Issue 
A&A
Volume 573, January 2015



Article Number  A79  
Number of page(s)  12  
Section  The Sun  
DOI  https://doi.org/10.1051/00046361/201423930  
Published online  22 December 2014 
Overdamped Alfvén waves due to ionneutral collisions in the solar chromosphere
^{1} Departament de Física, Universitat de les Illes Balears, 07122 Palma de Mallorca, Spain
email: roberto.soler@uib.es; joseluis.ballester@uib.es
^{2} Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, 8042 Graz, Austria
email: teimuraz.zaqarashvili@oeaw.ac.at
^{3} Abastumani Astrophysical Observatory at Ilia State University, 3/5 Cholokashvili Avenue, 0162 Tbilisi, Georgia
Received: 2 April 2014
Accepted: 12 November 2014
Alfvénic waves are ubiquitous in the solar atmosphere and their dissipation may play an important role in atmospheric heating. In the partially ionized solar chromosphere, collisions between ions and neutrals are an efficient dissipative mechanism for Alfvén waves with frequencies near the ionneutral collision frequency. The collision frequency is proportional to the ionneutral collision cross section for momentum transfer. Here, we investigate Alfvén wave damping as a function of height in a simplified chromospheric model and compare the results for two sets of collision cross sections, namely those of the classic hardsphere model and those based on recent quantummechanical computations. We find important differences between the results for the two sets of cross sections. There is a critical interval of wavelengths for which impulsively excited Alfvén waves are overdamped as a result of the strong ionneutral dissipation. The critical wavelengths are in the range from 1 km to 50 km for the hardsphere cross sections, and from 1 m to 1 km for the quantummechanical cross sections. Equivalently, for periodically driven Alfvén waves there is an optimal frequency for which the damping is most effective. The optimal frequency varies from 1 Hz to 10^{2} Hz for the hardsphere cross sections, and from 10^{2} Hz to 10^{4} Hz for the quantummechanical cross sections. Future observations at sufficiently high spatial or temporal resolution may show the importance of highfrequency Alfvén waves for chromospheric heating. For instance, the Atacama Large Millimeter/submillimeter Array (ALMA) may be able to detect the critical wavelengths and optimal frequencies and so to test the effective collision cross section in the chromospheric plasma.
Key words: magnetohydrodynamics (MHD) / Sun: atmosphere / Sun: chromosphere / Sun: oscillations / waves
© ESO, 2014
1. Introduction
Recent highresolution observations indicate that Alfvén waves are ubiquitous throughout the solar atmosphere. In particular, Alfvénic waves have been detected propagating in the chromosphere (e.g., Kukhianidze et al. 2006; Zaqarashvili et al. 2007; De Pontieu et al. 2007; Okamoto & De Pontieu 2011; Kuridze et al. 2012; De Pontieu et al. 2012; Morton et al. 2013; Morton 2014). It is believed that energy transport by Alfvénictype waves and its dissipation may play a relevant role in the heating and energy balance in the atmospheric plasma (see, e.g., Erdélyi & Fedun 2007; Cargill & de Moortel 2011; McIntosh et al. 2011; Hahn & Savin 2014). Both observations and theoretical aspects of Alfvén wave propagation have been reviewed by Zaqarashvili & Erdélyi (2009) and Mathioudakis et al. (2013).
The relatively cool temperature in the chromosphere causes the plasma to be partially ionized, with a predominance of neutrals at low heights in the chromosphere. In this context, ionneutral collisions have been invoked as a viable energy dissipation mechanism for Alfvén waves by, e.g., De Pontieu et al. (2001); Khodachenko et al. (2004); Leake et al. (2005); Russell & Fletcher (2013), among others. Estimations of the heating rate due to Alfvén waves damped by ionneutral collisions computed by Song & Vasyliūnas (2011) and Goodman (2011) indicate that this mechanism can generate sufficient heat to compensate the radiative losses at low altitudes in the solar atmosphere. For driven waves propagating from the photosphere to the corona, numerical simulations by Tu & Song (2013) show that the wave energy flux transmitted to the corona is at least one order of magnitude smaller than that of the driving source due to the reflection and strong damping in the chromosphere. Therefore, partial ionization seems to be a crucial ingredient to correctly understand the processes of plasma heating and energy transport in the chromosphere (e.g., Khomenko & Collados 2012; MartínezSykora et al. 2012; Leake et al. 2013), including those processes that involve propagation and dissipation of Alfvén waves.
Damping of Alfvén waves due to ionneutral collisions in the solar chromosphere is usually investigated in the singlefluid approximation, which assumes a strong coupling between the various species in the plasma (e.g., De Pontieu et al. 2001; Khodachenko et al. 2004). Theoretical studies demonstrate that the damping is most efficient when the frequency of the wave and the ionneutral collision frequency are of the same order of magnitude (see Zaqarashvili et al. 2011b; Soler et al. 2013b). However, the singlefluid approximation breaks down for wave frequencies near the ionneutral collision frequency because the dynamics of ions and neutrals decouple. Ions and neutrals have to be considered as two separate fluids for those high frequencies. Multifluid approaches are therefore necessary to correctly investigate highfrequency Alfvén waves in the chromosphere (Zaqarashvili et al. 2011b; Soler et al. 2013b,a,c). In a general sense, both temporal and spatial scales should be taken into account to assess the applicability of the singlefluid approximation. For the waves of interest in this paper, however, it is enough to consider the criterion based on the wave frequency alone, since frequencies and wavelengths are intrinsically related. High frequencies are equivalent to short wavelengths, and vice versa.
The present paper deals with the theoretical study of Alfvén wave damping in the partially ionized chromosphere using the multifluid theory. The multifluid equations used here are rather general and contain a number of physical effects that were not considered in previous works (e.g., Soler et al. 2013b). For instance, we consistently take into account ionneutral collisions, electronneutral collisions, electron inertia, viscosity, Ohm’s magnetic diffusion, and Hall’s current. This additional physics provides a more realistic representation of the chromospheric plasma. This investigation is also related to the recent work by Vranjes & Kono (2014) although, as we explain later, our results and those of Vranjes & Kono (2014) do not agree regarding the existence of a strict frequency cutoff for Alfvén waves.
The three main goals of this work are summarized as follows. (1) We discuss a fact usually ignored in the literature concerning the applicability of the multifluid theory. The correct study of waves with frequencies near the ionneutral collision frequency cannot be done in the usual framework of the multifluid theory in the low chromosphere (see Vranjes & Krstic 2013). Fluid theory is only applicable at sufficiently large heights (see Sect. 2 for details). (2) We show that the ionneutral collision cross section is a very important parameter for determining the wavelengths and wave frequencies that are most efficiently damped. Different values of the ionneutral collision cross section and frequency can be found in the literature (see, e.g., the various expressions of the collision frequency given in the Appendix of De Pontieu et al. 2001). An important goal of the present work is to determine whether the use of the more accurate cross sections recently proposed by Vranjes & Krstic (2013) modifies substantially the results obtained with the classical cross sections or, on the contrary, the numerical value of the cross sections plays a minor role. (3) In connection to the previous point, we suggest that future observations with instruments operating at very high temporal and spatial resolutions like, e.g., the Atacama Large Millimeter/submillimeter Array (ALMA), may be crucial to understand how these waves actually propagate and damp in the chromosphere and thus how they contribute to plasma heating (see Karlický et al. 2011).
This paper is organized as follows. Section 2 contains the description of the chromospheric model adopted in this work. Discussions about the applicability of the fluid theory and the importance of the ionneutral collision cross section are also given. The basic multifluid equations and the dispersion relation of Alfvén waves are given in Sect. 3. Then, Sect. 4 contains computations of the quality factor for Alfvén wave damping as a function of height in the chromosphere. Both the impusive driver and the periodic driver scenarios are analyzed. Finally, the discussion of the results and their observational implications are included in Sect. 5.
Fig. 1 Dependence on height above the solar photosphere of the a) plasma temperature and b) hydrogen ionization fraction, χ = ρ_{n}/ρ_{i}, according to the FAL93F model. c) Magnetic field strength as a function of height according to the semiempirical relation of Eq. (1). We note the logarithmic scale in the vertical axis of panel b). 

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2. Chromospheric model
2.1. Variation with height of physical parameters
In this work, we adopt a simplified onedimensional model for the chromosphere. We treat the chromospheric medium as a partially ionized hydrogen plasma composed of ions (protons), electrons, and neutrals (hydrogen atoms). The influence of heavier species, specially that of helium, is ignored. The specific effect of helium on the damping of Alfvén waves was studied by Soler et al. (2010) and Zaqarashvili et al. (2011a, 2013). The reader is refereed to these previous works for details. The subscripts “i”, “e”, and “n” denote ions, electrons, and neutrals, respectively, while the subscript “β” is used to refer to a unspecified species. MKS units are used throughout this paper.
We use the chromospheric bright region model F of Fontenla et al. (1993), hereafter the FAL93F model, to account for the variation of the physical conditions with height, that here corresponds to the zdirection in Cartesian coordinates. Figures 1a and b show the dependence on height above the photosphere, h, of the plasma temperature, T, and the ionization fraction, χ = ρ_{n}/ρ_{i}, where ρ_{i} and ρ_{n} are the ion and neutral densities, respectively. The photosphere corresponds to h = 0. The plasma is permeated by a vertical magnetic field, namely B = Bê_{z}, with B the magnetic field strength. The dependence of the magnetic field strength on height is taken after the semiempirical formula by Leake & Arber (2006), namely (1)where ρ is the total mass density, whose dependence on height is prescribed by the FAL93F model, ρ_{ph} is the total density at the photospheric level (also taken from the FAL93F model), and B_{ph} is the photospheric magnetic field strength. Equation (1) roughly represents the magnetic field strength in an intense magnetic flux tube expanding with height. We consider an intense magnetic element at the photospheric level and use B_{ph} = 2 kG. Figure 1c shows the dependence on height of the magnetic field strength. In this model the magnetic field strength decreases with height and is B ≈ 190 G at 1000 km and B ≈ 35 G at 2000 km above the photosphere. The largest variation of B takes place for h ≲ 1000 km, that represents the strong expansion of the magnetic field at low heights in the chromosphere. On the contrary, for h ≳ 1000 km the variation of B is much less important and B becomes almost constant at large heights. We note that a horizontal component of the magnetic field should be included in order to satisfy the divergencefree condition. However, this geometrical effect would complicate matters substantially. For this reason, we restrict ourselves to a purely vertical magnetic field and neglect the horizontal component. This is approximately valid near the axis of the flux tube, where the horizontal component is much smaller than the vertical component.
It should be noted that the simplified model used here represents a static, gravitationally stratified chromosphere. Therefore, the model misses part of the highly dynamical behavior of the chromospheric medium seen in both highresolution observations and numerical simulations (e.g., MartínezSykora et al. 2012). A timedependent background is necessary to account for all the fast, timevarying dynamics of the chromospheric plasma. This is, however, far beyond the purpose of the present work.
2.2. Collision frequencies and applicability of the fluid theory
We use the threefluid theory for a partially ionized plasma, in which ions, electrons, and neutrals are considered as separate fluids. The three fluids exchange momentum by means of particle collisions. The collision frequency of species β with species β′, namely ν_{ββ′}, is defined by means of the symmetric friction coefficient α_{ββ′}, so that ν_{ββ′} = α_{ββ′}/m_{β}n_{β}, where m_{β} and n_{β} are the mass and number density of species β, respectively. The friction coefficient between two charged species, namely β and β′, is (e.g., Spitzer 1962; Braginskii 1965) (2)while the friction coefficient between a charged or neutral species, β, and a neutral species, n, is (e.g., Braginskii 1965; Chapman & Cowling 1970) (3)In these expressions, is the reduced mass, T_{β} is the temperature of species β, e is the electron charge, k_{B} is Boltzmann’s constant, ϵ_{0} is the permittivity of free space, Z_{β} is the sign of the electric charge (Z_{i} = 1 and Z_{e} = −1), σ_{βn} is the momentum transfer cross section for collisions involving neutrals, and lnΛ_{ββ′} is Coulomb’s logarithm given by (e.g., Spitzer 1962; Vranjes & Krstic 2013) (4)The expressions of the friction coefficients given above are also valid for selfcollisions, i.e., collisions between particles of the same species. If for simplicity we assume the same temperature for ions, electrons, and neutrals, i.e., T_{i} = T_{e} = T_{n}, and take into account that the number density of ions and electrons is the same in a hydrogen plasma to satisfy quasineutrality, i.e., n_{i} = n_{e}, we may drop the subscripts from the temperatures and from Coulomb’s logarithm. In addition, we can substitute the numerical values of the various constant parameters into the expression of Coulomb’s logarithm, so that it reduces to (e.g., Priest 1984) (5)We are interested in studying the damping of Alfvén waves in the chromosphere. Specifically, we are interested in the role of ionneutral collisions. It is known from previous works (e.g., Zaqarashvili et al. 2011b; Soler et al. 2013b) that the damping is most efficient when the wave frequency and the ionneutral collision frequency are of the same order. We are therefore interested in frequencies near the ionneutral collision frequency. It is important to known whether the fluid theory used here is applicable or breaks down for those wave frequencies. The fluid theory implicitly assumes that selfcollisions are frequent enough for fluid behavior to be established in the three fluids separately. This imposes a minimum value for the selfcollision frequency to keep the velocity distribution close to a MaxwellBoltzmann distribution. In other words, the selfcollision frequency of a particular species must be higher than the wave frequency and also higher than any of the collision frequencies with the other species.
The collision frequencies between charged species are essentially determined by the densities and the temperature (see Eq. (2)), while the collision frequencies involving neutrals also depend on the neutral collision cross section (see Eq. (3)). The classical approach to compute the collision cross section is the socalled model of hard spheres, from here on HS. In the HS model the particles are considered as solid spheres that interact by means of direct impacts only (e.g., Chapman & Cowling 1970). The HS cross section is usually computed as , where r_{β} and r_{β′} are the radii of particles β and β′, respectively. In the case of ionneutral and electronneutral collisions, the radii of both ions and electrons are much smaller than the radius of neutral atoms, so that their HS cross sections are approximately the same, namely σ_{in} ≈ σ_{en} ≈ 10^{20} m^{2}. Likewise, the HS cross section for neutralneutral collisions is σ_{nn} ≈ 4 × 10^{20} m^{2}.
Recently, Vranjes & Krstic (2013), from here on VK, presented quantummechanical computations of collision cross sections that include several important ingredients missing from the classic HS model. For instance, VK considered variations of the cross section with temperature, quantum indistinguishability corrections, and charge transfer. The VK cross sections coincide with the classical ones at high temperatures, but are different from the HS cross sections at low temperatures akin to those in the chromosphere. In their paper, VK plot the computed cross section as a function of the energy of the colliding species, which is related to the temperature. For chromospheric temperatures of interest here, we have to consider the results at low energies. The ionneutral collision cross section from Fig. 1 of VK is σ_{in} ≈ 10^{18} m^{2}, while the electronneutral collision cross section from their Fig. 4 is σ_{en} ≈ 3 × 10^{19} m^{2}. Concerning neutralneutral collisions, VK provide in their Fig. 3 different cross sections for momentum transfer and viscosity. The cross section for momentum transfer is σ_{nn} ≈ 10^{18} m^{2}, while the cross section for viscosity is σ_{nn} ≈ 3 × 10^{19} m^{2}. In summary, the VK cross sections are between one and two orders of magnitude larger than the classic HS cross sections.
Fig. 2 Dependence on height above the solar photosphere of the collision frequencies for a) ions, b) electrons, and c) neutrals. HS and VK denote collision frequencies with neutrals computed with the hard sphere cross sections and the Vranjes & Krstic (2013) cross sections, respectively. In panels a) and b), Ω_{i} and Ω_{e} denote the ion and electron cyclotron frequencies, respectively. 

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The value of the cross section is not only important from the academic point of view but also from the practical point of view. The reason is that the value of the cross section directly affects the collision frequency and, therefore, the cross section is important to determine both the applicability of the fluid theory and the optimal frequency for wave damping. Uncertainties in the collision frequency also cause uncertainties in the various transport coefficients that govern basic collisional phenomena in the plasma (e.g., MartínezSykora et al. 2012). The value of the collision cross section may play an important role in theoretical computations.
Figure 2 shows the dependence on height of the relevant collision frequencies for ions, electrons, and neutrals taking into account both HS and VK cross sections. Concerning ions (Fig. 2a), we find that ν_{in} ≫ ν_{ii} in the low chromosphere. Collisions with neutrals are too frequent for ions to reach a MaxwellBoltzmann distribution independently. In other words, ions collide too frequently with neutrals so that ionion collisions do not have enough time to make the ion distribution Maxwellian on their own without the influence of neutrals. Ions are too coupled with neutrals. This means that the condition for ions to be treated as an individual fluid is not satisfied. The multifluid theory breaks down for h ≲ 600 km using the HS cross sections and for h ≲ 900 km using the VK cross sections. We also see that ions would not be magnetized for h ≲ 700 km in the VK case since ν_{in}> Ω_{i} at those low heights, where Ω_{i} = eB/m_{i} is the ion cyclotron frequency (see a discussion on this issue in Vranjes et al. 2008). The dependence on height of the ion collision frequencies shown here could be compared to those plotted in VK. However, we note that the magnetic field model used here is different from that of VK. This causes our ion cyclotron frequency to be slightly larger than in VK. We also note that VK used the atmospheric model C of Fontenla et al. (1993), while here we use model F. This leads to a different dependence of the physical parameters (and so the collision frequencies) on height. Concerning magnetization, VK argue that the largest collision frequency of all the possible ones should be used to discuss magnetization. According to VK (see their Fig. 7), that collision frequency corresponds to the collision frequency for elastic scattering. However, we note that in Fig. 7 of VK the collision frequency for elastic scattering is only slightly larger than that for momentum transfer used here. The use of any of these two frequencies leads essentially to the same results concerning magnetization of ions.
In the case of electrons (Fig. 2b), we also see that electrons should not be treated as a separate fluid at low heights due to the very frequent collisions with neutrals, i.e., ν_{en} ≫ ν_{ee}. At large heights, however, it is found that ν_{ee} ≫ ν_{en} and ν_{ee} ~ ν_{ei}, so that electrons are strongly coupled to ions (they effectively behave as an ionelectron single fluid) but are weakly affected by neutrals. In all cases, the electron cyclotron frequency, Ω_{e} = eB/m_{e}, remains larger than the electronelectron collision frequency. As before, we could compare the electron frequencies computed here to those given in VK. We note again that both the magnetic field dependence on height and the atmospheric model are different in the present paper and in VK. This leads to variations in the physical parameters that may explain the small differences between our Fig. 2b and the corresponding graphs of VK.
Finally, the collision frequencies for neutrals (Fig. 2c) show that ν_{nn} is always the largest frequency at all heights, so that treating neutrals as a separate fluid is a valid assumption. This last result remains the same for both HS and VK cross sections.
The results discussed in the previous paragraphs indicate that for the wave frequencies of interest here, i.e., for wave frequencies near the ionneutral collision frequency, ions should not be considered as an individual fluid separate from neutrals at low heights in the chromosphere. This was previously noted by Vranjes & Krstic (2013). The same restriction applies to electrons. The fluid theory is applicable for h ≳ 600 km using the HS cross sections and for h ≳ 900 km using the VK cross sections. Hence, the use of the more accurate VK cross sections results in a more restrictive criterion for the applicability of the fluid theory than that obtained with the classical HS cross sections. The correct study of highfrequency waves in the low chromosphere should be done using hybrid fluidkinetic models, or even fully kinetic models, since standard fluid theory is not applicable for those highfrequencies. Here we consider sufficiently large heights in the chromosphere for the fluid theory to be applicable for the wave frequencies under study. Of course, for wave frequencies lower than all the collision frequencies the plasma dynamics can be studied using the singlefluid approximation (e.g., De Pontieu et al. 2001; Khodachenko et al. 2004), which assumes that ions, electrons, and neutrals are strongly coupled. However, here we are interested in higher frequencies beyond the range of applicability of the singlefluid approximation.
3. Basic equations
3.1. Threefluid model for the upper chromosphere
The general multifluid equations for a partially ionized plasma can be found in, e.g., Zaqarashvili et al. (2011b), Meier & Shumlak (2012), Khomenko et al. (2014) among others. Here, we restrict ourselves the linearized version of the equations, that govern the dynamics of small perturbations superimposed on the equilibrium state. This approach is appropriate to study Alfvén waves whose velocity amplitudes are much smaller than the Alfvén velocity in the plasma. Since Alfvén waves are strictly polarized in the plane perpendicular to the direction of the magnetic field, which is vertical in the present model, gravity has no effect on the perturbations. In addition, we restrict ourselves to values of the wavelength that are much shorter than the stratification scale height, and so we perform a local analysis of the perturbations. A limitation of the local analysis is that possible cutoff frequencies and reflection due to the background gravitational stratification are absent (see, e.g., Roberts 2006). This last issue was recently explored analytically by Zaqarashvili et al. (2013) and using numerical simulations by Tu & Song (2013). It is beyond the purpose of the present investigation to take into account the effects of gravitational cutoffs and wave reflection. The reason is that gravitational cutoff may affect waves with longer wavelengths than those studied here.
The linearized momentum equations of ions, electrons, and neutrals are where v_{β}, , , and ρ_{β} = m_{β}n_{β} are the velocity perturbation, scalar pressure perturbation, viscosity tensor, and mass density of species β, and E^{′} is the electric field perturbation. Since in the present paper we study incompressible Alfvén waves, Eqs. (6)−(8) are complemented with the incompressibility conditions for the three fluids, namely (9)For Alfvén waves the zcomponents of the velocity perturbations are zero, i.e., v_{i,z} = v_{e,z} = v_{n,z} = 0. This means that it is enough take the x and ycomponents of Eqs. (6)−(8). Although we include scalar pressure terms in the momentum equations for completeness, we note that these forces do not act on incompressible Alfvén waves and may be dropped. The terms with α_{in}, α_{ie} and α_{en} in Eqs. (6)–(8) account for the transfer of momentum between species due to particle collisions. Concerning viscosity, we take into account that the viscosity of a partially ionized plasma is determined essentially by ions and neutrals by virtue of their larger masses (see, e.g., Braginskii 1965; Meier & Shumlak 2012). Therefore, the electron viscosity is neglected compared to the ion and neutral viscosities. The ion viscosity tensor is a complicated expression usually described as the sum of five components accounting for compressive viscosity, shear viscosity, and gyroviscosity (see the full expression in Braginskii 1965). Keeping the spatial variations (derivatives) of the velocity along the direction of the magnetic field only, as appropriate for Alfvén waves, the x and ycomponents of the divergence of the ion viscosity tensor reduce to with ξ_{i, ⊥} and ξ_{i,g} the reduced coefficients of ion shear viscosity and gyroviscosity, respectively, which are adapted from Braginskii (1965), namely where is the ion thermal velocity. We note that the coefficient of ion compressive viscosity (see Braginskii 1965) does not play a role in Alfvén waves. The reason for this result is that Alfvén waves are incompressible and produce no velocity perturbations along the magnetic field direction. In the neutral fluid the form of the viscosity tensor is simpler because of the absence of the effect of the magnetic field. Thus, the divergence of the neutral viscosity tensor is (14)with ξ_{n} the isotropic coefficient of neutral viscosity given by (15)where is the neutral thermal velocity. Since m_{n} ≈ m_{i} for hydrogen, c_{T,i} ≈ c_{T,n} and so we can drop the subscript from the thermal velocity.
3.2. Reduction of the main equations
From here on we specialize in Alfvénic perturbations, and so we drop pressure perturbations. It is frequent in the literature to exclude the electric field perturbation, E^{′}, from the equations and to work with the magnetic field perturbation, B^{′}, instead. In that case, the induction equation governing the evolution of the magnetic field perturbation has to be obtained (see, e.g., Zaqarashvili et al. 2011b). It is also useful to manipulate the equations so that the electron velocity does not explicitly appear. To do so, we define the current density perturbation as (16)which is related to the magnetic field perturbation as (17)where μ is the magnetic permeability. These relations are used to express the electron velocity, v_{e}, as (18)where we used the quasineutrality condition n_{i} = n_{e}. This equation governs the electron dynamics and replaces their full momentum equation (Eq. (7)). In turn, Eqs. (6)–(8) and (18) can be conveniently combined to eliminate E^{′} and v_{e} from the ion and neutral momentum equations, namely where we approximated ρ_{i} + ρ_{e} ≈ ρ_{i}.
Next, the expression for the electric field perturbation, E^{′}, is obtained from Eq. (7), namely (21)Finally, we use the Maxwell Equation, (22)and arrive at the equation governing the evolution of the magnetic field perturbation, namely (23)Equation (23) is the linearized induction equation in a pressureless threefluid partially ionized plasma. The terms on the righthand side of Eq. (23) are the inductive term, Ohm’s magnetic diffusion, a term due to electron inertia, Hall’s current, and a term that mostly accounts for the effect of electronneutral collisions, respectively. We define the various coefficients in Eq. (23) as follows Ohm’s term and the term due to electronneutral collisions represent diffusion of the magnetic field due to collisions between particles. Hall’s current and the electron inertia term are not dissipative terms. The socalled Hall effect arises in a plasma when electrons are able to drift with the magnetic field but the much heavier ions are not completely frozen to the magnetic field. As a result, the current density vector has a component normal to the electric field vector (see, e.g., Priest 1984). Hall’s effect may be enhanced by electronneutral collisions, which tend to further decouple ions and electrons (Pandey & Wardle 2008).
3.3. Dispersion relation and the quality factor
To obtain the dispersion relation of Alfvén waves, we take into account that any disturbance in the plasma can be expressed as a superposition of its Fourier modes and, for linear waves, it is enough studying the behavior of the Fourier modes separately. Thus, we put all perturbations proportional to exp(ikz − iωt), where k is the wavenumber along the magnetic field direction, and ω is the angular frequency. The wavelength, λ, and the wave frequency, f, are related to these two parameters as λ = 2π/k and f = ω/ 2π.
Equations (19), (20) and (23) define an eigenvalue problem where the x and ycomponents of v_{i}, v_{n}, and B^{′} form the eigenvector, and either ω or k is the eigenvalue. The zcomponents of v_{i}, v_{n}, and B^{′} are zero for Alfvén waves. The eigenvalue is the solution of the dispersion equation that relates the frequency to the wavenumber. The dispersion relation is here expressed as a 6 × 6 determinant, namely (28)with We consider the paradigmatic case that the effects of partial ionization, viscosity, Ohm’s diffusion, and Hall’s current are all dropped from the dispersion relation. In that case, the dispersion relation reduces to a 2 × 2 determinant, namely (34)whose solutions are the wellknown ideal linearly polarized Alfvén waves in a fully ionized plasma, namely (35)where is the ion Alfvén velocity, and the + and − signs stand for forward and backward propagating waves, respectively. The ideal Alfvén waves are modified when nonideal mechanisms are taken into account.
Alfvén waves efficiently transport energy in magnetized plasmas. Due to the presence of dissipation mechanisms, wave energy can be deposited in the plasma. For instance, ion shear viscosity, neutral isotropic viscosity, collisions, and Ohm’s diffusion are dissipation mechanisms that produce the damping of the waves. Hall’s current and ion gyroviscosity, however, do not produce dissipation but dispersion. Hall’s current and gyroviscosity are able to break the symmetry between the two possible circular polarizations of the electric field, namely left and right circular polarizations (see, e.g., Zhelyazkov et al. 1996; Cramer 2001), which increases the number of different waves that can propagate in the plasma. Formally, a linearly polarized Alfvén wave can be written as a sum of a left circularly polarized wave and a right circularly polarized wave, with the implicit assumption that both waves have the same frequency (see, e.g., Pécseli 2013). When the two circular polarizations have different frequencies a pure linearly polarized Alfvén wave cannot be formed, and so the two waves with opposite circular polarization appear as different solutions of the dispersion relation.
The dispersion relation (Eq. (28)) applies to both the spatial and the temporal regimes, depending on whether ω or k is prescribed. On the one hand, the solutions in the temporal regime can be related to the impulsively driven or initialvalue problem, in which the waves are excited by an impulsive driver of short duration that generate local perturbations in the plasma with a certain spatial extent. In the temporal regime the wavenumber, k, is a prescribed real quantity and the angular frequency, ω, is obtained from the dispersion relation. Due to the presence of dissipation mechanisms the waves are damped in time. Temporal damping is mathematically represented by the fact that ω is complex. The real part of ω is related to the oscillatory behavior of the wave, i.e., the period. In turn, the imaginary part of ω corresponds to the temporal damping rate. On the other hand, the solutions in the spatial regime can be linked to the periodically driven or boundaryvalue problem, in which the waves are excited by a periodic driver with a certain frequency. In the spatial regime ω is a prescribed real quantity and k is the complex solution of the dispersion relation. In this case, the real part of k is related to the actual wavelength and the imaginary part of k corresponds to the spatial damping length.
The quality factor, Q, is a dimensionless parameter that characterizes how efficiently damped a wave is. In the case of temporal damping for a prescribed k, the standard definition of the quality factor is (36)The quality factor compares the frequency at which a wave oscillates to the rate at which it damps. Equivalently, in the case of spatial damping for a prescribed ω, the quality factor is (37)so that Q compares the wavelength with the damping length. The behavior of the waves depends on the value of Q. When Q> 1/2 perturbations are underdamped, meaning that the perturbations oscillate while their amplitude decrease in time or space. Most of the energy of the perturbations can propagate away as weakly damped Alfvén waves. The larger Q, the weaker the damping and so the farther the wave can propagate from the excitation location until all the wave energy is dissipated in the plasma. If Q → ∞, the wave is undamped and no energy dissipation takes place. Conversely, when Q< 1/2 the dissipation is very strong and the perturbation is overdamped. Most of the energy stored in the perturbation is dissipated in situ instead of being transported away in the form of a propagating Alfvén wave. The case Q = 1/2 that separates the two regimes is often called critical damping. The most extreme situation, however, takes place when Q = 0. In such a case, the wave has a socalled cutoff. In a cutoff scenario, perturbations are evanescent in time or space instead of oscillatory and therefore Alfvén waves cannot propagate at all. The remainder of this paper is devoted to investigating the quality factor of Alfvén waves in the solar chromosphere.
Fig. 3 Contour plots of the quality factor Q (in logarithmic scale) of impulsively driven Alfvén waves in the upper solar chromosphere as function of the wavelength λ (vertical axis in logarithmic scale) and height above the photosphere (horizontal axis). Top and botton panels correspond to the left and right polarized waves, respectively. Left and right panels are the results obtained using the hardsphere cross sections (HS) and the Vranjes & Krstic (2013) cross sections (VK), respectively. The red dotted lines enclose zones where Alfvén waves are overdamped, i.e., Q< 1/2. The white dashed lines correspond to the approximate critical wavelengths given in Eqs. (39) and (40). We note that the VK results are only strictly valid for heights larger than 900 km. 

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4. Alfvén wave damping in the upper chromosphere
4.1. Impulsive driver
We start by investigating the case of Alfvén waves excited by an impulsive driver. Hence, the temporal damping of the waves for a fixed wavelength is explored. The dispersion relation is solved to obtain the complex wave frequency, and so the quality factor, as a function of height. The dispersion relation has six solutions for the frequency. Four solutions correspond to forward and backward, left and right circularly polarized Alfvén waves, while the two remaining solution are vortex modes (see Zaqarashvili et al. 2011b; Soler et al. 2013b), also called forced neutral oscillations (Vranjes & Kono 2014). Vortex modes are associated with vorticity perturbations in the neutral fluid and do not represent Alfvén waves. Hence, the solutions corresponding to vortex modes are discarded from the present study. We focus on studying the quality factor of the Alfvén waves.
Figure 3 shows contour plots of the quality factor (in logarithmic scale) as a function of height, h, above the photosphere for wavelengths, λ = 2π/k, in between 1 m and 10^{6} m. We note that the pressure scale height in the chromosphere is around 300 km, hence wavelengths above 10^{5} m are probably stretching the assumptions behind the local analysis. The quality factor does not show a strong dependence on the wave circular polarization, and both left and right polarized solutions have similar values of Q. However, the quality factor is found to be strongly dependent on the set of cross sections used in the computations. Figure 3 displays some regions where Alfvén waves are overdamped, i.e., Q< 1/2 (see the regions denoted by red dotted lines in the various panels). The position of these regions of overdamping is different depending on the cross sections used. For instance, the region of overdamping takes place at longer wavelengths for the HS cross sections than for the VK cross sections. Hence, the use of the more accurate VK cross sections has here a very strong impact. The presence of regions of overdamping has important implications concerning the dissipation of wave energy (see Soler et al. 2013b,a). Perturbations in the plasma whose wavelengths fall within those regions cannot propagate away from the location of the excitation in the form of traveling Alfvén waves. Instead, all the energy stored in the perturbations is necessarily dissipated in situ. This may translate in a strong plasma heating in those locations (see also Song & Vasyliūnas 2011).
The regions of overdamping shown in Fig. 3 can be directly related to the cutoff interval of wavelengths explored by Soler et al. (2013b). These authors found that there is an interval of wavelengths, namely λ_{1}<λ<λ_{2}, for which the ionneutral friction force becomes dominant over the restoring magnetic tension force. As a consequence, magnetic field perturbations decay in a time scale much shorter than the wave period, which result in the suppression of the Alfvén wave magnetic field oscillations. The existence of a critical interval of wavelengths for Alfvén waves in a partially ionized plasma was first reported by Kulsrud & Pearce (1969) and was subsequently investigated by, e.g., Mouschovias (1987), Kamaya & Nishi (1998), Soler et al. (2013b,a,c), among others. The overall physical picture taking into account the dynamics of ions, electrons, and neutrals can be summarized as follows. Ions, electrons, and neutrals move as a single fluid when λ>λ_{2}. When λ_{1}<λ<λ_{2}, the strength of friction becomes larger than that of magnetic tension and the fluids cannot oscillate as a whole any more, i.e., magnetic tension is not strong enough to move the whole plasma. When λ<λ_{1} neutrals decouple from ions and electrons, i.e., magnetic tension is again able to put ions and electrons into motion, but neutrals remain at rest. Thus, when λ<λ_{1} Alfvén waves only produce perturbations in the ion and electron fluids, whereas neutrals are not perturbed. The critical interval of wavelengths represents the transition from the regime where ions, electrons, and neutrals support Alfvén waves to the regime where Alfvén waves perturb ions and electrons only (see an extended discussion in Kamaya & Nishi 1998).
As explained in Soler et al. (2013b), the presence or absence of the critical interval of wavelengths depends upon the value of the ionization fraction, χ = ρ_{n}/ρ_{i}. The condition to be satisfied is that χ> 8, which takes place for h ≲ 1500 km in the present chromospheric model. Analytic expressions of λ_{1} and λ_{2} were obtained by Soler et al. (2013b), namely (38)where the − and the + signs stand for λ_{1} and λ_{2}, respectively. Simplified expressions for these wavelengths can be obtained assuming weak ionization, i.e., χ ≫ 1, so that the approximations areThese approximate wavelengths agree reasonably well with the boundaries of the regions of overdamping in Fig. 3. The differences may be attributed to the additional physical processes included here and that were absent from the analysis of Soler et al. (2013b). The ratio of the two critical wavelengths is (41)Importantly, λ_{2}/λ_{1} is independent of the ionneutral collision cross section and is only a function of the ratio of neutral to ion densities. Equation (41) could be used to indirectly estimate the plasma ionization degree if the values of λ_{1} and λ_{2} were inferred from observations.
The effects of Hall’s current, electronneutral collisions, electron inertia, magnetic difussion, and viscosity were absent from the work of Soler et al. (2013b). The additional physical effects considered here provide a more realistic representation of the chromospheric plasma and have an impact on the behavior of the waves. The presence of Hall’s current and electron inertia cause the strict frequency cutoffs obtained by Soler et al. (2013b) to be replaced by zones where Alfvén waves are overdamped. This result was also discussed in the previous work by Zaqarashvili et al. (2012). In simple physical terms, the effect of Hall’s current and electron inertia for removing the strict frequency cutoff can be understood as follows. In the absence of Hall’s current and electron inertia, electrons can be considered as tightly coupled to ions, in the sense that electrons just follow the behavior of ions. Both ions and electrons are frozen into the magnetic field. In this case, ionneutral collisions can completely suppress the magnetic field perturbations and so cause the cutoff, as discussed in Soler et al. (2013b). However, when either Hall’s current or electron inertia are included, electrons can have a different dynamics than that of ions. Ions may not be able follow the magnetic field fluctuations due to the effect of ionneutral collisions, but it is easier for electrons to remain coupled to magnetic field. Therefore, ionneutral collisions cannot completely suppress the fluid oscillations because of the distinct behavior of electrons when Hall’s current and/or electron inertia are included (see also the discussion in Pandey & Wardle 2008).
The influence of Hall’s current also allows us to understand why, within the regions of overdamping, the damping is stronger for the HS model than for the VK model. Hall’s current helps to reduce the efficiency of damping, i.e., the influence of Hall’s current increases the quality factor. The importance of Hall’s current grows when the wave frequency increases and approaches the ion cyclotron frequency. Since the region of strongest damping takes place at higher frequencies (shorter wavelengths) in the VK case than in the HS case, the effect of Hall’s current in the regions of overdamping is more important in the VK case than in the HS case. Thus, the strength of the damping appears to be slightly lower in the VK case than in the HS case when the value of the quality factor within the regions of overdamping of Fig. 3 is compared.
Fig. 4 Contour plots of the quality factor Q (in logarithmic scale) of periodically driven Alfvén waves in the upper solar chromosphere as function of the frequency f (vertical axis in logarithmic scale) and height above the photosphere (horizontal axis). Top and botton panels correspond to the left and right polarized waves, respectively. Left and right panels are the results obtained using the hardsphere cross sections (HS) and the Vranjes & Krstic (2013) cross sections (VK), respectively. The black dashed line corresponds to the approximate optimal frequency given in Eq. (43). We note that the VK results are only strictly valid for heights larger than 900 km. 

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4.2. Periodic driver
Here we move to study the case of Alfvén waves excited by a periodic driver. Thus, we explore the spatial damping of the waves for a fixed frequency. Now the dispersion relation is solved to obtain the complex wavenumber and to compute the quality factor afterwards. The dispersion relation has twelve solutions for the wavenumber. As in the case of the solutions for the frequency explored in the previous subsection, some of the solutions do not actually correspond to propagating Alfvén waves. Instead, these solutions are heavily damped modes because they are directly related to the various dissipative mechanisms included in the main equations. As before, these solutions are discarded from our study and we only focus on investigating the quality factor of the Alfvén waves.
Figure 4 shows contour plots of the quality factor as a function of height, h, above the photosphere for frequencies, f = ω/ 2π, in between 10^{3} Hz and 10^{6} Hz. We note that the wavelengths associated with the frequencies of the lower part of this range may be greater than the pressure scale height in the chromosphere. Hence, the local analysis may be compromized for the lowest frequencies considered in Fig. 4. Visually, in Fig. 4 we do not see noticeable differences between the left and right polarized solutions. This is so because the considered wave frequencies are lower than the ion cyclotron frequency. A remarkable difference with the case of temporal damping displayed in Fig. 3 is that the quality factor never goes below Q = 1/2. In the case of spatial damping the waves are not overdamped. There is, however, a region around a certain optimal frequency where the damping is maximal, i.e., Q reaches its lowest value. This optimal frequency varies with height and depends on the cross sections used in the computations. The optimal frequency is about two orders of magnitude higher in the VK case than in the HS case. Again, the use of the more accurate VK cross sections has a strong impact on the results.
Fig. 5 Contour plots of the ratio of Ohm’s heating rate to ionneutral collisions heating rate (in logarithmic scale) for periodically driven Alfvén waves in the upper solar chromosphere as function of the frequency f (vertical axis in logarithmic scale) and height above the photosphere (horizontal axis). We used the expression derived by Song & Vasyliūnas (2011, Eq. (A.5)). Left and right panels are the results obtained using the hardsphere cross sections (HS) and the Vranjes & Krstic (2013) cross sections (VK), respectively. The red dotted line denotes the same heating rate for both mechanisms. We note that the VK results are only strictly valid for heights larger than 900 km. 

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As before, we can use the previous results by Soler et al. (2013b) in order to better understand the computations displayed in Fig. 4. From Eqs. (37) and (38) of Soler et al. (2013b) we can derive the optimal frequency for the damping of Alfvén waves due to ionneutral collisions exclusively. Equations (37) and (38) of Soler et al. (2013b) correspond to the real and imaginary parts of the wavenumber, so that an expression of the quality factor can be straightforwardly computed as (42)We find that the quality factor is minimal, i.e., the damping is maximal, when , which corresponds to an optimal wave frequency, f_{op}, given by (43)We overplot in Fig. 4 the optimal frequency computed from Eq. (43) and an excellent agreement is found. In this case, the improved physics taken into account in the present work does not significantly modify the main results by Soler et al. (2013b) concerning the efficiency of ionneutral collisions as a damping mechanism for periodically driven Alfvén waves.
5. Discussion
In this paper we have investigated theoretically the damping of Alfvén waves in the partially ionized chromosphere. The present analysis improves the physical description of the chromospheric plasma considered in previous computations by, e.g., Soler et al. (2013b), by including several processes missing from the previous works. Ionneutral collisions have a strong impact on the damping of both impulsively driven and periodically driven Alfvén waves in the chromosphere. Thus, Alfvén waves with frequencies near the ionneutral collision frequency are very efficiently damped. Ionneutral collisions are the most important damping mechanism in that frequency range, while the other damping mechanisms considered in this work, namely viscosity, magnetic diffusion, and electronneutral collisions, provide corrections to the damping by ionneutral collisions. The implications of this strong damping for plasma heating are straightforward.
In the case of waves excited by an impulsive driver, we found that the strict frequency cutoff due to ionneutral collisions commonly discussed in the literature (e.g., Kulsrud & Pearce 1969; Kamaya & Nishi 1998; Soler et al. 2013b) is here replaced by a critical interval of wavelengths for which Alfvén waves are overdamped, i.e., their propagation is inhibited due to the very strong damping. Hall’s current and electron inertia are the main physical effects responsible for removing the strict cutoff (see Zaqarashvili et al. 2012). In a recent work, Vranjes & Kono (2014) claim that the strict cutoff occurs regardless of the presence of Hall’s current and the electron inertia term. Although Vranjes & Kono (2014) use a set of equations similar to the one used here and their mathematical analysis is correct, their conclusions concerning the presence of the strict cutoff do not agree with our findings. The present results, and those of Zaqarashvili et al. (2012), indicate that strict cutoffs should also be absent from the results of Vranjes & Kono (2014). In connection to the amount of wave energy that can be dissipated in the plasma, the fact that the waves have strict cutoffs (Q = 0) or are overdamped (0 <Q< 1/2) makes no practical difference. In both cases, all the energy of the disturbance is dissipated in situ instead of traveling far away as a propagating wave.
All the energy stored in the impulsively generated perturbations with wavelengths belonging to the critical interval is necessarily dissipated in the vicinity of the location of the impulsive driver instead of begin transported away by propagating waves. Strong plasma heating might therefore be produced by these overdamped waves. It is seen from Fig. 3 that the impulsively driven waves are overdamped when the spatial extent of the perturbation is in the range from 1 km to 50 km in the HS case, and from 1 m to 1 km in the VK case, while the perturbations with spatial extents outside these intervals generate regular propagating waves. In a realistic chromosphere, where the plasma and the magnetic field dynamically evolve in time, Alfvén waves are most likely to be impulsively driven continuously and everywhere in the chromosphere, meaning that overdamped Alfvénic perturbations may contribute significantly to chromospheric heating. Another way to excite overdamped, shortwavelength Alfvén waves in the chromosphere is by means processes like cascades of energy via magnetohydrodynamic turbulence. However, to determine how the waves are excited and what is the actual heating rate generated by the overdamped waves, it is necessary, first, to consider selfconsistent numerical simulations including the excitation and back reaction of the waves on the plasma and, second, to use the full form of the energy equation taking into account all the possible sources and sinks of energy.
Periodically driven Alfvén waves are not overdamped, but there is an optimal driving frequency that produces the strongest damping and thus the strongest energy dissipation. From Fig. 4 we see that the optimal driving frequency varies from 1 Hz to 10^{2} Hz in the HS case, and from 10^{2} Hz to 10^{4} Hz in the VK case. Ionneutral collisions and Ohmic dissipation are two possible processes that can produce heating for the periodically driven waves. Song & Vasyliūnas (2011) derived an expression for the heating rate due to Ohmic dissipation and ionneutral collisions as a function of the frequency (see their Eq. (A.5)). From the expression derived by Song & Vasyliūnas (2011), the ratio of Ohm’s heating rate to ionneutral collisions heating rate is (44)Equation (44) compares the efficiency of the two heating mechanisms. Figure 5 displays the ratio of heating rates computed from Eq. (44). Ionneutral collisions heating is much more important that Ohmic heating in the upper chromosphere unless high driving frequencies are considered. Importantly, ionneutral collisions heating dominates over Ohmic heating not only for frequencies near the optimal frequency but also for lower frequencies. Again, there are differences between the results for the HS and the VK cross sections. The VK case requires higher frequencies than the HS case for Ohmic heating to be of importance compared to ionneutral collisions heating. Viscosity is another dissipative mechanism capable of producing plasma heating.
Throughout this paper it has been stressed that the value of the ionneutral cross section plays a very relevant role. This parameter directly determines, among other things, what wavelengths and frequencies are most efficiently damped and how they vary with height in the chromosphere. We found significant differences in the estimations of the critical wavelengths and optimal frequencies depending on the set of cross sections used in the computations. The classic hardsphere value of the cross section differs about two orders of magnitude from the recent quantummechanical calculations of this parameter by Vranjes & Krstic (2013). The values proposed by Vranjes & Krstic (2013) take into account several physical effects missing in the hardsphere model, so that the VK cross sections are more physically accurate than the HS cross sections. Since the numerical value of the cross sections plays an important role, in principle the more accurate VK values are the ones that should be used in theoretical computations.
However, although the basic atomic physics is obviously the same for laboratory plasmas and the chromospheric plasma, the chromosphere is far from being a controlled environment like a laboratory plasma. The chromosphere is a multithermal, multifluid environment. The cross sections measured in controlled laboratory plasmas or those theoretically computed in idealized models, as in Vranjes & Krstic (2013), may not necessarily match the effective ionneutral collision cross section in the chromospheric plasma. The use of observations of magnetohydrodynamic waves in the solar atmosphere in combination with the predicted behavior of these waves in theoretical models is an indirect method infer physical properties of the plasma and/or the magnetic field called magnetohydrodynamic seismology (see, e.g., Uchida 1970; Roberts et al. 1984). We propose that future observations with sufficiently high temporal and spatial resolutions may be able to detect the optimal wavelengths and frequencies for the damping of Alfvén waves in the chromosphere. Thus, a seismological test of the effective ionneutral collision frequency and cross section in the chromospheric plasma may be possible if the required observations become available. In this direction, solar observations performed with ALMA (see Karlický et al. 2011) may shed some light on these important problems and on the role of highfrequency Alfvén waves in chromospheric heating.
While in this paper we have investigated Alfvén waves, most of the results can be extrapolated to the case of magnetohydrodynamic kink waves, which have a predominantly Alfvénic character (Goossens et al. 2012). Kink waves have been observed in the chromosphere (e.g., Kukhianidze et al. 2006; Zaqarashvili et al. 2007; Okamoto & De Pontieu 2011; Pietarila et al. 2011; Kuridze et al. 2012; Morton 2014). Results from Soler et al. (2012, 2013c) indicate that ionneutral collisions affect kink waves in a similar manner as they affect pure Alfvén waves. The critical wavelengths and optimal frequencies that maximize the damping would be the same for both pure Alfvén waves and kink waves. Hence, the main conclusions of this paper are also valid in the case of kink waves.
Finally, we should discuss some of the limitations of this study. The two main simplifications are, first, the static chromospheric model and, second, the local analysis of the perturbations. On the one hand, the chromospheric model is based on the FAL93F static onedimensional model, which misses part of the highly dynamical behavior observed in the actual chromosphere. On the other hand, the local analysis does not fully capture the behavior of waves with wavelengths similar to or longer than the stratification scale height and ignores their possible reflection (Zaqarashvili et al. 2013; Tu & Song 2013). This second limitation may be overcome in future studies by investigating the propagation and damping of the waves using numerical simulations that consistently include the effect of gravitational stratification as in, e.g., Russell & Fletcher (2013) and Tu & Song (2013). Furthermore, in order to properly address the first of the limitations discussed above, these numerical simulations should include a timedependent dynamic background instead of the static model adopted here. This is an interesting task to be done in forthcoming investigations.
Acknowledgments
We thank the referee, Dr. Richard Morton, for useful suggestions that helped us to improve the quality of the paper. We acknowledge discussion within the ISSI team on “Partially ionized plasmas in astrophysics” and thank ISSI for their support. R.S. and J.L.B. acknowledge support from MINECO and FEDER funds through project AYA201122846, and from CAIB through the “Grups Competitius” program and FEDER funds. R.S. also acknowledges support from MINECO through a “Juan de la Cierva” grant, from MECD through project CEF110012, and from the “Vicerectorat d’Investigació i Postgrau” of the UIB. The work of T.Z. was supported by the Austrian Fonds zur Förderung der Wissenschaftlichen Forschung (project P26181N27), by the European FP7PEOPLE2010IRSES269299 project SOLSPANET and by Shota Rustaveli National Science Foundation grant DI/14/6310/12.
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All Figures
Fig. 1 Dependence on height above the solar photosphere of the a) plasma temperature and b) hydrogen ionization fraction, χ = ρ_{n}/ρ_{i}, according to the FAL93F model. c) Magnetic field strength as a function of height according to the semiempirical relation of Eq. (1). We note the logarithmic scale in the vertical axis of panel b). 

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In the text 
Fig. 2 Dependence on height above the solar photosphere of the collision frequencies for a) ions, b) electrons, and c) neutrals. HS and VK denote collision frequencies with neutrals computed with the hard sphere cross sections and the Vranjes & Krstic (2013) cross sections, respectively. In panels a) and b), Ω_{i} and Ω_{e} denote the ion and electron cyclotron frequencies, respectively. 

Open with DEXTER  
In the text 
Fig. 3 Contour plots of the quality factor Q (in logarithmic scale) of impulsively driven Alfvén waves in the upper solar chromosphere as function of the wavelength λ (vertical axis in logarithmic scale) and height above the photosphere (horizontal axis). Top and botton panels correspond to the left and right polarized waves, respectively. Left and right panels are the results obtained using the hardsphere cross sections (HS) and the Vranjes & Krstic (2013) cross sections (VK), respectively. The red dotted lines enclose zones where Alfvén waves are overdamped, i.e., Q< 1/2. The white dashed lines correspond to the approximate critical wavelengths given in Eqs. (39) and (40). We note that the VK results are only strictly valid for heights larger than 900 km. 

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In the text 
Fig. 4 Contour plots of the quality factor Q (in logarithmic scale) of periodically driven Alfvén waves in the upper solar chromosphere as function of the frequency f (vertical axis in logarithmic scale) and height above the photosphere (horizontal axis). Top and botton panels correspond to the left and right polarized waves, respectively. Left and right panels are the results obtained using the hardsphere cross sections (HS) and the Vranjes & Krstic (2013) cross sections (VK), respectively. The black dashed line corresponds to the approximate optimal frequency given in Eq. (43). We note that the VK results are only strictly valid for heights larger than 900 km. 

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In the text 
Fig. 5 Contour plots of the ratio of Ohm’s heating rate to ionneutral collisions heating rate (in logarithmic scale) for periodically driven Alfvén waves in the upper solar chromosphere as function of the frequency f (vertical axis in logarithmic scale) and height above the photosphere (horizontal axis). We used the expression derived by Song & Vasyliūnas (2011, Eq. (A.5)). Left and right panels are the results obtained using the hardsphere cross sections (HS) and the Vranjes & Krstic (2013) cross sections (VK), respectively. The red dotted line denotes the same heating rate for both mechanisms. We note that the VK results are only strictly valid for heights larger than 900 km. 

Open with DEXTER  
In the text 
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