Issue 
A&A
Volume 608, December 2017



Article Number  A108  
Number of page(s)  10  
Section  The Sun  
DOI  https://doi.org/10.1051/00046361/201731193  
Published online  13 December 2017 
Fast magnetohydrodynamic waves in a solar coronal arcade
School of Mathematics and Statistics, University of Sheffield, S3 7RH, UK
email: hthackray1@sheffield.ac.uk
Received: 18 May 2017
Accepted: 28 August 2017
Aims. Our aim is to investigate detailed properties of fast magnetohydrodynamic (MHD) modes of a threedimensional waveguide for a cylindrical magnetic arcade.
Methods. We derive governing equations and dispersion relations for different density profiles and numerically solve them to obtain discrete eigenvalues for fast modes and the corresponding eigenfunctions.
Results. We find that small changes in the density structure in the vicinity of the field lines can lead to drastic effects on propagating solutions and, under certain conditions, two evanescent waves arise.
Conclusions. We investigate coronal loop oscillations in an arcade as fast MHD modes of oscillations. We find that coronal loops with slightly different density structures can exhibit different oscillatory behaviour and some eigenmodes can be present or absent depending on this density structure. Though the model has a simple potential field, the role of a cylindrical waveguide in conjunction with differing density structures is demonstrated clearly. Multiplewavelength observations at several points in the coronal loop arcades is suggested for correct mode identification; this is crucial for unraveling the plasma properties of the oscillating loops.
Key words: Sun: magnetic fields / Sun: oscillations / Sun: corona / waves / magnetohydrodynamics (MHD)
© ESO, 2017
1. Introduction
It is generally believed that the plasma density decreases with height in the quiet Sun (see, e.g. Melrose 1980). However, some regions are more clearly visible than others in the solar atmosphere possibly due to localised heating and nonuniform plasma blobs present in these regions. It has been difficult to determine density stratification in such localised regions of the solar corona. In particular, the visible oscillating coronal loops are clearly illuminated against the surroundings in the Sun’s corona and it is generally believed that the plasma density along the field lines is denser compared to its surroundings in these loops. However, this really depends on the observing wavelength. Coronal extreme UV (EUV) wavelengths can cause cooler loops to appear dark compared to the material which surrounds them, and in certain EUV wavelengths, seemingly bright loops may be of lower density. The precise nature of the density stratification is, however, difficult to determine observationally, and multiple wavelength analysis is often necessary (e.g. Aschwanden 2005).
Some coronal loops have been seen to oscillate near regions of flaring events (Ashwanden et al. 1999; Nakariakov & Ofman 2001; Schrijver et al. 2002; Verwichte et al. 2004; Jain et al. 2014). Their intensity variations have been studied with the aim to determine magnetic field strength and density contrast in such oscillating loops (e.g. Nakariakov et al. 1999; Verwichte et al. 2004). An important observable of the oscillating loops is their periodicity (or the eigenfrequency of the trapped modes of oscillations) which are compared with the periodicities from an empirical model. These empirical models are crucial as the density and magnetic field strengths of the observed loops are then indirectly estimated from the models.
There have been many studies in the past that relate the oscillations of the coronal loops to the oscillations of a cavity in onedimensional (1D) wave cavity models (Edwin & Roberts 1983; Goossens et al. 2002; Nakariakov & Verwichte 2005; Andries et al. 2009). A threedimensional (3D) magnetohydrodynamic (MHD) model with dipole magnetic field in an isothermal condition was studied by Ofman et al. (2015) to explain vertical transverse oscillation (see also Liu & Ofman 2014). The authors conclude that the results of their stratified model are similar to a magnetic arcade without gravity. Recently strong evidence of multiple loops oscillating in a magnetic arcade has been reported by Jain et al. (2015) and Li et al. (2017), using AIA images (see, also, Verwichte et al. 2009, for TRACE data). Such observations undeniably require a new approach and investigation of wave cavities in multidimensional waveguides. In this context, Hindman & Jain (2014) explored the importance of fast MHD wave propagation in 2D and 3D waveguides (see Hindman & Jain 2015). Hindman & Jain (2014) argue that since the lowplasmabeta of the solar corona indicates a magnetically dominated environment, the eruptive events such as flares can easily stimulate and transmit fast MHD waves across the field lines of a coronal arcade. They first investigated the importance of fast MHD waves for a 2D waveguide and computed a continuous power spectrum due to fast wave propagation at an angle to the magnetic field direction for a driven problem. The interference between the waves travelling down the waveguides results in a rich power spectrum from which the dominant period and wavenumber information can be obtained. This enables an understanding of the type of oscillations, the waveguide, density and magnetic field stratification of the coronal loops in greater detail. Their work also emphasised the importance of magnetic pressure and magnetic tension forces in the corona as opposed to simply magnetic tension, the only restoring force in 1D wavecavity models.
Recently, Hindman & Jain (2015) considered a 3D waveguide consisting of a twoshell model of coronal loop structure in a cylindrical magnetic arcade. They investigated the fast MHD wave propagation for such a model in which the axial direction is invariant and the waves are trapped in radial and azimuthal direction. This study explains, for the first time, how the coupling of axial and radial modes can be attributed to the different linesofsight observation of an oscillating loop, resulting in vertically and horizontally polarised oscillations and how such an elliptical polarisation varies with height in a loop. The Hindman & Jain (2015) model has been promising for our understanding of the coupling of radial and axial velocities in a 3D waveguide, although the model interface, which represents the region where the observed oscillations are supposed to reside, is a very thin layer of a sharp density discontinuity. It was clearly discussed by Goossens et al. (2002) that when a sharp discontinuous density is replaced by a continuous smooth density variation, it gives rise to quasimodes which allow classic kink mode oscillations to be resonantly damped by quasimodes (see also Ruderman & Roberts 2002). We defer the studies of quasimodes for future work, and instead focus on studying the effect of a discontinuous transition of density on the fast discrete eigenmodes and eigenfunctions.
In this paper, we extend the twoshell model of Hindman & Jain (2015) by incorporating a middle shell of inhomogeneous density between the two shells to investigate whether a small variation in density structure alters the fast mode eigenfunctions or not. The middle shell represents the situation where an oscillating loop has maximum amplitude of oscillation in a region of enhanced or suppressed density compared to its immediate surroundings. We refer to this as a threeshell model. We first derive a dispersion relation relating the eigenfrequencies and wavenumbers and then solve it for various relative amplitudes of Alfvén speeds in the three shells. We compare the resulting propagation diagrams of eigenfrequencies for twoshell and threeshell models. We also compute the corresponding eigenfunctions to study various polarisations of the oscillating loop.
2. The model and governing equation
Following Hindman & Jain (2015), we consider the coronal loop structure as a halfcylindrical waveguide. We employ a model in cylindrical coordinates, that is (r,θ,y), and assume that the azimuthal range is such that θ lies between 0 and π, and assume the footpoints anchored in the photosphere.
In this regime, we assume a potential magnetic field of the form (1)in a low plasmabeta atmosphere, with negligible gravity effects. The equilibrium atmosphere is considered to be at rest.
Such a profile has been previously studied by many (e.g. Carrion 1988; Verwichte et al. 2006); however, none of these studies considered propagation in the axial direction perpendicular to the equilibrium magnetic field (i.e. in the ydirection), resulting in coupled radial and axial motion.
We also note that a more general magnetic field with B = (0,B_{θ},B_{z}) has been considered for MHD waves in 1D straight cylindrical plasmas (Appert et al. 1974; Sakurai et al. 1991; Khongorova et al. 2012). However, in the current study we focus on propagation in 3D waveguide (see also, Hindman & Jain 2015) in cylindrical arcades with a middle shell of varying thickness. We consider fast mode propagation in axial direction (k ≠ 0) and show how the coupling of radial and axial velocities leads to mixed horizontal and vertical polarisations.
The corresponding linearised momentum equation is thus (2)where subscript 0 denotes a background quantity, and subscript 1 a perturbed quantity. Here, J_{1} is the perturbed current density.
Considering Fourier analysis of perturbed quantities in the form sin(mθ)e^{iky}e^{− iωt}, we derive the perturbed axial and radial velocities (see also Hindman & Jain 2015): (3)Here, V_{A} = V_{A}(r) is the Alfvén speed, and the function, (4)is related to the temporal variation of the magnetic pressure.
Combining Eqs. (3) and (4) yields the governing equation (5)where Hindman & Jain (2015) solved this governing equation for an analytical model comprising two shells separated by an interface in the radial direction. In their model, density decreases radially as r^{4} in both shells, with a discontinuity at the interface. For such a density profile, the Alfvén speed V_{A}(r) ∝ r^{2} in each shell and the governing equation is simplified considerably with solutions in terms of modified Bessel functions I and K. Although mathematically tractable, the Hindman & Jain (2015) model is only applicable if the oscillating coronal loops reside in a thin shell at the interface of a dense plasma overlying an evacuated cavity. It is quite possible that many field lines close to one another can oscillate simultaneously in a wider region of smoothly varying density (instead of an interface with sharp density discontinuity) in the solar corona. A natural extension of this twoshell model, therefore, is with the inclusion of a middle shell of finite width near the interface. This is what is considered in the following sections.
The limit as r → 0 must first be addressed, since at r = 0 the magnitude of the magnetic field in (1) becomes infinitely large. Consider the twoshell model as in Hindman & Jain (2015), such that the Alfvén speed profile is (6)in the limit where b → 0. The resulting eigenfunctions of the governing Eq. (5) for the profile (6) yields (7)where (8)Continuity of eigenfunctions φ and the radial velocity u_{r} at r = r_{0}, and the condition φ(b) = 0 with evanescent solutions as r → ∞ produces the dispersion relation (9)Figure 1 shows the resulting eigenvalues obtained by solving Eq. (9) with solid lines for kb = 0.01 and kb = 0.5. For comparison, we also plot the eigenvalues of the twoshell model of Hindman & Hain (2015), where kb ≡ 0. We note that in the left panel, where kb = 0.01, the curves are indistinguishable from one another for all wavenumbers (kr_{0}) considered here. This is because the ratio is very small for kb ≪ 1. Thus, if kb ≪ 1, the magnetic field profile (see Eq. (1)) is reasonable, and we will consider the model arcades to be valid in 0 <r< ∞. This is justifiable as the eigenfunctions are evanescent for r ≪ r_{0} and r ≫ r_{0} + a.
Fig. 1
Propagation diagram for the eigenfrequencies against the wavenumber kr_{0}, for the ratio, and m = 1, for kb = 0.01 (left) and kb = 0.5 (right). 

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3. Threeshell profile
We consider the Alfvén speed V_{A}(r) in each shell as follows: (10)The corresponding densities ρ(r) in the shells are: (11)We note that there are two interfaces, r = r_{0} and r = r_{0} + a. An Alfvén speed profile such as the one shown in Eq. (10) enables two reasonable scenarios for the coronal loop densities. The first one is where V_{1}<V_{0}: thus, V_{1}<V_{m}<V_{0}, V_{1}<V_{0}<V_{m} or V_{m}<V_{1}<V_{0}. We will refer to this as the “piecewise linear I” model. The second one is where V_{0} = V_{1} and V_{0,1}>V_{m}, such that the middle shell is denser than its surroundings. We refer to this as the “piecewise linear II” model. We discuss results for each model after solving the governing equation.
Using the Alfvén speed profiles (10), the governing Eq. (5) reduces to (12)with (13)The solution of Eq. (12) takes the form of the modified Bessel functions I, K and L as defined in Dunster et al. (1990). For , Eq. (12) yields (14)where we ensure boundedness as r → 0 and r → ∞.
Similarly, for , the solution becomes (15)where (16)as defined in Dunster (1990).
The choice of is implied, since otherwise the modified Bessel function I becomes complex and unbounded at the origin. The choice of parity for becomes more clear when considering the propagation diagrams, shown in Sect. 4.
4. Results
4.1. Dispersion relation
Continuity of eigenfunctions and the radial velocity, at r_{0} and r_{0} + a, yields the dispersion relation. For the case where in Eq. (14), it takes the form (17)and when (see Eq. (15)), the L_{νm} modified Bessel function is used in place of I_{νm}.
Fig. 2
The nondimensionalised Alfvén speed against the wavenumber kr, for a) : (top panel), (middle panel), and b) : (bottom panel). In all cases, and kr_{0} = 0.2, for ka = 0.1 (left) and ka = 0.5 (right). 

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Fig. 3
Case I: . Propagation diagram for the eigenfrequencies against the wavenumber kr_{0}, for the ratios and , and m = 1, for ka = 0.1 (left) and ka = 0.5 (right). 

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Solving the dispersion relation for the eigenfrequencies and wavenumber kr_{0} allows us to examine the propagating and evanescent regions. The wavenumber kr_{0} can be considered as the nondimensionalised location of the first interface, between the inner cavity and the middle layer, and the thickness of the middle shell is represented by the nondimensionalised quantity ka. Throughout, the propagation diagrams show the solid curves as obtained from the threeshell model and the dasheddot curves as obtained from the twoshell model.
4.2. The piecewise linear I model
In this model, we consider two cases: and . Taking the ratio and the location of the first interface to be kr_{0} = 0.2, the plots of the nondimensionalised Alfvén speed against the wavenumber kr, are shown in Fig. 2 for thicknesses ka = 0.1 (left) and ka = 0.5 (right). In the top panel, we have assumed , in the middle panel , and in the bottom panel .
4.2.1. Case I:
First consider the case where V_{1}<V_{m}<V_{0}. We solve the dispersion relation (17) for the Alfvén speeds shown in Fig. 2 and plot the propagation diagram in Fig. 3, for azimuthal order m = 1. The upper and lower dashed lines are governed by the parity of and – in this case; for there to be propagating solutions, we take and we must take , to ensure boundedness of eigenfunctions as r → ∞. The grey area indicates the evanescent region, and the white area the propagating region, separated by a curve representing the cutoff frequency, above which waves propagate, and below which they are evanescent. The solid curves indicate the modes for the threeshell model. We also consider the twoshell model (see Hindman & Jain 2015) and solve the corresponding dispersion relation (18)The curves for the twoshell model are overplotted in Fig. 3 as dashdot lines.
We note that the n = 0 mode exists for both the twoshell (dashdot) and threeshell (solid) models. It also changes the propagating behaviour to evanescence for large values of kr_{0} in both models. However, as the thickness of the middle layer increases in the threeshell model, the absence of the higher order radial modes is noticeable. The n = 1 mode is present for ka = 0.1 (left panel) but is suppressed in the right panel for ka = 0.5. Recall that ka should be exactly zero for the dashdot curves and that is why the dashdot and solid curves do not overlap here. The nondimensionalised eigenfrequencies (obtained for kr_{0} = 0.1 in the twoshell model) now corresponds to kr_{0} = 0 and ka = 0.1. To further study the nature of the propagating solutions, we examine the eigenfunctions.
Fig. 4
Case I: . The eigenfunction, φ, normalised radial and axial velocities, u_{r} and u_{y} and polarisation fraction, f, against the wavenumber kr, for the ratios and , kr_{0} = 0.2, and m = 1, for ka = 0 (left column). This is analogous to the twoshell case. The middle column and right column are for the cases and , with kr_{0} = 0.2, and m = 1, for ka = 0.1 and ka = 0.5, respectively. The curves are normalised with respect to the eigenfunctions, for comparison. 

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We once again set ka = 0 and to reproduce the twoshell eigenfunctions studied in Hindman & Jain (2015), and compare with eigenfunctions for the threeshell model for , ka ≠ 0. Thus, in Fig. 4, we plot the nondimensionalised eigenfunctions φ, and the radial and axial velocities as a function of kr for three different values of ka. As expected from Fig. 3, not only are the higherorder modes absent in the middle and right panels, the peaks of the eigenmodes are now at the interface ka. This can be understood by the fact that it is as if the eigenfrequencies of the twoshell model are shifted from kr_{0} to ka.
We also plot the polarisation fraction, f, defined as (19)to study what portion of radial and axial velocities contribute at each wavenumber.
The fraction yields a value of 0 if the motion of the wave is fully radial, and yields a value of 1 if the motion is fully axial. The n = 0 mode displays a mixture of axial and radial motion. Such elliptical polarisation can be seen even for ka ≠ 0, but the location of the peak value appears to be shifted based on the thickness of the middle shell. The polarisation fraction also changes with radial height in all cases.
Fig. 5
Same as Fig. 3, except for . 

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Fig. 6
Same as Fig. 4, except . 

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Now, we consider the case where V_{1}<V_{0}<V_{m}. Solving the dispersion relation (17) for the Alfvén speeds in (10), the propagation diagrams shown in Fig. 5 are obtained. The upper boundary is now raised to where will allow real eigenfrequencies. As a result, for ka = 0.1, the n = 2 curve is no longer suppressed, and for ka = 0.5, the n = 1 curve now exists. Similar to Fig. 3, the solid curves do not overlap with the dashdot curves.
We compare the eigenfunctions in Fig. 6 in the same format as in Fig. 4. In the top panel, we note that the peaks are shifted to the interface at ka, and the n = 2 mode now exists for ka = 0.1, but is suppressed for ka = 0.5. The middle two panels once again indicate the axial and radial motion, as a function of kr. For the polarisation fraction, it is clear that the peak values are once again shifted relative to the position of the second interface, with elliptical motion present for large wavenumbers. Despite the shift, the polarisation fraction of n = 0 remains mostly unchanged.
It is interesting to note from Figs. 3 and 5 that if the middle shell is thin (e.g. ka = 0.1) and is less dense than the inner cavity (where r<r_{0}), and the eigenmodes and their behaviour are similar to the twoshell eigenfunctions. However, if the middle shell is denser than the inner cavity, the higher radial modes (n ≥ 2) do not exist.
4.2.2. Case II:
For V_{1}<V_{m}<V_{0} and V_{m}<V_{1}<V_{0}, we can also consider the case where . Solving the dispersion relation with L_{νm} in place of I_{νm} in Eq. (17), when V_{1}<V_{m}<V_{0} , we obtain the eigenfrequencies and wavenumber kr_{0}. The resulting propagation diagrams are shown in Fig. 7.
It is immediately apparent in Fig. 7 that the choice of has diminished the evanescent region that was previously shaded grey in Fig. 3. The change in parity of means that the upper boundary is indicative of , and the lower boundary of . The solid lines once again show the modes in the threeshell case, and the dashdot the modes in the twoshell case. The n = 0 curve in both plots becomes almost parallel with the lower boundary, though the n = 0 curve in the ka = 0.1 now begins at a nonzero wavenumber, around 0.3, since, as for , we have a nonzero interface at ka when kr_{0} = 0. The n = 1 and n = 2 curves in both propagation diagrams are displaced significantly when compared with the corresponding modes in the twoshell case. In the bottom right of each plot is the line which divides the evanescent and propagating regions.
Examination of the eigenmodes, radial and axial velocities and polarisation fraction, in Fig. 8, for the ka = 0.1 case, in comparison to the twoshell case, indicates that only the n = 1 and n = 2 modes exist for kr_{0} = 0.2. As expected for the ka = 0.5 case, only the n = 0 and n = 1 modes exist. The axial velocity for n = 0 shows quite unique behaviour in the middle shell. Once again, all modes exhibit evanescent behaviour below kr_{0}, and for large wavenumbers, kr.
Qualitatively, the radial velocities in the middle panel have the same behaviour after the second interface as they do beyond the interface in the corresponding plot to the left. However, the axial velocity of the n = 1 mode is enhanced in the middle layer for the ka = 0.1 case, resulting in mostly an axial motion in the polarisation fraction plot below. Once again, as in the twoshell case, the curves exhibit a mixture of axial and radial motions beyond the interface. In the right panel, the polarisation plot indicates that both the n = 0 and n = 1 modes exhibit a mixture of both radial and axial motion, particularly in the middle shell. For both ka = 0.1 and ka = 0.5, as the wavenumber becomes large the motion becomes almost equally radial and axial.
Fig. 7
Case II: . All parameters the same as in Fig. 4. 

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Fig. 8
Case II: . All parameters the same as in Fig. 4. 

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Now, consider the model where V_{m}<V_{1}<V_{0}. Figure 9 shows the propagation diagrams for this case. The lower boundary of permitted real eigenfrequencies is now imposed by the condition . Once again, the solid lines indicate the threeshell curves, and the dasheddot lines the twoshell curves. Whilst there is suppression of some of the radial modes, at kr_{0} = 0.2, the n = 2 mode still exists for both ka = 0.1 and ka = 0.5. Comparing the two thicknesses, we note that when the thickness of the middle shell increases, the number of modes increases. This is because, when ka becomes larger, it is as if we have only one interface at kr_{0} = 0.2, and so waves are produced in a similar manner as in the twoshell model.
We find the eigenfunctions, radial and axial velocities and polarisation fraction, as before, and plot them in Fig. 10. It is clear that as the middle shell widens, more and more higherorder modes are present. The modes of higher radial orders are clearly visible in the middle shell for ka = 0.5.
The axial and radial motion shown in the middle panels is manifested in the polarisation plots on the bottom panel. For large wavenumbers, motion becomes a mixture of both radial and axial, though, in both plots, n = 1, n = 2 and (in the ka = 0.5 plot) n = 3 show elliptical motion initially after the first interface.
4.3. The piecewise linear II model
If coronal loops are, in fact, an augmentation of plasma which lies along the fieldlines of a coronal arcade, then it logically follows that the density structure in the inner cavity would be the same just above and below the middleshell. We thus consider , with the Alfvén speed profile demonstrated in Fig 11. Hence, for real eigenfrequencies to exist, for V_{m}<V_{0}. We note that the case for V_{m}>V_{0}(=V_{1}) would correspond to a rarer middle shell surrounded by denser regions above and below it. Since coronal loops are believed to reside in a denser region, we do not consider this case.
Figure 12 shows the propagation diagram for where we first notice that for the threeshell model (solid curves), the eigenfrequencies are lower than the twoshell model (dashdot curves), for large kr. The second substantial curve, n = 1, asymptotes for large wavenumbers, as the n = 0 mode did for the piecewise linear I model. For ka = 0.1, there are only three modes in the propagating region, though one exists only for small wavenumbers. In the ka = 0.5 plot, there is still the existence of a mode close to the lower boundary, however the higherradialorder modes take on much the same qualitative behaviour as in the piecewise linear I model. We note that, in the ka = 0.5 plot, both the n = 0 and n = 1 curves become evanescent modes for high wavenumbers.
Fig. 9
Same as Fig. 7, except . 

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Fig. 10
Same as Fig. 8, except . 

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Figure 13 shows the φ eigenfunction, radial and axial velocities, and polarisation fraction, as a function of kr. For ka = 0.5, we see that the eigenfunction for n = 0 (solid) and n = 1 (dotted) is evanescent in the middle shell, that is, between kr_{0} and kr_{0} + ka. The dashed line (n = 2) is a body mode in the middle region. Figure 13 also shows that the axial velocity peaks in the middle shell. Thus, as shown in the bottom panel, the polarisation is predominantly axial in the middle shell.
5. Discussion
The actual oscillating solar coronal loops reside in a magnetic arcade, which appear to be finite in length. There is inhomogeneity along the waveguide and in the direction transverse to the magnetic loops. In the current model, we assume that the scalelength of the inhomogeneity along the waveguide is much larger than the scalelength of the inhomogeneity across the height of the arcade and thus we ignore the inhomogeneity in the axial direction and consider the magnetic field and density varying in the radial direction.
Hindman & Jain (2015) considered the density to decrease with the height in a cylindrical loop separated at an interface. They found that fast waves can be trapped if the Alfvén speed increases with height. In the present work, we introduced a middle shell near the interface. We find that the behaviour of the fast MHD waves depend significantly on the density variation with height with localised eigenmodes absent if the density decreases slowly with height. However, if the density decreases rapidly with height, the fast MHD waves are naturally refracted back towards the photosphere, forming a cavity within which they are trapped. Such modes will have a discrete spectrum.
When (see Figs. 8 and 9), the threeshell model yields similar results for the larger middleshell as the twoshell model. This is because, for large ka, the dispersion relation (17) reduces to the dispersion relation obtained for the twoshell model (see Eq. (18)). This can be understood as follows.
When the thickness of the middle shell increases,that is, ka → ∞, we can simplify the dispersion relation (17). The modified Bessel functions I and K have limiting values such that and as kr → ∞ (see Olver et al. 2010).
Thus, (24)The righthand side of Eq. (17) can then be rearranged, such that (25)and from (24) becomes (26)as ka → ∞.
Fig. 11
The nondimensionalised Alfvén speed against the wavenumber kr, for the ratios and V_{1} = V_{0}, with kr_{0} = 0.2, for ka = 0.1. 

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Thus, the dispersion relation in Eq. (17) reduces to (27)which is analogous to the twoshell case of Hindman & Jain (2015).
Similar to the current threeshell model, Edwin & Roberts (1983) also studied a cylindrical tube model. However, the Edwin & Roberts (1983) model only considers propagation in a direction parallel to the magnetic field. Here, we have a nonzero axial wavenumber. Additionally, contrary to the Edwin & Roberts (1983) model, here the density is varying with radius. Thus, the two models are not easily comparable (even for V_{Ae}>V_{A}>c_{e} as in Edwin & Roberts 1983). However, it is interesting to note from Fig. 13 the existence of two surface modes in the middle shell as also reported in Fig. 5 of Edwin & Roberts (1983).
6. Conclusions
We have studied the wavemodes of a 3D waveguide of a potential magnetic field arcade. Although the potential field arcade is an idealised situation for the solar corona, it enables us to investigate coronal loop oscillations as fast mode oscillations in the magnetically dominated solar corona. In particular, we investigated in detail the effect of a small region of inhomogeneity in the loop consisting of the twoshell model studied in Hindman & Jain (2015). We also compared the results of the threeshell model with the twoshell model. Similar to the twoshell, our threeshell model also supports the eigenmodes in the radial and azimuthal directions, and depending on the lineofsight observation, the motion can be a mixture of radial and axial velocities. The elliptical polarisation is quite natural in both models as the radial and axial velocity equations are coupled.
We find that, depending on the thickness of the middle layer, the propagation diagram changes. Not only do a subset of the eigenfrequencies of the twoshell model satisfy the dispersion relation here, but depending on the properties of the middle layer, the reflective property of the wave cavity changes which leads to either suppression of the higherorder radial modes (piecewise linear I model) or the suppression of the evanescent n = 0 mode. In the case of a middle layer which is denser compared with its surroundings (piecewise linear II), the n = 1 radial mode changes its propagating behaviour at large wavenumbers, kr, to evanescence. On the other hand, for a rarer loop embedded inside a denser surrounding, as shown in Fig. 6, the eigenfunctions are similar to the twoshell eigenfunctions (see, e.g. Hindman & Jain 2015).
Fig. 12
Propagation diagram for the eigenfrequencies against the wavenumber kr_{0}, for the ratio , with kr_{0} = 0.2, and m = 1, for ka = 0.1 (left) and ka = 0.5 (right). 

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Fig. 13
The eigenfunction, φ, radial and axial velocities, normalised u_{r} and u_{y} and polarisation fraction, f, against the wavenumber kr, for the ratio , with kr_{0} = 0.2, and m = 1, for ka = 0.1 (left) and ka = 0.5 (right). The curves are normalised with respect to the eigenfunctions, for comparison. 

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The present study of a threeshell model suggests that the propagating behaviour of the oscillating modes will be quite different in identical coronal loops if the location of observation is different in the respective waveguides. Even for the same eigenfrequency, slightly different inhomogeneity in Alfvén speeds in two different loops could result in very different eigenfunctions for a given wavenumber. One of the important findings of our threeshell model investigation is that some radial modes of the twoshell model (see Hindman & Jain 2015) are absent at the interface, r_{0}, if there is a small shell of increased density near the interface of the twoshell model. This suggests that some eigenmodes (or eigenfrequencies) may not be observed in such oscillating coronal loops.
We also find that, even in the fundamental mode (n = 0), its propagating behaviour is different depending on the wavenumber if there is a small shell of rarer plasma present within the twoshells considered by Hindman & Jain (2015). The presence and absence of eigenmodes is quite sensitive to the density inhomogeneity in a coronal loop; observation of two similarlooking loops could have very different eigenmodes if the density profiles are slightly different at the observation point. Thus, correct mode identification with multiple wavelength observation at several points on a coronal loop and arcade are essential for understanding the plasma properties of the oscillating loops correctly.
The presence and then subsequent absence of some trapped modes in the twoshell and threeshell models, respectively, suggests that it would be interesting to considering a smoothly varying density for the model arcades. This will introduce a singularity in Eq. (5), which will then introduce damping of modes near the Alfvén resonance. This will be the subject of future work.
Acknowledgments
We acknowledge the SoMaS (University of Sheffield) GTA funding. We thank the anonymous referee for suggesting improvements to the manuscript.
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All Figures
Fig. 1
Propagation diagram for the eigenfrequencies against the wavenumber kr_{0}, for the ratio, and m = 1, for kb = 0.01 (left) and kb = 0.5 (right). 

Open with DEXTER  
In the text 
Fig. 2
The nondimensionalised Alfvén speed against the wavenumber kr, for a) : (top panel), (middle panel), and b) : (bottom panel). In all cases, and kr_{0} = 0.2, for ka = 0.1 (left) and ka = 0.5 (right). 

Open with DEXTER  
In the text 
Fig. 3
Case I: . Propagation diagram for the eigenfrequencies against the wavenumber kr_{0}, for the ratios and , and m = 1, for ka = 0.1 (left) and ka = 0.5 (right). 

Open with DEXTER  
In the text 
Fig. 4
Case I: . The eigenfunction, φ, normalised radial and axial velocities, u_{r} and u_{y} and polarisation fraction, f, against the wavenumber kr, for the ratios and , kr_{0} = 0.2, and m = 1, for ka = 0 (left column). This is analogous to the twoshell case. The middle column and right column are for the cases and , with kr_{0} = 0.2, and m = 1, for ka = 0.1 and ka = 0.5, respectively. The curves are normalised with respect to the eigenfunctions, for comparison. 

Open with DEXTER  
In the text 
Fig. 5
Same as Fig. 3, except for . 

Open with DEXTER  
In the text 
Fig. 6
Same as Fig. 4, except . 

Open with DEXTER  
In the text 
Fig. 7
Case II: . All parameters the same as in Fig. 4. 

Open with DEXTER  
In the text 
Fig. 8
Case II: . All parameters the same as in Fig. 4. 

Open with DEXTER  
In the text 
Fig. 9
Same as Fig. 7, except . 

Open with DEXTER  
In the text 
Fig. 10
Same as Fig. 8, except . 

Open with DEXTER  
In the text 
Fig. 11
The nondimensionalised Alfvén speed against the wavenumber kr, for the ratios and V_{1} = V_{0}, with kr_{0} = 0.2, for ka = 0.1. 

Open with DEXTER  
In the text 
Fig. 12
Propagation diagram for the eigenfrequencies against the wavenumber kr_{0}, for the ratio , with kr_{0} = 0.2, and m = 1, for ka = 0.1 (left) and ka = 0.5 (right). 

Open with DEXTER  
In the text 
Fig. 13
The eigenfunction, φ, radial and axial velocities, normalised u_{r} and u_{y} and polarisation fraction, f, against the wavenumber kr, for the ratio , with kr_{0} = 0.2, and m = 1, for ka = 0.1 (left) and ka = 0.5 (right). The curves are normalised with respect to the eigenfunctions, for comparison. 

Open with DEXTER  
In the text 
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