Issue 
A&A
Volume 512, MarchApril 2010



Article Number  A28  
Number of page(s)  5  
Section  The Sun  
DOI  https://doi.org/10.1051/00046361/200913478  
Published online  25 March 2010 
Time damping of nonadiabatic magnetohydrodynamic waves in a partially ionized prominence plasma: effect of helium
R. Soler  R. Oliver  J. L. Ballester
Departament de Física, Universitat de les Illes Balears, 07122 Palma de Mallorca, Spain
Received 15 October 2009 / Accepted 14 December 2009
Abstract
Context. Prominences are partially ionized, magnetized
plasmas embedded in the solar corona. Damped oscillations and
propagating waves are commonly observed. These oscillations have been
interpreted in terms of magnetohydrodynamic (MHD) waves. Ionneutral
collisions and nonadiabatic effects (radiation losses and thermal
conduction) have been proposed as damping mechanisms.
Aims. We study the effect of the presence of helium on the time
damping of nonadiabatic MHD waves in a plasma composed by electrons,
protons, neutral hydrogen, neutral helium (He I), and singly ionized helium (He II) in the singlefluid approximation.
Methods. The dispersion relation of linear nonadiabatic MHD
waves in a homogeneous, unbounded, and partially ionized prominence
medium is derived. We compute the period and the damping time of
Alfvén, slow, fast, and thermal waves. A parametric study of the ratio
of the damping time to the period with respect to the helium abundance
is performed.
Results. The efficiency of ionneutral collisions, as well as
thermal conduction, is increased by the presence of helium. However, if
realistic abundances of helium in prominences (10%) are considered, this has a minor influence on the wave damping.
Conclusions. The presence of helium can be safely neglected in studies of MHD waves in partially ionized prominence plasmas.
Key words: Sun: oscillations  magnetic fields  Sun: corona  Sun filaments, prominences
1 Introduction
Smallamplitude oscillations and propagating waves are commonly observed in both quiescent and active region prominences/filaments. They have been interpreted in terms of magnetohydrodynamic (MHD) eigenmodes of the magnetic structure and/or propagating MHD waves. The reader is referred to some recent reviews for more information about the observational and theoretical backgrounds (Engvold 2008,2004; Banerjee et al. 2007; Ballester 2006; Oliver & Ballester 2002).
Prominence oscillations are known to be quickly damped, with damping times corresponding to a few oscillatory periods (reviewed by Mackay et al. 2010; Oliver 2009). Several damping mechanisms of MHD waves have been proposed, with nonadiabatic effects and ionneutral collisions the more extensively investigated. To understand these effects in detail, they have been studied in simple configurations such as unbounded and homogeneous media. Carbonell et al. (2004) investigated the time damping in a homogeneous prominence medium taking nonadiabatic effects (optically thin radiation losses and thermal conduction) into account. Later on, the spatial damping was studied by Carbonell et al. (2006) and the effect of a background mass flow was analyzed by Carbonell et al. (2009). Subsequently, some works have extended these previous results by considering the presence of the coronal medium (Soler et al. 2009a,2007,2008). The common conclusion of these investigations is that only slow and thermal waves are efficiently damped by nonadiabatic effects, while fast waves are very slightly damped and Alfvén waves are completely unaffected.
On the other hand, the influence of partial ionization on the propagation and time damping of MHD waves has been also investigated in an unbounded medium. Forteza et al. (2007) follow the treatment by Braginskii (1965) to derive the full set of MHD equations along with the dispersion relation of linear waves in a partially ionized, singlefluid plasma (see also Pinto et al. 2008). The electrons, protons, and neutral hydrogen atoms were taken into account, whereas helium and other species were not considered. In a subsequent work (Forteza et al. 2008), they extended their previous analysis by considering radiative losses and thermal conduction by electrons and neutrals. Their main results with respect to the fully ionized case (Carbonell et al. 2004) were, first of all, that ionneutral collisions (by means of the socalled Cowling's diffusion) can damp both Alfvén and fast waves but nonadiabatic effects remain only important for the damping of slow and thermal waves, and second, that critical values of the wavenumber exist in which the real part of the frequency vanishes, so wave propagation is impossible for larger wavenumbers. Again, applications to a more complex cylindrical geometry have also been performed (Soler et al. 2009c,b).
On the basis of these previous results, it seems clear that partial ionization plays a relevant role on wave propagation in prominences. Prominences are roughly composed of 90% hydrogen and 10% helium but, to date, all the investigations considered a pure hydrogen plasma. Therefore, the effect of the helium on the propagation and damping of MHD waves is still unknown and is the motivation for the present work. Here, we consider an unbounded and homogeneous prominence medium permeated by a homogeneous magnetic field. The plasma is assumed to be partially ionized, because electrons, protons, neutral hydrogen, neutral helium (He I), and singly ionized helium (He II) are the species taken into account. Recent studies by Gouttebroze & Labrosse (2009) indicate that, for central prominence temperatures, the ratio of the number densities of He II to He I is around 10%, whereas the presence of He III is negligible. This result allows us to neglect He III in this work. Extending the works by Forteza et al. (2008,2007), the derivation of the basic MHD equations for a nonadiabatic, partially ionized, singlefluid plasma has been generalized by now considering five different species, allowing us to study how the presence of neutral and singly ionized helium affects their previous results.
This paper is organized as follows. The description of the equilibrium and the basic equations are given in Sect. 2. The results are discussed in Sect. 3. Finally, Sect. 4 contains the conclusion of this work.
2 Equilibrium and basic equations
Our equilibrium configuration is a homogeneous and unbounded partially ionized plasma composed by electrons, protons, neutral hydrogen, neutral helium, and singly ionized helium. Hereafter, subscripts e, p, H, He I, and He II explicitly denote these species, respectively. The magnetic field is also homogeneous and orientated along the xdirection, , with B_{0} constant. We adopt the singlefluid approximation. Following Forteza et al. (2008,2007) and neglecting the electron contribution, we define the centerofmass velocity, , as(1) 
with the relative density of species , and the corresponding species velocity. Equivalently, the equilibrium total density, , and gas pressure, p, are
(2) 
(3) 
Since , we get the relation . We assume a strong thermal coupling between species, so all the species have the same equilibrium temperature T. Then, the three equilibrium quantities are related as
(4) 
where R is the ideal gas constant and the mean atomic weight,
(5) 
We can express in a more convenient form,
here we have defined
(7) 
The quantity is equivalent to the mean atomic weight of a pure hydrogen plasma defined in Eq. (3) of Forteza et al. (2007), and ranges between for a fully ionized hydrogen plasma and for a fully neutral hydrogen gas. On the other hand, indicates the helium ionization degree. A realistic value of this parameter is according to the results of Gouttebroze & Labrosse (2009). From Eq. (6) one can see that because of the presence of helium. In the absence of helium, so . Figure 1 displays the dependence of on for several values of .
Figure 1: Mean atomic weight, , as a function of the relative neutral helium density, , for (dotted line), (dashed line), (solid line), and (dashdotted line). In all cases, . 

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The details of the derivation of the basic governing equations for a
nonadiabatic, partially ionized, onefluid plasma can be followed in,
e.g., Braginskii (1965), Forteza et al. (2008,2007), Pinto et al. (2008). Here, we follow the same procedure but generalize the analysis of Forteza et al. (2007)
by including additional species. In brief, the separate governing
equations for the five species are added and a generalized Ohm's law is
obtained. A key step in the present derivation is to compute the
density current, ,
as
(8) 
along with the condition , where , , and are the electron, proton, and He II number densities, respectively, and e the electron charge. The resulting general induction equation (see Eq. (14) of Forteza et al. 2007) contains several diffusion terms whose coefficients depend on the collisional frequencies between species. The physical meaning of these nonideal terms is explained in detail in Pinto et al. (2008). In particular, ionneutral collisions are responsible for the socalled Cowling's diffusion, which is much more efficient than Ohm's diffusion in a partially ionized plasma. However, some terms are not relevant for our present application. Hall's effect is negligible in prominence conditions (Soler et al. 2009c), and the socalled ``Biermann's battery'' term is identically zero in a homogeneous medium. For this reason, our final form of the induction equation only contains the terms corresponding to Ohm's and ambipolar (Cowling's) diffusion, along with the diamagnetic current term. Therefore, our basic equations are
(13) 
where is the material derivative for time variations following the plasma motion, N A^{2} is the magnetic permeability , is the adiabatic index, and are the Ohm's and Cowling's coefficients of magnetic diffusion, respectively, is the diamagnetic current coefficient, is the heatloss function, and is the thermal conductivity. The quantities and can be expressed in terms of their corresponding magnetic conductivities,
Thus, Ohm's and Cowling's conductivities, as well as the diamagnetic current coefficient, , which applies in our case when helium is included, are
(17) 
In addition, , , and are the electron, electronneutral, and neutral friction coefficients, respectively, whose expressions depend on the sum of the friction coefficients between particular species,
(18) 
(19) 
(20) 
Each particular friction coefficient, , is computed as
(21) 
with the number density of the species , the collisional frequency between species and , and
(22) 
with the mass particle of the species . As given by De Pontieu et al. (2001), see also Soler et al. (2009b), the collisional frequencies between electrons and protons or He II are
(23) 
with or He II and the Coulomb logarithm, while the collisional frequency between a charged species, , , or He II, and a neutral species, or He I, is
(24) 
with the Boltzmann's constant, and the collisional crosssection. Here, we consider the values m^{2}, and m^{2}.
Figure 2: Ratio of the damping time to the period, , versus the wavenumber, k, corresponding to the a) Alfvén wave, b) fast wave, and c) slow wave for , , and . The different linestyles represent (solid line), (dotted line), and (dashed line). The results for and are plotted by means of symbols for comparison. The shaded regions correspond to the range of typically observed wavelengths of prominence oscillations. 

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Figure 3: Ratio of the damping time to the period, , versus the wavenumber, k, corresponding to the a) Alfvén wave, b) fast wave, and c) slow wave for , , , and . The different linestyles represent B_{0} = 5 G (solid line), B_{0} = 10 G (dotted line), and B_{0}= 20 G (dashed line). 

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On the other hand, the thermal conductivity due to neutrals (Eq. (16) of Forteza et al. 2008) now has to include the helium contribution. According to Parker (1953), a corrected expression for the conductivity of neutrals in MKS units is
Finally, we assume an optically thin radiation (Hildner 1974) to represent the hydrogen radiative losses. According to Cox & Tucker (1969, see their Fig. 3), the radiative losses by helium are several orders of magnitude less than those of hydrogen for typical prominence temperatures (10^{4} K), hence irrelevant for the present investigation.
Hereafter, our analysis follows that of Forteza et al. (2008). We linearize the basic equations and assume small perturbations proportional to
.
Then the resulting equations (Eq. (18)(27) of Forteza et al. 2008)
are combined and finally two different, uncoupled dispersion relations,
one for Alfvén waves (their Eq. (28)) and another for
magnetoacoustic and thermal waves (their Eq. (30)), are obtained.
Although our definitions of ,
,
,
and
contain the effect of helium, the resulting dispersion relations are formally identical to those of Forteza et al. (2008).
For the sake of simplicity, we do not write these expressions here
again and refer the reader to that paper. The dispersion relations are
numerically solved for real values of the wavenumber modulus,
,
and the angle
between
and .
A complex frequency,
,
is obtained. The period, P, and damping time,
,
are related to the real and imaginary parts of the frequency as
(26) 
3 Results
In the following computations, unless otherwise stated, we consider typical quiescent prominence conditions, kg m^{3}, T=8000 K, and B_{0} = 5 G. Quantities , , and are considered free parameters. We focus our attention on the effect of the relative neutral helium density, , on the ratio .
3.1 Free propagation in an unbounded medium
First, we assume
.
Figure 2 displays
as a function of k
for the Alfvén, fast, and slow waves. The results corresponding to
several helium abundances are compared for hydrogen and helium
ionization degrees of
and
,
respectively. We see that even in the case of the largest quantity of helium considered (
), the presence of helium has a minor effect on the results. In the case of Alfvén and fast waves (Fig. 2a,b), their critical wavenumber (i.e., the value of k which causes the real part of the frequency to vanish) is shifted toward slightly lower values, so the larger
,
the smaller
.
This result can be understood by considering that the Alfvén wave critical wavenumber,
,
given by Eq. (38) of Forteza et al. (2008) is
with the Alfvén speed. Equation (27) is also approximately valid for the fast wave critical wavenumber. Then, we see that is inversely proportional to Cowling's diffusivity, . Since is larger in the presence of helium than in the pure hydrogen case, because of additional collisions of neutral and singly ionized helium species, is therefore smaller. Turning our attention to the slow wave (Fig. 2c), we see that the maximum and the right hand side minimum of are also slightly shifted toward lower values of k. Results from Carbonell et al. (2004) and Forteza et al. (2008) indicate that thermal conduction is responsible for the maximum and minimum of . Thus, the additional contribution of neutral helium atoms to thermal conduction (Eq. (25)) causes this displacement of the curve of . As for Alfvén and fast waves, this effect is not very important. For comparison, equivalent results with and are plotted by means of symbols in Fig. 2. We see that, for realistic values of , its role is almost irrelevant, meaning that the presence of He II can be neglected. It is worth mentioning that we repeated these calculations for other values of and had similar results.
Now, Fig. 3 shows the dependence of on the magnetic field strength, B_{0}. The value of Cowling's diffusion, , is proportional to B_{0}^{2} (see Eqs. (15) and (16)). For this reason, the Alfvén mode is more attenuated as B_{0} grows, since Cowling's diffusion is more efficient. The fast wave shows a similar behavior for large k, whereas for small k, including the region on typical wavelengths, the behavior is the opposite because the damping is dominated by thermal mechanisms instead of ionneutral collisions. As expected, the slow mode shows no dependence on the value of the magnetic field strength.
Figure 4: Damping time, , of the thermal wave versus the wavenumber, k, with . The different linestyles represent: (solid line), (dotted line), and (dashed line). In all computations, and . The result for and is plotted by means of symbols for comparison. 

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Next, we study the thermal mode. Since it is a purely damped, nonpropagating disturbance ( ), we only plot the damping time, , as a function of k for and (Fig. 4). We can see that the effect of helium is different in two ranges of k. For m^{1}, thermal conduction is the dominant damping mechanism, so the larger the amount of helium, the smaller because of the enhanced thermal conduction by neutral helium atoms. On the other hand, radiative losses are more relevant for m^{1}. In this region, the thermal mode damping time grows as the helium abundance increases. Since these variations in the damping time are very small, we again have to conclude that the damping time obtained in the absence of helium does not significantly change when helium is taken into account. Computations with other values of and do not modify this statement. We also checked that, as for the slow mode, the value of the magnetic field strength does not affect the thermal mode damping.
3.2 Constrained propagation by a waveguide
Figure 5: Ratio of the damping time to the period, , versus the wavenumber component parallel to magnetic field lines, k_{x}, corresponding to the a) Alfvén wave, b) fast wave, and c) slow wave for , with L=10^{5} m, , and . The different linestyles represent (solid line), (dotted line), and (dashed line). The vertical dotdashed lines in a) and c) correspond to the approximated critical wavenumbers given by Eqs. (29) and (30), respectively, for . 

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We can estimate the effect of a magnetic structure, say a slab or a
cylinder, which would act as a waveguide. To do so, we set the
wavenumber component in the perpendicular direction to magnetic field
lines to a fixed value,
,
with L a typical lengthscale in the perpendicular direction. Since highresolution observations of filaments (see, e.g., Lin et al. 2009,2007) show fine structures (threads) with a typical width of 100 km, we select
L = 10^{5} m as our perpendicular lengthscale. Therefore, the propagation angle
now depends on k_{x},
(28) 
Figure 5 displays the results for the Alfvén, fast, and slow waves. We see that the behavior of the three solutions is substantially different from that of the free propagation case. The Alfvén mode now possesses an additional critical wavenumber for low values of k_{x}, namely , which is independent of the ionization degree and the helium abundance. It can be approximated (see details in Soler et al. 2009b, Eq. (38)) as
On the other hand, the fast wave is now more attenuated in the relevant range of wavenumbers than in the free propagation case, whereas the slow wave also has a new critical wavenumber, namely , which falls within the relevant range. An expression for the slow mode critical wavenumber is also provided by Eq. (48) of Soler et al. (2009b), which in our present notation is
where is the sound speed, with the adiabatic index. The slow mode critical wavenumber is shifted toward higher values as the helium abundance increases. There is no additional critical wavenumber for the fast wave. These approximated critical wavenumbers are indicated in Fig. 5. We see excellent agreement in the case of the Alfvén mode critical wavenumber (Eq. (29)). For the slow wave, the approximated value (Eq. (30)) is slightly higher than when numerically obtained. The reason that makes the slow wave critical wavenumber less accurate is found in the simplifications assumed in its derivation (see extensive details in Soler et al. 2009b).
Finally, we also computed the results in the case of the guided thermal disturbance. We find that the thermal mode behavior is the same in the waveguide case and in the free propagation case. As a result, this mode is not affected by the variation of the propagation angle, and no further comments are needed.
4 Conclusion
In this work, we have studied the effect of helium (He I and He II) on the time damping of thermal and MHD waves in a partially ionized prominence plasma. This is an extension of previous investigations by Forteza et al. (2008,2007) in which helium was not taken into account. We conclude that, although the neutral helium increases the efficiency of both ionneutral collisions andthermal conduction, its effect is not important for realistic helium abundances in prominences. In addition, thanks to the very small He II abundance for central prominence temperatures, its presence is irrelevant to the wave behavior. This conclusion applies both to the free propagation case and the constrained propagation by a waveguide case. Although the role of He II (or even He III) could be greater for typical prominencecorona transition region temperatures, the present result allows future studies of MHD waves and oscillations in prominences to neglect the presence of helium. AcknowledgementsWe thank N. Labrosse for giving helpful information about the helium ionization degree in prominences, I. Arregui for some useful comments, and the anonymous referee for constructive suggestions. The authors acknowledge the financial support received from the Spanish MICINN, FEDER funds, and the Conselleria d'Economia, Hisenda i Innovació of the CAIB under Grants No. AYA200607637 and PCTIB2005GC303. R.S. thanks the CAIB for a fellowship.
References
 Ballester, J. L. 2006, Phil. Trans. R. Soc. A, 364, 405 [NASA ADS] [CrossRef] [Google Scholar]
 Banerjee, D., Erdélyi, R., Oliver R., & O'Shea, E. 2007, Sol. Phys., 246, 3 [NASA ADS] [CrossRef] [Google Scholar]
 Braginskii, S. I. 1965, Rev. Plasma Phys., 1, 205 [NASA ADS] [Google Scholar]
 Carbonell, M., Oliver, R., & Ballester, J. L. 2004, A&A, 415, 739 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Carbonell, M., Terradas, J., Oliver, R., & Ballester, J. L. 2006, A&A, 460, 573 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Carbonell, M., Oliver, R., & Ballester, J. L. 2009, NewA, 14, 277 [Google Scholar]
 Cox, D. P., & Tucker, W. H. 1969, ApJ, 157, 1157 [NASA ADS] [CrossRef] [Google Scholar]
 De Pontieu, B., Martens, P. C. H., & Hudson, H. S. 2001, ApJ, 558, 859 [NASA ADS] [CrossRef] [Google Scholar]
 Engvold, O. 2004, Proc. IAU Collq. on Multiwavelength investigations of solar activity, ed. A. V. Stepanov, E. E. Benevolenskaya & A. G. Kosovichev, 187 [Google Scholar]
 Engvold, O. 2008, in Waves & Oscillations in the Solar Atmosphere: Heating and MagnetoSeismology, ed. R. Erdélyi, & C. A. MendozaBriceño (Cambridge: Cambridge Univ. Press), IAU Symp., 247, 152 [Google Scholar]
 Forteza, P., Oliver, R., Ballester, J. L., & Khodachenko, M. L. 2007, A&A, 461, 731 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Forteza, P., Oliver, R., & Ballester, J. L. 2008, A&A, 492, 223 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Gouttebroze, P., & Labrosse, N. 2009, A&A, 503, 663 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Hildner, E. 1974, Sol. Phys., 35, 123 [NASA ADS] [CrossRef] [Google Scholar]
 Lin, Y., Engvold, O., Rouppe van der Voort, L. H. M., & van Noort, M. 2007, Sol. Phys., 246, 65 [NASA ADS] [CrossRef] [Google Scholar]
 Lin, Y., Soler, R., Engvold, O., et al. 2009, ApJ, 704, 870 [NASA ADS] [CrossRef] [Google Scholar]
 Mackay, D. H., Karpen, J. T., Ballester, J. L., Schmieder, B., & Aulanier, G. 2010, Space Sci. Rev., accepted [arXiv:1001.1635] [Google Scholar]
 Oliver, R. 2009, Space Sci. Rev., in press [Google Scholar]
 Oliver, R., & Ballester, J. L. 2002, Sol. Phys., 206, 45 [NASA ADS] [CrossRef] [Google Scholar]
 Parker, E. N. 1953, ApJ, 117, 431 [NASA ADS] [CrossRef] [Google Scholar]
 Pinto, C., Galli, D., & Bacciotti, F. 2008, A&A, 484, 1 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Soler, R., Oliver, R., & Ballester, J. L. 2007, A&A, 471, 1023 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Soler, R., Oliver, R., & Ballester, J. L. 2008, ApJ, 684, 725 [NASA ADS] [CrossRef] [Google Scholar]
 Soler, R., Oliver, R., & Ballester, J. L. 2009a, NewA, 14, 238 [Google Scholar]
 Soler, R., Oliver, R., & Ballester, J. L. 2009b, ApJ, 699, 1553 [NASA ADS] [CrossRef] [Google Scholar]
 Soler, R., Oliver, R., & Ballester, J. L. 2009c, ApJ, 707, 662 [NASA ADS] [CrossRef] [Google Scholar]
All Figures
Figure 1: Mean atomic weight, , as a function of the relative neutral helium density, , for (dotted line), (dashed line), (solid line), and (dashdotted line). In all cases, . 

Open with DEXTER  
In the text 
Figure 2: Ratio of the damping time to the period, , versus the wavenumber, k, corresponding to the a) Alfvén wave, b) fast wave, and c) slow wave for , , and . The different linestyles represent (solid line), (dotted line), and (dashed line). The results for and are plotted by means of symbols for comparison. The shaded regions correspond to the range of typically observed wavelengths of prominence oscillations. 

Open with DEXTER  
In the text 
Figure 3: Ratio of the damping time to the period, , versus the wavenumber, k, corresponding to the a) Alfvén wave, b) fast wave, and c) slow wave for , , , and . The different linestyles represent B_{0} = 5 G (solid line), B_{0} = 10 G (dotted line), and B_{0}= 20 G (dashed line). 

Open with DEXTER  
In the text 
Figure 4: Damping time, , of the thermal wave versus the wavenumber, k, with . The different linestyles represent: (solid line), (dotted line), and (dashed line). In all computations, and . The result for and is plotted by means of symbols for comparison. 

Open with DEXTER  
In the text 
Figure 5: Ratio of the damping time to the period, , versus the wavenumber component parallel to magnetic field lines, k_{x}, corresponding to the a) Alfvén wave, b) fast wave, and c) slow wave for , with L=10^{5} m, , and . The different linestyles represent (solid line), (dotted line), and (dashed line). The vertical dotdashed lines in a) and c) correspond to the approximated critical wavenumbers given by Eqs. (29) and (30), respectively, for . 

Open with DEXTER  
In the text 
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