The exact numerical solutions, the real frequency a), and the growth rate b), c), d) for the PFHI (small wavenumbers) and the EFHI (large wavenumbers) as provided by Eq. (7) for different indices κ_{e,p}, and typical solar wind plasma parameters T_{e,∥}/T_{p,∥} = 2, β_{e,∥} = 4, (β_{p,∥} = 2), T_{e,∥} ≃ 10^{6} K and different anisotropies T_{e,⊥}/T_{e,∥} = 0.5, T_{p,⊥}/T_{p,∥} = 0.8 a), b), 0.4 c), 0.2 d). (W_{r} = ω_{r}/Ω_{p}, W_{i} = ω_{i}/Ω_{p}, K = kc/ω_{p,p}). 

Open with DEXTER  
In the text 
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