Issue 
A&A
Volume 555, July 2013



Article Number  A74  
Number of page(s)  16  
Section  The Sun  
DOI  https://doi.org/10.1051/00046361/201220784  
Published online  03 July 2013 
Lineofsight geometrical and instrumental resolution effects on intensity perturbations by sausage modes
Centre for mathematical Plasma Astrophysics, Department of
Mathematics, KU Leuven,
Celestijnenlaan 200B, bus 2400, 3001
Leuven, Belgium
email: patrick.antolin@wis.kuleuven.be; tom.vandoorsselaere@wis.kuleuven.be
Received:
23
November
2012
Accepted:
19
March
2013
Context. Diagnostics of magnetohydrodynamic (MHD) waves in the solar atmosphere is a topic that often encounters interpretation problems, partly because of the high complexity of the solar atmospheric medium. Forward modelling can significantly guide interpretation, bridging the gap between numerical simulations and observations, and increasing the reliability of mode identification for applying MHD seismology.
Aims. We determine the characteristics of the fast MHD sausage mode in the corona on the modulation of observable quantities, such as line intensity and spectral line broadening. Effects of the lineofsight angle and of spatial, temporal, and spectral resolutions are considered.
Methods. We take a cylindrical tube that simulates a loop in a lowβ coronal environment with an optically thin background and let it oscillate with the fast sausage mode. A parametric study is performed.
Results. Longitudinal structuring of the intensity modulation is obtained and set by the nodal structure of the radial velocity. The modulation is strongly dependent on the contribution function of the spectral line. Under the assumption of equilibrium ionisation, the intensity variation can be very low (≲4% for Fe ix 171) or significant (35% for Fe xii 193). Most of this variation disappears when considering the radiative relaxation times of the ions, due to the fast timescales of the sausage mode in the corona. Regardless of the ionisation state of the plasma, the variation in spectral line broadening can be significant, even for low intensity modulation. The nature of this broadening is not thermal but is mostly turbulent. This places spectrometers in clear advantage over imaging instruments for the detection of the sausage mode. The modulation of all quantities can considerably decrease with the lineofsight angle with respect to the perpendicular to the tube axis. The spatial and temporal resolution are the main factors affecting modulation, erasing longitudinal structuring when these are on the order of the mode’s wavelength or the mode’s period, placing high constraints on instrumentation. Significant variability in all quantities can still be obtained when viewing at an angle of up to 30°, with pixel size resolutions up to onethird of the mode’s wavelength, or temporal resolution of one fifth of the mode’s period. Modulation is only weakly dependent on spectral resolution due to the mode’s inherent symmetry.
Key words: magnetohydrodynamics (MHD) / Sun: corona / Sun: oscillations
© ESO, 2013
1. Introduction
During the past decade solar physics has witnessed a boom in observational reports on wavelike behaviour in all layers of the solar atmosphere (see the recent review by De Moortel & Nakariakov 2012). This is due, on the one hand, to the advances in imaging and spectroscopic instruments, allowing higher spatial, temporal, and spectral resolutions, which have allowed proper visualization of magnetohydrodynamic (MHD) waves with a rather wide range of properties in terms of amplitudes, periods, and speeds. On the other hand, theoretical progress points to the strong potential of waves for explaining the heating demands of the chromosphere and the corona on the observed spatial and time scales, as well as the important role they can play for the indirect estimation of local physical parameters of the plasma (MHD seismology, Roberts et al. 1984; Uchida 1970; Aschwanden 2004; Taroyan & Erdélyi 2009). This of course applies to all physical parameters dictating the behaviour of these waves: the magnetic field strength (Nakariakov et al. 1999; Pascoe et al. 2007b), the magnetic field geometry (Verth & Erdélyi 2008; Ruderman et al. 2008; Van Doorsselaere et al. 2009), the density inhomogeneity (Aschwanden et al. 2003; Goossens et al. 2002, 2008; Arregui et al. 2007), the temperature structure, the response of the plasma to energy injection (polytropic index, Van Doorsselaere et al. 2011b), the plasma β parameter (Van Doorsselaere et al. 2011a), and the transport coefficients (Nakariakov & Verwichte 2005a). Therefore, much emphasis has been put on searching for all kinds of MHD waves, each contributing in a more or less specific way to the measurement of a specific quantity.
The fast MHD sausage mode (m = 0 mode), which we consider in this study, is compressible, characterised by axisymmetric radial displacements of the plasma, having magnetic pressure and gas pressure acting in phase as restoring forces. Thus, this mode does not perturb the main axis of loops but its crosssection, producing intensity variations and spectral line broadening.
The MHD fast sausage mode was first described analytically by Rosenberg (1970), Zaitsev & Stepanov (1975), Roberts et al. (1984), and Cally (1986). Most observations of oscillatory phenomena interpreted as sausage modes have been made in events associated to solar flares, observed with radiometers in the microwave range. These have been most frequently reported using the Nobeyama Radioheliograph (NoRH, Nakajima et al. 1994), with a cadence of 0.1 s and a spatial resolution of 5″−10″ observing in microwave frequencies of 17 GHz and 34 GHz (Nakariakov et al. 2003; Melnikov et al. 2005; Reznikova et al. 2007; Inglis et al. 2008). The RHESSI spectrometer (Lin et al. 2002), with a time resolution of 4 s and a spatial resolution of 2.3″ in the 3−100 keV range, has also been able to observe modulation characteristic of sausage modes in the hard Xray range (Zimovets & Struminsky 2010). In observations with the LYRA radiometer aboard PROBA2, which includes both chromospheric and coronal channels, Van Doorsselaere et al. (2011a) report two modes of oscillation in a single flaring loop, which were interpreted as slow and fast sausage modes. Few reports also exist in extreme ultraviolet (EUV) lines with the EIS spectrometer of Hinode (Kitagawa et al. 2010), with the Atmospheric Imaging Assembly of SDO (Su et al. 2012) and with SECIS (Williams et al. 2002, 2001). Similarly, few reports also exist in cooler (chromospheric and photospheric) lines with ARIES (Srivastava et al. 2008), with the Solar Optical Telescope of Hinode (Fujimura & Tsuneta 2009), and with the ROSA instrument (Morton et al. 2011; Jess et al. 2012; Morton et al. 2012).
Most observations of fast sausage modes are linked to quasiperiodic pulsations (QPPs) commonly observed during solar flares in microwave and soft and hard Xray ranges (see Nakariakov & Verwichte 2005b; De Moortel & Nakariakov 2012, for reviews on the subject). As shown by Mossessian & Fleishman (2012), not only can the sausage mode but also the kink and the torsional Alfvén mode lead to modulation of the source parameters (e.g. energetic electron distribution, magnetic field strength, and column thickness along the lineofsight) resulting in gyrosynchrotron radiation. Nakariakov et al. (2003) show that the period of the sausage mode in the corona is mostly determined by the length of the hosting structure and the external Alfvén speed, thus leading to very short periods. They further show that nonleaky sausage modes occur in sufficiently thick and dense loops, thus greatly constraining their existence in the solar atmosphere (Nakariakov et al. 2012). It is therefore not surprising that most of the reported sausage modes in the literature come from observations with high cadence instruments, mostly radiometers, and are mostly associated with flaring loops, where densities are high. However, by performing 2D MHD simulations, Pascoe et al. (2007b) have investigated the existence of sausage modes in long coronal loops with weak density contrast by extending the wave numbers into the leaky regime. In flaring conditions, they found sausage modes with periods from 5 s to 60 s of detectable quality in loops of length up to 60 Mm, thus supporting the interpretation from observations of QPPs. In this regime the period of the sausage mode is determined by the length of the loop and the external Alfvén speed, therefore providing a seismological way to measure the latter and the external magnetic field. Very few reports exist, however, of sausage modes in long coronal (nonflaring) loops, a fact that may be linked either to MHD radiation (leaky modes), leading to a poor quality factor for such modes, or to the lack of adequate temporal and spatial resolutions.
In a 3D MHD model De Moortel & Pascoe (2012) analyse the effects of lineofsight integration on energy budget estimates in multistranded coronal loops subject to propagating kink modes. The modes strongly couple to azimuthal Alfvén waves, to which all energy is eventually transferred, resulting in kinetic energy estimates from Doppler shifts one to two orders of magnitude lower than the true wave energy. This suggests that most of the energy could be observed in spectral line broadening.
Cooper et al. (2003a,b) used a 2D model to investigate analytically the modulation of intensity from propagating kink and sausage modes based on variation in the angle between the lineofsight and the emitting structure. They furthermore consider the effect of curvature and apply the results to explain propagating intensity perturbations along a loop observed with SECIS (Williams et al. 2001, 2002).
Gruszecki et al. (2012) have performed 3D numerical simulations of (trapped and leaky) sausage modes oscillating in a cylinder, and study the resulting modulation of the intensity along a ray perpendicular to the axis of the cylinder. They consider the variation in the pixel size, thus simulating different spatial resolution during observations, and find that intensity variation essentially disappears for resolutions close to the mode’s wavelength.
These previous works calculate the intensity by integrating the density squared along the lineofsight, and therefore ignore the radiative response of the plasma and effects from instrumental resolution. Based on numerical simulations, synthetic observations of TRACE channels and Hinode/EIS by De Moortel & Bradshaw (2008) illustrate the illposed intensity inversion problem, which can even alter the period of oscillations. Similarly, synthetic observations of AIA channels of SDO by MartínezSykora et al. (2011) show that a significant contribution to the emerging intensity can come from nondominant ions of a specific channel. These results imply that not only density but also ionisation balance and emissivity need to be taken into account for forward modelling intensities.
The application of MHD seismology strongly relies on the capacity to pinpoint the nature of the wave in observations. However, as analytical, numerical, and observational studies show, mode identification is far from a trivial matter. In this work we choose a simple approach to characterise the observable properties of the MHD fast sausage mode in the corona. This approach can be used as a platform for constructing more complex models or can help understand more complex numerical results, such as those coming from 3D numerical simulations. We assume that we have a cylindrical structure in a lowβ coronal environment, which offers significant density contrast with the ambient plasma, and hosts the fast sausage mode. By synthesising the emerging intensity in specific coronal lines using the CHIANTI atomic database (Dere et al. 1997, 2009), we investigate the effects from varying lineofsight angles, as well as effects from spatial, temporal, and wavelength resolutions on the modulation of observable quantities. By doing so we are able to predict the detectability of this mode with current instruments, as well as incoming instruments in the near future.
The paper is structured as follows. In Sect. 2 we describe the different models we considered, and in Sect. 3 we present the results from two different point of views: that of imaging instruments, and that of instruments with spectrometric capabilities. In Sect. 4 we discuss the results and conclude in Sect. 5.
2. Models
2.1. Variation in thermodynamic quantities
In the forward modelling approach, the task of identifying MHD modes in the solar corona starts by implementing these modes in realistic numerical simulations. For the latter, it is necessary first to identify the theoretical observational signatures from such modes, free of nonlinear effects. In this work we take such an approach and consider the simplest model of an axisymmetric plasma cylinder of radius R embedded in a lowβ coronal environment, oscillating with the sausage mode, i.e. the axisymmetric m = 0 mode described in Edwin & Roberts (1983). In this study we ignore the effects of gravity, fieldline curvature, and twist. The variation in the thermodynamic quantities is found by linearising the perturbed ideal MHD equations about the magnetostatic equilibrium. In a cylindrical coordinate system (r,φ,z) we have where v = (v_{r},v_{φ},v_{z}) is the perturbation velocity; ρ, p, B are the perturbed mass density, gas pressure, and magnetic field; and ρ_{0}, p_{0}, B_{0} = (0,0,B_{z,0}) correspond to the unperturbed quantities (with μ the magnetic permeability and γ = 5/3 the ratio of specific heats). In the case of a sinusoidal perturbation leading to a standing mode, we have ∇·v = −ℛ(r)Acos(ωt)sin(kz), where A is the total amplitude of the perturbation, k = πN/L_{0} is the longitudinal wavenumber (with N the longitudinal mode number, and L_{0} the length of the cylinder). In the case of a sausage mode, ℛ, the radial dependence of the divergence of v must satisfy (5)Here, , , where is the Alfvén speed and is the sound speed. ω satisfies the dispersion relation: (6)where K_{0} and J_{0} are the 0th order Bessel functions. The perturbed variables of interest become The unperturbed thermodynamic quantities are linked through the ideal gas law for a fully ionized hydrogen gas .
2.2. Base model
Once we know the analytical solution for the thermodynamic quantities we produce a 3D data cube of a cylinder oscillating with the sausage mode. All the models considered in this work are variations on a “base model”. For comparison purposes we choose our base model to be similar to the simulation model by Gruszecki et al. (2012). Accordingly, we take a discontinuous density profile with a mass density contrast ρ_{i}/ρ_{e} = 5 and a magnetic field ratio B_{i}/B_{e} = 0.89 between the interior and the exterior of the unperturbed cylinder. Correspondingly, the Alfvén speeds inside and outside the cylinder oscillate around 350 km s^{1} and 900 km s^{1}, respectively. The plasma β parameter is at all times lower than 0.3. The internal and external temperature for the unperturbed cylinder are set in this model to 1.05 × 10^{6} K and 2.4 × 10^{5} K. For a further analogy with Gruszecki et al. (2012), we choose the wavenumber in the base model as kR = 2.24, where R = 1 Mm denotes the radius of the cylinder. This results in a wavelength of ≈2.8 Mm. The amplitude A of the standing mode (see Eq. (7)) is chosen so as to generate velocity perturbations in agreement with typical values deduced from spectral line broadening in the corona (Chae et al. 1998; Peter 2010). Accordingly, we choose A = 0.011 (similar to the value used in Gruszecki et al. 2012).
Typical sizes for plasma inhomogeneities in the corona are still not well known. This has led to several debates concerning the concept of loops as monolithic or rather multistranded structures in the corona. Currently, stateoftheart coronal imaging devices such as SDO/AIA with instrumental point spread functions (PSF) in the range 1−1.2 Mm are providing increasing observational evidence for a family of structures with sizes not resolved by the telescopes (Brooks et al. 2012). Higher resolution imaging can be achieved with chromospheric instruments through tracing coronal rain in loops, which has provided evidence of strandlike structures of a few hundred km (Antolin & Rouppe van der Voort 2012). While these works reveal subarcsecond density structure providing support for multistranded loop models, it is reasonable to think that the collection of strands composing the loop (defining the main waveguide) is actually much larger and behave collectively, agreeing with our choice of 1 Mm for the radius of our loop. Such families of neighbour strands traced by coronal rain indeed have several Mm in diameters, as seen in Antolin & Verwichte (2011) or Antolin & Rouppe van der Voort (2012). Furthermore, it has been shown that the characteristics of a sausage mode are rather insensitive to the presence of crosssectional inhomogeneities in loops (Pascoe et al. 2007a, 2009).
Numerically, our numerical model consists of a 204 × 204 × N_{z} grid. The parameter N_{z} denotes the number of points in the z direction and is chosen so that the different lineofsight rays for the intensity calculation (explained in Sect.2.3) traverse the same crosssectional area in the model. In the base model, three wavelengths are enough, leading to N_{z} = 342 points. The spatial resolution in x, y, and z axes is the same: about 25 km. The fast sausage mode in the corona produces very low crosssectional area variation, which for some of the considered models leads to very low intensity variations. To correctly calculate the variations in those models we have also considered a numerical model with ten times the resolution in each direction. Correspondingly, all results related to intensity modulation are obtained with the highresolution models. All other results do not vary significantly between the low and high spatial resolution models.
Figure 1 shows a snapshot of our base model, representing a cut along the middle axis of the cylinder. The sausage mode creates inphase perturbations between the density and the magnetic field, and antiphase perturbations between the density and the radius. Furthermore, the radial and longitudinal velocities are π/4 out of phase with the density. The snapshot in Fig. 1 is taken at a time of onethird of the period P, which, in this model, corresponds to P ≈ 4.6 s. Positive velocity values correspond to outflow towards the axis of the cylinder. From Fig. 1 it can be noticed that the perturbation of longitudinal velocity is about one order of magnitude less than the radial perturbation. They have maximum values of about 19 km s^{1} and 3.4 km s^{1}, respectively. At the location of an antinode of the radial velocity, density oscillates about 7% around a mean value of 4.9 × 10^{12} kg m^{3}, and temperature oscillates about 5% around a mean value of 1.048 × 10^{6} K.
Fig. 1 Maps of radial velocity (topleft), longitudinal velocity (topright), density (bottomleft), and temperature (bottomright) along the middle of the cylinder for the base model − 171 (see Sect. 2.4 for more details). The snapshot is taken at onethird of the mode period. The black and white dashed lines in the top panels denote the 4 different lineofsight angles considered: 0°,30°,45°, and 60°. For each angle two rays along the lineofsight are plotted, one passing through a node of the radial velocity (left ray of the pair) and one passing through an antinode of the same quantity (right ray of the pair). The different pixel sizes considered are shown centred at a node: “0R” (=25 km), “1R” = 1 Mm, “2R” = 2 Mm, “3R” = 3 Mm. In the base model, 1R, 2R, and 3R correspond roughly to ℓ/3,2ℓ/3, and ℓ, respectively, where ℓ denotes the wavelength of the mode. 

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2.3. Calculation of synthetic spectra
To calculate synthetic spectra, we choose different viewing angles on the structure, simulating different lineofsight configurations. Denoting by θ the angle between the lineofsight and the perpendicular to the axis of the cylinder, we consider the cases: θ = 0°,30°,45°,60°, shown in Fig. 1. For each lineofsight, we define rays 1 and 2 as two particular rays crossing the cylinder at a node and an antinode of the radial velocity, respectively (unless stated otherwise, the terms “node” and “antinode” will refer to the radial velocity amplitude throughout the manuscript). For simulating observations it is also important to consider spatial, temporal, and spectral resolution of the instrument at hand. For each ray we consider four different resolution “pixels”: “0R” (0 radius, equal to the spatial resolution of our model, i.e. 25 km), “1R” (1 radius ≈1/3ℓ, where ℓ is the wavelength of the mode in the base model), “2R” (2 radii ≈2/3ℓ), and “3R” (≈ℓ). These pixel sizes correspond to the dotted squares in Fig. 1. A pixel of 1 R would correspond roughly to the size of the instrumental PSF for the 171 and 193 channels of the AIA instrument of SDO (Grigris et al. 2012, AIA Team Online Document). Considering that the timescale of the sausage mode in a coronal structure such as this one is of the order of seconds (the period P of the mode in the base model is about 5 s), which is very low compared to the current cadence of available instruments (at most 1 s for imaging instruments, in general 12 s), we consider the following temporal resolutions: “0s” (equal to the temporal resolution in our model, i.e. 0.15 s), “1 s” (≃P/5), and “2 s” (≃3P/7). The spectral resolution in our numerical model is set at 1.4 mÅ for the Fe ix 171 line and 1 mÅ for the Fe xii 193 line, leading to a spectral sampling of 48 points across 99% of the spectrum (details about the selected lines are given below). We also consider coarser spectral resolutions of Δλ = 4.2 mÅ and Δλ = 8.5 mÅ, leading to samplings of 16 and 8 points, respectively.
The quantity that we are mostly interested in synthesising is the specific intensity for optically thin (coronal) plasma along a given lineofsight: (13)where A_{b} is the (coronal) abundance of the element (denoted by its wavelength at line centre λ_{0}) relative to hydrogen, g_{eff} is the Gaunt factor, f_{λ0} is the oscillator strength of the line, G_{λ0}(T,n_{e}) is mostly a temperaturedependent function characterising the response of the plasma for that particular line, n_{e} is the electron number density, and the integral is evaluated along a ray crossing the emitting plasma (dl is an element of length along the lineofsight). The G_{λ0}(T,n_{e}) function depends mainly on the ion population fraction, which can be obtained by solving the timedependent ion balance equations. While such a treatment would provide a thorough analysis of the radiative response of the plasma, it would take us beyond the scope of this paper (as followed by, e.g. Bradshaw & Mason 2003). Here, we assume that the plasma is at all times in equilibrium ionisation, and we estimate the effects of nonequilibrium on the observable quantities.
The purpose of this work is not to determine the absolute value of line intensities exactly, but rather to analyse the effect on the intensities from temperature, density and especially the geometry (the lineofsight rays). We therefore concentrate here on the quantities that compose the integrand in Eq. (13). The calculation of the integral in Eq. (13) for all rays crossing the domain is a computationally expensive procedure that can be considerably sped up with the following techniques. For calculating G_{λ0}(T,n_{e}), we produce a lookup table that depends on temperature and density using the CHIANTI atomic database (Dere et al. 1997, 2009). For the latter we choose the chianti collisional ionisation equilibria file (chianti.ioneq) and coronal abundances (sun_coronal.abund file, from Feldman 1992). The lookup table is composed of a 2000 × 100 points uniform sampling in the electron number density n_{e} − temperature T domain (respectively), where log n_{e} ∈ [8,10] and log T ∈ [4.95,6.5], which covers the values obtained in our numerical model. Since the G function mostly depends upon temperature, the values of the table are only interpolated to the temperature values of each pixel in our model. We produce histograms of the lineofsight velocity choosing a bin size of 0.5 km s^{1} (much smaller than the plasma motions produced by the perturbation) and work with the resulting bins instead of pixelbypixel. For each resulting bin we produce a second histogram of the emissivity with the data points within the bin. Thanks to the symmetry in our model the bin number necessary for high accuracy for this second histogram is lower than 10 000. The spectral line is then calculated for each emissivity bin by assuming a Gaussian distribution for the plasma. The maximum of the Gaussian is given by the value of the emissivity bin. The width of the Gaussian is set by the thermal broadening, given by the logarithmic average temperature of the pixels within the emissivity bin. The displacement of the Gaussian’s centre is set by the bin value of the velocity histogram. The last step consists in integrating along the lineofsight the Dopplershifted emission. This involves an interpolation from the values of the cartesian grid of the Dopplershifted emission to equally spaced points along the lineofsight rays. With the outlined method the calculation time of the synthetic spectrum for one line for four different lineofsight angles is eight to ten times faster than with a normal pixelbypixel method.
Fig. 2 Same as Fig. 1 but for the long λ model. See Sect. 2.4 for more details. 

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2.4. Models
The modulation of the intensity due to the sausage mode is analysed in several models which differ in 1 specific way from our base model.

The “base model − 171” – We analyse the modulation in intensityfor our base model in the transition region lineFe ix 171.073 Å, which has a formation temperature at log T = 5.9 K.

The “base model − 193” – We analyse the modulation in intensity for our base model in the coronal line Fe xii 193.509 Å, which has a formation temperature at log T = 6.1 K.

The “highT model” – The effects of high external temperature are analysed in this model. We use an external temperature of 8 × 10^{5} K, which results in a slightly higher internal density, with a mean value at the antinode of 5.5 × 10^{12} kg m^{3} and a variation around this value of roughly 7%.

The “long λ model” – Keeping the same values of internal and external thermodynamic quantities for the unperturbed cylinder (base model), here we model the longest possible wavelength for a nonleaky sausage mode for these conditions: ≈5 Mm, which results in a wavenumber of kR = 1.25. Figure 2 shows a snapshot of a cut along the middle axis of the cylinder for the radial and longitudinal velocities, density, and temperature for this case. The snapshot is taken at onethird of the period, which in this case is 5.8 s. For this model two wavelengths in the z direction are enough to cover the lineofsight rays, giving N_{z} = 408 grid points. The density and temperature have roughly the same average values as before but now exhibit slightly larger variations at the antinodes, about 8.5% and 6%, respectively. The radial and longitudinal velocities now have maxima at 23 km s^{1} and 3 km s^{1}.
Fig. 3 Integrated intensity along the lineofsight for the base model − 171, at the four different angles considered: 0°,30°,45°, and 60° (see Sect. 2.4 for more details). The snapshot is taken at onethird of the mode period. The crosses in each panel denote the location of the 2 lineofsight rays defined in Sect. 2.3. In each panel, the left and right crosses correspond to the rays crossing a node and an antinode of the oscillation. 

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3. Results
Since the aim of this work is to identify the observational signatures of the sausage mode in coronal structures, we present the results of our models as they would be perceived by the instruments at hand. We therefore divide the results into two relevant categories depending on the instrument: imaging and spectroscopic.
3.1. For imaging instruments
Figure 3 shows the integrated intensity for the base model − 171 (corresponding to the ten times higher spatial resolution model), obtained by integrating the intensity in Eq. (13) over the full Fe ix 171 Å line, for the four lineofsight angles: 0°,30°,45°, and 60°. The crosses in the centre of each panel show the location of rays 1 and 2 crossing the cylinder defined in Sect. 2.3. The snapshot is taken at onethird of the period, coinciding with that of Fig. 1.
One of the main features of this figure is the absence of significant intensity structuring along the cylinder, in sharp contrast to the density or temperature maps shown in Fig. 1. The intensity pattern matches the radial expansion of the cylinder, which is barely discernible, equal to only one pixel in the lowresolution model (25 km). We thus have a longitudinal structuring in intensity qualitatively similar to the longitudinal structure of the radial velocity. On the other hand, unlike what would be expected if the intensity is assumed to be proportional to the density squared, the regions of increased intensity correspond to regions of low density at the centre of the cylinder. This is because the Fe ix 171 Å line has a formation temperature at log T = 5.9, and the sausage mode is only slightly compressible in the corona, producing temperatures in our cylinder that oscillate between log T = 5.99 and log T = 6.04. Therefore, a drop in temperature in our model leads to an increase in the fraction of the Fe ix population, thus increasing the emission, as can be seen in Fig. 6. On the other hand, as shown in Fig. 6, the Fe xii 193 Å line has a formation temperature at log T = 6.2 K. In this case, higher temperature implies an increase in the ion population, leading to higher intensity and thus creating a structure that is similar to the temperature or density structure, as can be seen in the base model − 193 shown by Fig. 4. This effect is further reinforced because at 0° viewing angle, the rays crossing these regions will cross more material since they only correspond to regions of contraction (higher density). This fact highlights the dominant role of the contribution function G_{λ0}(T,n_{e}) in the formation of the emergent intensity. It is important to remind the reader that these results are subject to the assumption of equilibrium ionisation, and therefore that the plasma responds instantaneously to the changes in temperature and density from the MHD mode. The limitations of this assumption will be discussed at the end of this section.
Fig. 4 Same as Fig. 3 but for the base model − 193 (see Sect. 2.4 for more details). The pixel sizes corresponding to 1R, 2R and 3R are shown around the location of ray 2 (antinode). 

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Figure 5 shows the evolution of the integrated intensity along the lineofsight at an angle of 0° for the base model − 171 (left panels) and the base model − 193 (right panels), for rays 1 (top panels) and 2 (bottom panels) crossing at a node and an antinode of the oscillation, respectively. Any other location along the axis of the cylinder displays features similar to either ray 1 or ray 2. For each ray different spatial resolution pixels are taken (see figure for details). In the case of the base model − 171 we have a very low modulation of the intensity, as compared to the density modulation at the centre of the cylinder. While the latter varies by ≲7%, the intensity varies by ≲2% at an antinode and is basically negligible at the location of a node. Furthermore, as explained earlier, the variation in the intensity is in antiphase with that of the density because the contribution function G_{171}(T,n_{e}) has a peak at lower temperature values than those of the plasma in the cylinder. The slightly longer column thickness created by the area expansion creates the slight asymmetry between the two dips in the intensity cycle.
Fig. 5 Integrated intensity along the lineofsight (normalised with respect to the equilibrium value) for the 0° angle case for the base model − 171 (left panels) and the base model − 193 (right panels) for two specific rays: ray 1 crossing a node (top most panels) and ray 2 crossing an antinode (bottom panels), shown with crosses in Figs. 3 and 4. Different colours denote different pixel sizes: 0R,1R,2R, and 3R in red, purple, blue, and green, respectively, where R = 1 Mm ≈ ℓ denotes the radius of the cylinder and 0R denotes the spatial resolution in the high resolution model: 2.5 km. The black curve denotes the density profile at the centre of the cylinder and the same location along the axis of the cylinder as rays 1 and 2. The intensity range of the top panels is set significantly narrower than that of the bottom panels in order to show the low intensity modulation at the nodes. 

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This scenario is in sharp contrast with that of the base model  193, shown in the righthand panels of Fig. 5. The G_{193}(T,n_{e}) function presents a peak at a higher temperature value than that of the plasma inside the cylinder. In this case we thus have inphase intensity variations with the density (or temperature) profile. Also, as shown in Fig. 6, the G_{193}(T,n_{e}) contribution function is significantly more sensitive to the temperature changes inside the cylinder than the G_{171}(T,n_{e}) function, leading to intensity variations of ≃35%. The difference in intensity from the initial value is greater for the maximum values than the minimum values. This is because the gradient of the G_{λ0}(T,n_{e}) function is steeper for both 171 and 193 above its initial value (mainly in the direction of higher temperature) than below the initial value. This effect is further amplified by the density enhancement at a time of contraction, since each pixel along the lineofsight contributes with the square of the local density value. We further notice two small bumps for ray 1 at times of density extrema when considering pixel sizes different from 0R. These are again due to the combined effect of the steepness of the G_{λ0}(T,n_{e}) gradient and enhanced density in regions of contraction, which are within the lineofsight for coarse pixel sizes.
The variation in the intensity decreases significantly with the pixel size for all models, especially at antinode locations when viewing at a 0° lineofsight angle. In the considered models the intensity variation is reduced by factors of 10−17 when increasing the pixel size to 3R. This is expected since a larger pixel size implies a higher probability of crossing mixed regions of expansion and contraction. For the models with a wavenumber ka = 2.24, the unit of the pixel is slightly larger than onethird of the wavelength, and therefore three pixel units (≃3R) not only covers the entire region of expansion and contraction, but also produces a slight imbalance between the two, as can be seen in Figs. 3 and 4. At a time of contraction the pixel will therefore cover slightly more expanding material, and viceversa, resulting in a reversal of the variation in intensity at antinode locations (ray 2). This can be seen in Fig. 5 for both models, 171 and 193. However, in this case, most of the longitudinal intensity structuring is erased, and with it the difference between the 171 and the 193 line intensity variation. Furthermore, if our pixel is centred on a node, regardless of the size of the pixel, the amount of expansion and contraction will always be similar, thus producing minimal intensity variation. As can be seen in the top righthand panel of Fig. 5, this variation attains a maximum for a 2R pixel size, which is linked to the fact that the amount of material entering and leaving the lineofsight is close to a maximum for this size. This of course depends on the shape of the pixel, which in our case is a square.
Fig. 6 Contribution function G_{λ0}(T,n_{e}) for Fe ix 171 and Fe xii 193. The maximum formation temperature for these ions are, respectively, log T = 5.9 and log T = 6.2 K. The black parallelogram in each surface has its corners defined by the minimum and maximum temperature and density values found in the base model, and therefore includes the G_{λ0}(T,n_{e}) values used here. The temperature range in the upper panel has been inverted in order to show the parallelogram for the G_{171}(T,n_{e}) surface. 

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Fig. 7 Comparison between an intensity calculated as I ≈ ρ^{2}l, where l is the column thickness along the lineofsight (solid), the base model − 171 intensity I_{171}(t) (dotted), and the base model − 193 intensity I_{193}(t) (dashed) for a viewing angle of 0° and a pixel size resolution of 0R for ray 2. The differences between the lines illustrates the importance of the G_{λ0}(T,n_{e}) function. 

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Fig. 8 Same as the right panel of Fig. 5 but fixing the pixel size resolution to 0R and varying the angle of the lineofsight for the base model − 193. 0°,30°,45°, and 60° correspond to the red, purple, blue, and green curves, respectively. 

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Fig. 9 Time variation of the specific intensity I_{λ} integrated along ray 1 (left panels) and ray 2 (right panels) for the base model − 171 when viewing at an angle of 0° and for a pixel size of 0R (upper panels) and 2R (lower panels). Contours of the intensity are also shown for better visualisation of the variation. 

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Fig. 10 Same as Fig. 9 but for a lineofsight crossing the cylinder at an angle of 45°. 

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As explained in the introduction, a common approximation to the intensity calculation is I ≈ ρ^{2}l, where l is the column thickness along the lineofsight. In Fig. 7 we compare this approach to the outcomes of the more proper intensity calculation performed in this work, plotting ρ^{2}l and the results from the base model − 171 and base model − 193. To clearly show the difference we plot the case of a 0° viewing angle and a pixel size resolution of 0R for ray 2 (antinode). By following the I ≈ ρ^{2}l approximation, we find maximum intensity variations below 3%, which match those obtained with the 171 line. However, both profiles are in antiphase with each other because the Fe ix ion population decreases with increasing temperature for the range of temperatures considered here. The discrepancy in amplitude with the 193 line intensity is obvious. This illustrates the important role of the contribution function G_{λ0}(T,n_{e}) in the formation of the emergent intensity.
The variation in the integrated intensity due to different lineofsight angles is shown in Fig. 8. To show the variation best we fix the pixel size resolution at 0R and consider the base model − 193, for which large intensity variation is found for the temperature and density variations created by the sausage mode. By increasing the lineofsight angle, the rays cross more regions of hot (contraction) and cold (expansion) plasma, thus reducing the variation in the intensity by a factor of 2.5 (down to ~10%). For rays crossing nodes (ray 1), as discussed previously, the variation is greatly reduced from the crossing of mixed temperature regions in equal quantities along the rays. As in Fig. 5 (right panel), two small bumps can be seen for nonzero viewing angles produced by the combined effect of the local gradient steepness of the G_{λ0}(T,n_{e}) function and the regions of enhanced density along the lineofsights.
Apart from the two models discussed in this section, the other models exhibit the same behaviour as that of the base model − 171, with minor quantitative differences. The main differences are discussed in Sect. 3.4.
Nonequilibrium ionisation effects
Perhaps the most important assumption in the intensity modulation presented here is to consider that the plasma is at all times in equilibrium ionisation, i.e. that the plasma response to the temperature and density changes produced by the MHD mode is instantaneous. However, this is never the case and significant departures from equilibrium can occur on timescales that can be shorter than the timescale of the driver (De Moortel & Bradshaw 2008). The population densities of the ions in the plasma will vary according to the ionisation and recombination rates, which depend on the thermodynamic conditions at each specific moment of time. The rigorous solution to this problem involves solving the timedependent ion balance equations, which would take us outside the scope of this paper. However, we can estimate the consequences of nonequilibrium ionisation on the emergent intensity. For this we assume that the plasma follows a Maxwellian distribution at all times. Timescales for ionisation and recombination equilibrium for the ions Fe ix and Fe xii can then be obtained through CHIANTI. These values are shown in Table 1 (in the case of a κdistribution, as shown by Dzifčáková 2002, the rates would increase leading to smaller timescales than those presented here).
For Fe ix we can see that the ionisation and recombination timescales for reaching equilibrium are of the order of 2 s, which is almost half the period of the sausage mode. This means that at a time of expansion (cooling) the material will have just started being ionised and will therefore start recombining without attaining full ionisation. We therefore have a time lag effect and an attenuation (and deformation) of the intensity profile. The loss in amplitude will be similar to what is obtained when integrating the profile over a period of 2 s, in which case the intensity is reduced by a factor of roughly 1.5. This effect is shown in Fig. 13. For Fe xii the ionisation and recombination timescales are between 13 s and 20 s, that is, considerably larger than the period of our mode. In this case, there would basically be no modulation of intensity.
Nonequilibrium ionisation effects would, however, have no influence on the spectrometric results presented in Sect. 3.2. Indeed, as we see in the next section, most of the spectral broadening has a turbulent nature and is not of thermal origin.
3.2. For spectroscopic instruments
We now analyse the spectral variation caused by the sausage mode, which is of interest for observations performed by spectroscopic instruments. For this we concentrate on rays 1 and 2 alone, simulating slits that would cross the cylinder at a perpendicular angle, centred on a node or an antinode, respectively. All other positions along the cylinder present features similar to either ray 1 or ray 2.
Figures 9 and 10 show the time variation of the specific intensity I_{λ} for the base model − 171 for the lineofsight angles of 0° and 45°, respectively. The cases of 0R and 2R pixel size resolution for ray 1 (node) and ray 2 (antinode) are shown. For the 0° angle and 2R pixel size case we have periodic spectral broadening for rays crossing the cylinder at any location, especially clear for the 0R pixel size case of ray 2. This feature is only absent for the case of ray 1 with 0R pixel size. This is expected since for the latter the pixel size does not include any ray crossing a region of expansion or contraction, in contrast to all the other cases. When watching at an angle, rays will cross regions of expansion and contraction by different amounts when the slit is centred on a node, and in equal amounts when centred on an antinode. This creates an asymmetry for the former, hence an overall dominating redshift or blueshift. This translates into clear periodic blueshift or redshift excursions for the 0R pixel size case of ray 1 (left upper panel of Fig. 10), but hardly discernible for the 2R pixel size case (lower left panel). As expected, the periodic broadening is also present for this viewing angle for any pixel size.
The pixel size resolution dependence of the time variation of the specific intensity I_{λ} observed in Figs. 9 and 10 is shown in the lefthand panels of Fig. 11 for the 0° angle case. In these panels we show the result of Gaussian fits to the specific intensity I_{λ}(t) for all the considered pixel sizes. The time variation of the Doppler velocity, width of the Gaussian fit, and the goodnessoffit χ^{2} statistic are shown from top to bottom in the first three panels for ray 1 and the last three panels for ray 2. Since the 0° angle case is considered and the sausage mode is mainly a radial mode, negligible Doppler velocity results from the Gaussian fit for any pixel size resolution. On the other hand, the line width and the nonGaussianity χ^{2} parameter present significant variation, and have profiles that are in phase with the square of the radial velocity. This means that they both have a double periodicity. Maximum variations close to 20% and 50% are obtained for the line width, respectively for rays 1 and 2. For the case of ray 1 (ray 2) the spectral line broadening increases (decreases) for pixel sizes up to 2R. For 3R, which corresponds to one wavelength, and therefore an equal amount of expanding and contracting gas, the broadening is reduced (increased) for ray 1 (ray 2). The decreasing factors range between 2.5 and 3.4 between the models. The temperature (or density) modulation by the sausage mode contributes to a certain extent to the nonGaussianity of the line profile. This is especially the case for large pixel sizes (≳2R), for which the contribution from the radial velocity is lowest due to the wide range of velocities included, producing a broad Gaussianlike profile. This can be seen in the χ^{2} profiles as a bump at times of maximum and minimum densities at the centre of the cylinder. These bumps are similar to the perturbations created by the radial velocities, and therefore can give an observer the impression of a quadruple periodicity for the χ^{2} parameter (period of P/4 where P is the period of the sausage mode).
Fig. 11 Left panel: pixel size resolution dependence of the time variation of the specific intensity I_{λ} for the 0° angle case of the base model − 171. From top to bottom we show quantities ensuing from a Gaussian fit to the spectral line. The first 3 upper panels correspond to the Doppler velocity, the line width and the goodnessoffit χ^{2} parameter for the case of ray 1 (node). The 3 lower panels show the same quantities for the case of ray 2 (antinode). Different line styles correspond to different pixel size resolution: 0R (solid), 1R (dotted), 2R (dashed), 3R (dotdashed). The line width is normalised with respect to the initial value at time t = 0. The unit for the χ^{2} parameter is the logarithm of the normalised value, where the normalisation factor is the equilibrium value. Right panel: angle dependence of the time variation of the specific intensity I_{λ} for the 0R pixel size case of the base model − 171. The arrangement of these panels is the same as for the left panels. Different line styles denote different lineofsight angles: 0° (solid), 30° (dotted), 45° (dashed), 60° (dotdashed). For both left and right panels the variation in time of density (red curve) and radial velocity (blue curve) at the centre of the tube is plotted for reference in arbitrary units in the Doppler velocity panel. 

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The angle dependence of the time variation of the specific intensity I_{λ} for rays 1 and 2 is shown in the righthand panels of Fig. 11 for the 0R pixel size resolution case of the base model − 171. For nonzero viewing angles the rays now cross both regions of expansion and contraction. The Doppler velocity values ensuing from the Gaussian fits are therefore the emission measure weighted averages over these regions. A small contribution also comes from the longitudinal velocity component, but it is one order of magnitude smaller than the transverse velocity component. As observed in Fig. 10, depending on the lineofsight angle one can at any given time have either a dominating blueshift (30° and 45°) or redshift (60°). The variations in spectral line broadening given by the line width and the χ^{2} parameter decrease significantly with the angle when crossing an antinode (with maximum factors for line width between 5.6 and 11.3 between the models). On the other hand, rays crossing a node have slightly increasing variations in spectral line broadening with angle (below 10%). The maximum velocity component is directed perpendicularly to the cylinder axis. The components creating the width of the spectral line therefore decrease with the sine of the lineofsight angle. The contribution to the nonGaussianity of the line from the temperature and density profiles can also be observed at various angles. The bumps in the χ^{2} parameter profile created at times of maximum or minimum temperature (and density) at the centre of the cylinder are close to the perturbation created by the radial motions for any angle in the case of ray 1 and for angles ≳45° for ray 2.
To estimate the respective contribution from turbulence (unresolved velocity perturbations) and temperature to the broadening, we plot in Fig. 12 the time variation of two Gaussian widths obtained from rays 1 and 2 with a viewing angle of 0° and a pixel size of 0R. The Gaussian width corresponding to the thermal broadening contribution is obtained from the average of temperature for the pixels along the lineofsight crossing the cylinder. The Gaussian width corresponding to the turbulent broadening contribution is obtained from a Gaussian fit to the sum of multiple Gaussians, one for each pixel in the cylinder along the lineofsight, with a fixed temporal averaged thermal broadening and shifted centre given by the lineofsight velocity at that pixel. We can see that the turbulent broadening is the main contributor to the spectral line broadening. Only for cases of little plasma motion along the lineofsight (0° angle and 0R pixel size, or at times of 0 radial velocity) is the thermal broadening comparable to the turbulent broadening.
3.3. Effects of temporal and wavelength resolutions
In Sect. 3.1 we discussed the effects of nonionisation equilibrium, and in the last section we showed the effects of spatial resolution and lineofsight angle on the detection of intensity modulation by the sausage mode. In this section we would like to present the main effects of temporal and wavelength resolutions. The temporal and wavelength resolutions of our base model are, respectively, 0.15 s and 1.4 mÅ. Here we discuss the differences introduced by taking temporal resolutions of 1 s and 2 s (0.15 s, 1 s, and 2 s correspond, respectively, to 3%, 22%, and 44% of the mode period), and wavelength resolutions of 4.2 mÅ and 8.5 mÅ (1.4 mÅ, 4.2 mÅ, and 8.5 mÅ correspond, respectively, to 48, 16, and 8 points sampling of the spectral line).
Estimates of timescales for ionisation (I) and recombination (R) equilibrium for Fe ix and Fe xii inside the model.
Fig. 12 Estimation of the spectral line broadening contribution from the unresolved velocity perturbations (which we denote as turbulence) and temperature perturbations. The Gaussian width corresponding to the thermal broadening contribution (dashed curve) is obtained from the average of temperature for the pixels along the lineofsight crossing the cylinder. The Gaussian width corresponding to the turbulent broadening contribution (solid lines) is obtained from a Gaussian fit to the sum of multiple Gaussians, one for each pixel in the cylinder along the lineofsight, with a fixed temporal averaged thermal broadening and shifted centre given by the lineofsight velocity at that pixel. 

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Fig. 13 Effects of the temporal resolution on the modulation of observable quantities. We take the base model − 193, fix the pixel size resolution to 0R and consider cadences of “0s” (=0.15 s, solid curve), “1s” (=1 s) ≃P/5 (dotted curve), and “2s” (=2 s) ≃ 3P/7 (dashed curve), where P ≃ 4.5 s is the period of the mode. The upper panel shows the temporal evolution of the normalised integrated intensity along the lineofsight for ray 2 taking a viewing angle of 0°. The rest of the panels, respectively from top to bottom, show the temporal evolution of the Doppler velocity, the line width and (logarithm of) the χ^{2} nonGaussianity parameter resulting from Gaussian fits to the specific intensity profile I_{λ}(t) for the different temporal resolutions. In order to show best the effects on the Doppler velocity, only for this quantity we take the case of ray 1 with a viewing angle of 45°. The normalisation factor for the line width is the initial value at time t = 0 for the 0s temporal resolution. That of the χ^{2} parameter is the time average value of the profile for ray 1 for 0s temporal resolution. 

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Fig. 14 Temporal evolution of the Doppler velocity (upper panel), the line width (centre panel) and (logarithm of) the χ^{2} nonGaussianity parameter (lower panel) resulting from Gaussian fits to the specific intensity profile I_{λ}(t) obtained from the base model − 193, for different wavelength resolutions. We consider samplings of 1.4 mÅ (solid curve), 4.2 mÅ (dotted curve) and 8.5 mÅ, leading to 48, 16 and 8 points along the spectral line, respectively. In order to show best the effects of the wavelength we fix the pixel size resolution to 0R and show the case of ray 1 with a viewing angle of 45° for the top panel and the case of ray 2 with a viewing angle of 0° for the middle and bottom panels. The normalisation values are the same as in Fig. 13. 

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Figure 13 shows the effect of temporal resolution on the integrated intensity and spectral broadening obtained from the modulation by the sausage mode for the base model − 193. We choose a viewing angle of 0° and ray 2 (antinode), for which the effects are strongest for the integrated intensity (top panel), line width (third panel from top to bottom), and χ^{2} parameter (bottom panel), and a viewing angle of 45° and ray 1 (node) for the Doppler velocity (second panel from top to bottom). We also fix the spatial resolution to 0R. Different temporal resolutions are obtained by integrating the intensity profiles over temporal windows corresponding to the designated resolution. Since the period of the sausage mode is about 4.5 s, only a few points of the full profile are obtained per period. To obtain full period profiles, approximately 7 and 13 periods are needed, respectively, for 1 s and 2 s resolutions. Longer time integrations also generate phase differences between the profiles equal to the resolutions of each profile. We choose, however, to correct for this effect and present the shifted profiles in Fig. 13 in order to facilitate comparison.
As seen in the top panel of Fig. 13, the intensity variation from the sausage mode decreases with temporal resolution. Factors ranging from 1.2 to 1.5 were found among the models. Although this effect may not appear as important for strong intensity variations as those obtained for the base model − 193, they are especially relevant for low intensity variations, such as those obtained in the base model − 171. Longitudinal variation can therefore be erased in this case.
In the lower 3 panels of Fig. 13 we show the effects of temporal resolution on the Doppler velocity, the line width and the χ^{2} nonGaussianity parameter obtained from the Gaussian fits to the specific intensity profiles I_{λ}(t). As being the displacement of the bulk of the plasma along the lineofsight, the Doppler velocity is the least affected quantity, with maxima decreasing from 7 km s^{1} to ≲5 km s^{1} (decreasing factors between 1.1 to 1.5 among the models). On the other hand, the strength of the spectral broadening depends mostly on the fast components of the plasma. Correspondingly, the line width variations of about 40% obtained in the model are reduced to 30% and <10% for time cadences of 1 s and 2 s, respectively, compromising its detectability with the current instruments. Accordingly, decreasing factors between 4.6 and 6.3 are found between the models. Similarly, the variation in the χ^{2} parameter is reduced (spectra become more and less Gaussian at times of expansion and compression, respectively), especially in the 2 s cadence case, where it is reduced by several orders of magnitude. For the 2 s time cadence, therefore, the spectral line is seen as a profile with almost constant shape and the width roughly equal to the average width of the true profile, but for which bulk Doppler motions can still be observed.
Fig. 15 Model comparison of the temporal variation of the spectral line broadening. The line width (upper panels) and (logarithm of) the nonGaussianity χ^{2} parameter (lower panels) resulting from the Gaussian fits to the specific intensity I_{λ}(t) for the 0R pixel size case are presented. From left to right the first two panels correspond to rays 1 and 2 for the 0° angle case. The last two panels correspond to rays 1 and 2 for the 45° angle case. Different line styles denote the different models studied in this work, as indicated in the legend. The normalisation values are the time averages of the corresponding quantities for ray 1 and 0° viewing angle. 

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The effects of wavelength resolution on the spectral broadening of the specific intensity profile I_{λ}(t) for the base model − 193 are shown in Fig. 14. As for Fig. 13, here we show the case of ray 1 (node) with a viewing angle of 45° for the Doppler velocity and the case of ray 2 (antinode) with a viewing angle of 0° for the line width and the χ^{2} parameter. We fix the spatial resolution to 0R. Different spectral resolutions are produced by integrating the (high wavelength resolution) intensities over specific wavelength bins. We can see that no changes are produced in the Doppler velocity. This is due to the lack of asymmetries in our model: regardless of the nonGaussianity of the profiles, they will always be symmetric (with respect to the wavelength corresponding to the bulk velocity of the plasma). The effects on the line width are also minimal, with slightly increasing factors between 1.04 and 1.09 among the models. This increase is due to the wider wavelength bins over which intensity is added. At lower resolution the bumps created by the density profile cannot be detected, therefore increasing the Gaussianity of the profile. Factors of increase range between 1.20 and 1.23 between the models.
3.4. Differences between models
The results presented in the previous section apply in a qualitative manner to all the models presented in this paper. Apart from the differences in the integrated intensity between the 171 Å line (base model − 171) and the 193 Å line (base model − 193) treated in Sect. 3.1, differences between spectral broadening of the different models were also briefly stated in Sects. 3.2 and 3.3.
Figure 15 shows the time evolution of the spectral line broadening (the line width and the nonGaussianity χ^{2} parameter) resulting from the Gaussian fit to the specific intensity I_{λ} for all the models presented in this study, taking 0R as fixed pixel size. From left to right the first two panels correspond to the 0° angle case, for rays 1 and 2. The last two panels correspond to the 45° angle case for rays 1 and 2. The quantities are normalised with respect to the temporal average of the corresponding quantity for ray 1 with a 0° viewing angle.
As can be seen in the panels containing the line profile width all models except the long λ model have essentially the same variation. This is mainly because the same velocity field is achieved for the same wave number. Longer wavelengths (small wave number) produces higher velocity fields, leading to larger variations in line widths. Higher velocities also lead to stronger compression and rarefaction, hence greater variation in temperatures and densities. The effects on the spectral broadening of the line are low, however, since plasmas with a hotter temperature produce lower intensities in the 171 Å line. The longer wavelengths produce wider regions of compression and rarefaction, thus modifying the emission crossed by rays 1 and 2 between the models. This can be observed in the 45° angle case for ray 2, leading to stronger variation in line widths and χ^{2} values. This effect disappears for a viewing angle of 60°, where ray 2 crosses mixed regions. On the other hand, the high T model shows in general the lowest values in line width and χ^{2} parameter values (within models with same wave number especially). This is due to the hot plasma component at rest outside the cylinder. Only minimal differences occur between the base model − 171 and base model − 193. This is because the emission measure weighted radial velocities are very similar between the two models.
Influence of lineofsight angle, and spatial, temporal, and wavelength resolution on the modulation of observable quantities caused by the sausage mode.
4. Discussion
4.1. Intensity modulation
Table 2 summarizes the main findings of this work. These results have been obtained assuming equilibrium ionisation for the considered ions, and should be discussed taking this assumption into account. As discussed in Sect. 3.1, based on the results in Table 1, in the case of a Maxwellian plasma distribution nonequilibrium ionisation severely affects the modulation of intensity, but does not alter the results obtained for the modulation of spectral line shape (width and Gaussianity). The results for intensity presented in Table 2 and discussed in this section therefore constitute upper limits to the more realistic case of plasma modulation in a simulation where the ion balance equations are solved.
The modulation of the integrated intensity, especially important for imaging instruments, severely depends on the selected spectral line(s) of the observation. In the case of a coronal line formed at temperatures below those present in the structure, such as the 171 Å line for the base model − 171, the intensity is only lightly modulated by the sausage mode, even when increasing the mode’s wavelength, with maximum amplitudes of two to four percent. Such models present intensity variations in antiphase with the temperature and density variation, due to the negative slope of the ion population function at these temperatures. However, the modulation can be increased by a factor of 10−15 when considering coronal lines with formation temperature higher than that of the plasma, as is the case for the base model − 193. In this case we have an inphase variation between these quantities.
In our model the intensity is governed by the ion population fraction rather than the density of emitting ions. Indeed, as shown by Fig. 6, the change in the contribution function from the temperature modulation (at average density) is one order of magnitude greater than the change from the density modulation (at average temperature). This implies that nonequilibrium ionisation effects will be important, especially for Fe xii, in which the modulation of intensity would completely disappear for the short timescales of the sausage mode (as discussed in Sect. 3.1). The important role of the contribution functions of spectral lines, especially concerning nonequilibrium ionisation effects, have been discussed by De Moortel & Bradshaw (2008). Through synthetic intensity modelling of TRACE channels, the authors show similar results as those stated above. They further show that double periodicities can be obtained from the shape of the response function of the instrument due to perturbations leading to temperatures that drift in and out of the maximum formation temperature of the line.
Variation in the modulation of the intensity by kink and sausage modes due to variation in the angle between the lineofsight and the emitting structure were first treated analytically by Cooper et al. (2003a,b). Considering the effect of curvature they showed that propagating kink and sausage modes could produce an increase in intensity along part of the loop, such as observed by Williams et al. (2001, 2002). In their work the intensities are approximated by the lineofsight column thickness l and the density ρ, as I ≈ ρ^{2}l. As discussed in Sect. 3.1, the neglect of the contribution function can be misleading, and the variation in line intensities can be severely underestimated. In the present work we have monotonically decreasing dependence on the lineofsight angle for the range of parameters considered here, matching the results of Cooper et al. (2003a). In Cooper et al. (2003b) the case of a smooth density profile is considered (with the corresponding dispersion relations associated with that profile), which introduces an optimal angle for which the intensity variations are largest. This is because the MHD modes in a 2D model are more compressive, and therefore produce significant density variations outside the cylinder. This effect is, however, severely reduced for 3D geometries, as shown by Luna et al. (2008), suggesting that the existence of an optimal angle could be debated. The effect of such density profiles in a 3D model, such as the one considered here, is the subject of future research.
Gruszecki et al. (2012) have performed 3D numerical simulations of (trapped and leaky) sausage modes oscillating in a cylinder with a smooth density profile and analysed the modulation on the integrated intensity. As in Cooper et al. (2003a), the intensity is approximated by integrating the density squared along the lineofsight (for a viewing angle of 0°), but they further consider the pixel size resolution. With the same amplitude as used in this work they find intensity variations of the order of 2% with 0R pixel size resolution, which are strongly reduced by a factor of roughly 15 when increasing the pixel size to 3R (one wavelength), thus matching the results presented here. As can be seen in the table, among all parameters, we find the pixel size resolution to play a dominant role. A pixel size resolution roughly the same as wavelength erases the longitudinal structuring in all models.
The sausage mode in the corona oscillates with relatively short periods. Indeed, in the nonleaky regime and for lowβ plasma conditions, the period of an MHD sausage mode can be shown to satisfy the relation , where j_{0} ≈ 2.4 is the first zero of the Bessel function J_{0}(x) (Nakariakov et al. 2003; Kopylova et al. 2007). In our models, the periods oscillate around 5 s, making the cadence of the instrument a very important parameter. Intensity variations can be decreased by a factor of 1.5 and more than three to five periods of the mode need to be observed in order to half resolve the full profile.
All the interpretations as sausage modes in observations are mostly based on qualitative arguments, especially restricted by the spatial resolutions of the instrument, which in most cases does not allow the longitudinal variation of the oscillations to be investigated in detail along the flaring coronal structure. Still, resolutions such as that of NoRH have allowed the detection of different oscillatory power between loop top and footpoint, and allow more precise identification of the mode harmonics (Nakariakov et al. 2003; Melnikov et al. 2005; Inglis et al. 2008; Inglis & Nakariakov 2009). In these works, the fundamental mode and sometimes the first overtone can be identified. As discussed in Andries et al. (2009), observations of higher overtones are specifically important, since they significantly improve physical parameter estimates from application of MHD seismology. Observations of a fundamental mode at the apex of loops would be comparable to the case of ray 2 in our model, while observations towards the footpoints would correspond better to the case of ray 1. Most observations of sausage modes report short and thick loops, with lengths around 25 Mm. In this case, the resolution of NoRH (5″−10″) corresponds to a pixel size below or , with ℓ_{0} and ℓ_{1} being the wavelengths of the fundamental mode and the first overtone. According to the results presented here a pixel size of reduces the intensity variations by a factor of 30%−40%. For detecting higher harmonics, the pixel size starts to severely decrease the intensity variation, as seen in the lower bottom panel of Fig. 5. Observations of modes with large lineofsight angles with respect to the normal to the loop plane can easily have rays crossing mixed regions of expansion and contraction, corresponding for instance to nodes of the first overtone and the fundamental mode. These scenarios would bring results that are qualitatively similar to those obtained in the present model when varying the lineofsight angle.
4.2. Spectral line broadening modulation
Table 2 especially shows that even when intensity variations are low (as in the base model − 171), spectral line broadening can be important and could therefore be observed by current spectrometers. In Sect. 3.2 we have shown that the nature of the spectral line broadening from the sausage mode is not thermal but mainly turbulent broadening. This implies that nonequilibrium ionisation will not influence the obtained spectrometric results.
The sausage mode is essentially a radial mode, and therefore Doppler motions (through singleGaussian fitting) can only be detected when looking at an angle as shown in Sect. 3.2. In this case, bulk motions can be detected as blueshift and redshift excursions below 7 km s^{1}, roughly onethird of the maximum velocities achieved in the present model. Maximum variations are obtained for 0° viewing angle for the line width and the χ^{2} parameter for ray 2 (antinode), with values close to 50% and 4 orders of magnitude, respectively (see table). As shown in Fig. 11 longitudinal structuring can be detected in Doppler velocity, line width and the χ^{2} parameter for angles up to 30°, pixel size resolutions up to 1R, temporal resolution of 1 s (although with 2 s resolution it is still possible to detect bulk Doppler velocities) and for all considered wavelength resolutions. Furthermore, the line width and χ^{2} parameter present double periodicities. For lower resolutions or higher viewing angle, the χ^{2} parameter presents quadruple periodicity, but in these cases all quantities exhibit variations decreased by factors of 2 to 10 for each parameter, and therefore may become barely detectable.
So far very few reports have existed of periodic spectral broadenings in EUV lines with little or no associated intensity variations interpreted as fast sausage modes. Most of these studies are performed with the Hinode/EIS imaging spectrometer (Culhane et al. 2007), with the 1″ slit (with a pixel size resolution of 2″) and temporal resolutions of the order of 10 s or more. Kitagawa et al. (2010) Fourier analyse EUV intensity, Doppler velocity, and line width time series of data in an active region observed in the Fe xii 195 line. Moss regions were found to exhibit significant correlated intensity and Doppler velocity oscillations, with variations of 0.4% to 5.7% and 0.2 to 1.2 km s^{1} respectively, consistent with fast MHD waves modulation. Depending on the significance level of intensity oscillations to Doppler velocity and line width oscillations, the waves were interpreted as either fast sausage modes, Alfvén, or kink modes. However, our results suggest that a low significant level in intensity can be obtained with a sausage mode (any pixel size resolution for 171 line, 3R pixel size resolution for 193), while keeping a relatively high significant level for Doppler velocities and line width (above 10% variation). The long reported periods of around minutes could be produced by leaky fast sausage modes, especially towards the footpoints of loops, as explained below.
Many reports exist of observations in the same lines having similar attributes, interpreted as slow modes, kink modes, or Alfvén waves (see review by De Moortel & Nakariakov 2012). Although the authors discard the sausage mode interpretation for other reasons, the essential characteristic discarding sausage modes are the long reported periods. Sausage modes with long periods can exist in the corona, as shown by Pascoe et al. (2007b), but are leaky, and therefore their observability is severely limited for ranges matching the reported periods.
Often, observations of propagating disturbances are interpreted as slow modes based on the phase speed closely matching the local sound speed, periods between two and ten min, (low) intensity variations (of a few percent with respect to the background intensity) and the intensity fluctuation lagging the Doppler shifts by a quarter period (Wang et al. 2003). Here we would like to stress that it is the combination of all these characteristics that supports such an interpretation. Apart from the first two, (phase speed and period), a sausage mode can also explain the rest (intensity modulation and phase shift, as obtained when observing with a non 0° angle).
Wavelength resolution is found to play a minor role, compared to spatial and temporal resolutions. As shown in Sect. 3.4 only minor differences appear in the spectral broadening (and none in the Doppler velocity) when decreasing the wavelength resolution to only eight points across the spectrum (Δλ = 8.5 mÅ). This may be due to the symmetric nature of the sausage mode (with respect to the axis of the cylinder), but also to the absence of nonuniformities in density or temperature in the present models. Pascoe et al. (2007a, 2009) have considered the effects of varying loop crosssection and fine multilayered structuring on the resonant periods and the spatial profiles of fast sausage mode oscillations. These numerical studies find that the resonant properties of longwavelength sausage standing modes of the slab are not sensitive to the details of fine structuring, and the spatial profiles are only weakly affected by the crosssection inhomogeneity. This suggests that the inherent symmetries of the fast sausage mode are rather robust to loop divergence and internal density finestructuring and, therefore, that the properties of the modulation found for simple cylindrical geometries, such as those used here, are robust as well.
As discussed in the previous section, the detection of sausage modes is severely limited by its leaky nature in most coronal conditions. On the other hand, the lack of reported observations of sausage modes with spectrometers may also be due to an instrumental reason. Our results show that high spatial and temporal resolution in EUV lines is essential for the detection of such waves. Perhaps the most promising instrument for detecting these waves in the near future is the Interface Region Imaging Spectrograph (IRIS), whose launch is scheduled for June 2013. IRIS is specially designed for spectrometric observations of the solar atmosphere in EUV lines with high spatial and temporal resolutions. For instance, observation in the Fe xii 1349 Å line (log T = 6.2 K) will have a cadence of 1−2 s, a spatial resolution of 0.4″ (with a field of view of 0.3″ × 40″), an effective area of 2.8 cm^{2}, and a wavelength resolution of Δλ = 12.5 mÅ.
The new Atacama Large Millimeter/submillimeter Array (ALMA) telescope has started to operate and offers unique advantages for solar observations. Spatial resolutions from 0.06″ at 85 GHz to 0.005″ at 950 GHz and short integration times of 32 ms are expected, although a special filter is needed for solar observations, which may considerably reduce the capabilities of the telescope. Nevertheless, flare and chromospheric research may considerably benefit from ALMA, especially for fast waves such as the ones studied here.
The results obtained here would correspond to the ideal case of an imaging spectrometer with at least 2 s cadence, a pixel size resolution of at least one wavelength, and a wavelength resolution of at least 8 points across the line. Furthermore no blending of lines emission was considered, as is produced when observing with the channels of the AIA instrument onboard the Solar Dynamics Observatory, no background optically thick contribution and no instrumental noise. Together with the effects of curvature and non uniform media (leading to different wave dispersion relations) these scenarios will be treated in future work.
5. Conclusions
In this paper we have aimed to understand the variations in observable quantities introduced by the fast MHD sausage mode in coronal structures, by considering geometrical and instrumental effects. Complexities introduced by nonuniformity of the cylinder or the background, curved geometries, or complex instrumental effects, such as instrumental noise, are not taken into account. Although important for realistic models of loops, such characteristics are secondary and their effects on intensity modulation cannot be properly tackled before understanding the effects of simpler parameters on simple geometrical models such as the ones considered in this work. Details from the main results of this work can be found in Table 2. The main findings can be summarized as follows.
The intensity modulation strongly depends on the formation temperature of the spectral line with respect to the temperature of the plasma. Assuming equilibrium ionisation, for plasmas with higher temperature than the formation temperature of the line, such as the case of the base model − 171, the modulation is low (2%−4%) and is slightly affected by the geometrical variation of the cylinder. On the other hand, for plasmas with lower temperature than the formation temperature of the line, such as the base model − 193, the modulation matches the thermodynamical evolution (density and temperature), and can therefore be significant (35%). Nonequilibrium ionisation would completely eliminate the Fe xii intensity modulation (and reduce by a factor of 1.5 or more the Fe ix intensity) due to the fast timescales of the sausage mode. Simple approximations to the intensity that take the column thickness into account and disregard the contribution function G_{λ0}(T,n_{e}) can therefore be very misleading.
Depending on the contribution function, the intensity can be in antiphase with the density (or temperature) profile (case of the base model − 171) or inphase (case of the base model − 193). The line width and the χ^{2} parameter are in phase with the square of the radial velocity. The χ^{2} parameter can also respond to the density variation, which becomes significant for coarse pixel size or large viewing angle. The Doppler velocity is in antiphase with the radial velocity when watching at an angle (non 0°). Correspondingly, for these angles, the Doppler velocity presents a phase shift of one fourth of the period with the intensity. In accordance with the previous result, the intensity and Doppler velocity exhibit the same periodicity as the mode. Double periodicities are characteristic of the line width and the χ^{2} parameter. The χ^{2} parameter can present quadruple periodicities for coarse pixel size or large viewing angle.
The detection of intensity modulation from sausage modes strongly depends on the angle of observation. The intensity decreases with the viewing angle (where 0° angle denotes the perpendicular to the axis of the cylinder) by a factor of 2.5 for the studied range. Furthermore, the intensity modulation can significantly vary longitudinally (along the axis of the cylinder). Rays crossing the cylinder at nodes exhibit considerably less variation than those crossing the antinodes (a factor of 20 or more, depending on the pixel size resolution).
Setting aside equilibrium ionisation effects, the detection of intensity modulation strongly depends on spatial and temporal resolutions. Both can be the dominant parameters, especially if the pixel size is close to the mode’s wavelength or the temporal resolution is close to the mode’s period. A pixel size or a cadence with these values (respectively) can completely erase the longitudinal structuring, therefore eliminating the possibility of detection. Wavelength resolution is not particularly important for the case of sausage modulation. This is due to the inherent symmetry of the sausage mode with respect to the axis of the cylinder, leading to symmetric line profiles. Numerical studies suggest that this and most results presented here may be robust to any inhomogeneities in the model (leading to possible assymmetries), as well as to the effects of varying the crosssection along the cylinder.
Even when the intensity modulation is low, the variation in the Doppler velocity, and especially the line width and the χ^{2} nonGaussianity parameter, can be significant (a factor of up to 40% for line width and up to four orders of magnitude change for the χ^{2} parameter), placing spectrometers in a clear advantage over imaging instruments for detecting these waves. This result is independent of the ionisation state of the plasma, since the spectral line is mainly affected by the unresolved turbulent motions rather than the thermal motions. Significant variability in all quantities can still be obtained when viewing at an angle of up to 30°, with pixel size resolutions up to 1R, or temporal resolution of 1 s and for all considered wavelength resolutions. We consider this to be the most important result of this paper.
Acknowledgments
The authors would like to thank the referee for very constructive comments and Dr. Verwichte, Dr. De Moortel and Dr. Dzifčáková for productive discussions, all leading to a significant improvement of the manuscript. P.A. furthermore thanks Dr. D. Jess for allowing use of his monster Irish computer for the highresolution calculations. T.V.D. and P.A. have received funding from the Odysseus programme of the FWOVlaanderen. This research has been funded by the Interuniversity Attraction Poles Programme initiated by the Belgian Science Policy Office (IAP P7/08 CHARM). TVD also acknowledges funding from the EU’s Framework Programme 7 as an ERG with grant number 276808. CHIANTI is a collaborative project involving the NRL (USA), the Universities of Florence (Italy) and Cambridge (UK), and George Mason University (USA).
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All Tables
Estimates of timescales for ionisation (I) and recombination (R) equilibrium for Fe ix and Fe xii inside the model.
Influence of lineofsight angle, and spatial, temporal, and wavelength resolution on the modulation of observable quantities caused by the sausage mode.
All Figures
Fig. 1 Maps of radial velocity (topleft), longitudinal velocity (topright), density (bottomleft), and temperature (bottomright) along the middle of the cylinder for the base model − 171 (see Sect. 2.4 for more details). The snapshot is taken at onethird of the mode period. The black and white dashed lines in the top panels denote the 4 different lineofsight angles considered: 0°,30°,45°, and 60°. For each angle two rays along the lineofsight are plotted, one passing through a node of the radial velocity (left ray of the pair) and one passing through an antinode of the same quantity (right ray of the pair). The different pixel sizes considered are shown centred at a node: “0R” (=25 km), “1R” = 1 Mm, “2R” = 2 Mm, “3R” = 3 Mm. In the base model, 1R, 2R, and 3R correspond roughly to ℓ/3,2ℓ/3, and ℓ, respectively, where ℓ denotes the wavelength of the mode. 

Open with DEXTER  
In the text 
Fig. 2 Same as Fig. 1 but for the long λ model. See Sect. 2.4 for more details. 

Open with DEXTER  
In the text 
Fig. 3 Integrated intensity along the lineofsight for the base model − 171, at the four different angles considered: 0°,30°,45°, and 60° (see Sect. 2.4 for more details). The snapshot is taken at onethird of the mode period. The crosses in each panel denote the location of the 2 lineofsight rays defined in Sect. 2.3. In each panel, the left and right crosses correspond to the rays crossing a node and an antinode of the oscillation. 

Open with DEXTER  
In the text 
Fig. 4 Same as Fig. 3 but for the base model − 193 (see Sect. 2.4 for more details). The pixel sizes corresponding to 1R, 2R and 3R are shown around the location of ray 2 (antinode). 

Open with DEXTER  
In the text 
Fig. 5 Integrated intensity along the lineofsight (normalised with respect to the equilibrium value) for the 0° angle case for the base model − 171 (left panels) and the base model − 193 (right panels) for two specific rays: ray 1 crossing a node (top most panels) and ray 2 crossing an antinode (bottom panels), shown with crosses in Figs. 3 and 4. Different colours denote different pixel sizes: 0R,1R,2R, and 3R in red, purple, blue, and green, respectively, where R = 1 Mm ≈ ℓ denotes the radius of the cylinder and 0R denotes the spatial resolution in the high resolution model: 2.5 km. The black curve denotes the density profile at the centre of the cylinder and the same location along the axis of the cylinder as rays 1 and 2. The intensity range of the top panels is set significantly narrower than that of the bottom panels in order to show the low intensity modulation at the nodes. 

Open with DEXTER  
In the text 
Fig. 6 Contribution function G_{λ0}(T,n_{e}) for Fe ix 171 and Fe xii 193. The maximum formation temperature for these ions are, respectively, log T = 5.9 and log T = 6.2 K. The black parallelogram in each surface has its corners defined by the minimum and maximum temperature and density values found in the base model, and therefore includes the G_{λ0}(T,n_{e}) values used here. The temperature range in the upper panel has been inverted in order to show the parallelogram for the G_{171}(T,n_{e}) surface. 

Open with DEXTER  
In the text 
Fig. 7 Comparison between an intensity calculated as I ≈ ρ^{2}l, where l is the column thickness along the lineofsight (solid), the base model − 171 intensity I_{171}(t) (dotted), and the base model − 193 intensity I_{193}(t) (dashed) for a viewing angle of 0° and a pixel size resolution of 0R for ray 2. The differences between the lines illustrates the importance of the G_{λ0}(T,n_{e}) function. 

Open with DEXTER  
In the text 
Fig. 8 Same as the right panel of Fig. 5 but fixing the pixel size resolution to 0R and varying the angle of the lineofsight for the base model − 193. 0°,30°,45°, and 60° correspond to the red, purple, blue, and green curves, respectively. 

Open with DEXTER  
In the text 
Fig. 9 Time variation of the specific intensity I_{λ} integrated along ray 1 (left panels) and ray 2 (right panels) for the base model − 171 when viewing at an angle of 0° and for a pixel size of 0R (upper panels) and 2R (lower panels). Contours of the intensity are also shown for better visualisation of the variation. 

Open with DEXTER  
In the text 
Fig. 10 Same as Fig. 9 but for a lineofsight crossing the cylinder at an angle of 45°. 

Open with DEXTER  
In the text 
Fig. 11 Left panel: pixel size resolution dependence of the time variation of the specific intensity I_{λ} for the 0° angle case of the base model − 171. From top to bottom we show quantities ensuing from a Gaussian fit to the spectral line. The first 3 upper panels correspond to the Doppler velocity, the line width and the goodnessoffit χ^{2} parameter for the case of ray 1 (node). The 3 lower panels show the same quantities for the case of ray 2 (antinode). Different line styles correspond to different pixel size resolution: 0R (solid), 1R (dotted), 2R (dashed), 3R (dotdashed). The line width is normalised with respect to the initial value at time t = 0. The unit for the χ^{2} parameter is the logarithm of the normalised value, where the normalisation factor is the equilibrium value. Right panel: angle dependence of the time variation of the specific intensity I_{λ} for the 0R pixel size case of the base model − 171. The arrangement of these panels is the same as for the left panels. Different line styles denote different lineofsight angles: 0° (solid), 30° (dotted), 45° (dashed), 60° (dotdashed). For both left and right panels the variation in time of density (red curve) and radial velocity (blue curve) at the centre of the tube is plotted for reference in arbitrary units in the Doppler velocity panel. 

Open with DEXTER  
In the text 
Fig. 12 Estimation of the spectral line broadening contribution from the unresolved velocity perturbations (which we denote as turbulence) and temperature perturbations. The Gaussian width corresponding to the thermal broadening contribution (dashed curve) is obtained from the average of temperature for the pixels along the lineofsight crossing the cylinder. The Gaussian width corresponding to the turbulent broadening contribution (solid lines) is obtained from a Gaussian fit to the sum of multiple Gaussians, one for each pixel in the cylinder along the lineofsight, with a fixed temporal averaged thermal broadening and shifted centre given by the lineofsight velocity at that pixel. 

Open with DEXTER  
In the text 
Fig. 13 Effects of the temporal resolution on the modulation of observable quantities. We take the base model − 193, fix the pixel size resolution to 0R and consider cadences of “0s” (=0.15 s, solid curve), “1s” (=1 s) ≃P/5 (dotted curve), and “2s” (=2 s) ≃ 3P/7 (dashed curve), where P ≃ 4.5 s is the period of the mode. The upper panel shows the temporal evolution of the normalised integrated intensity along the lineofsight for ray 2 taking a viewing angle of 0°. The rest of the panels, respectively from top to bottom, show the temporal evolution of the Doppler velocity, the line width and (logarithm of) the χ^{2} nonGaussianity parameter resulting from Gaussian fits to the specific intensity profile I_{λ}(t) for the different temporal resolutions. In order to show best the effects on the Doppler velocity, only for this quantity we take the case of ray 1 with a viewing angle of 45°. The normalisation factor for the line width is the initial value at time t = 0 for the 0s temporal resolution. That of the χ^{2} parameter is the time average value of the profile for ray 1 for 0s temporal resolution. 

Open with DEXTER  
In the text 
Fig. 14 Temporal evolution of the Doppler velocity (upper panel), the line width (centre panel) and (logarithm of) the χ^{2} nonGaussianity parameter (lower panel) resulting from Gaussian fits to the specific intensity profile I_{λ}(t) obtained from the base model − 193, for different wavelength resolutions. We consider samplings of 1.4 mÅ (solid curve), 4.2 mÅ (dotted curve) and 8.5 mÅ, leading to 48, 16 and 8 points along the spectral line, respectively. In order to show best the effects of the wavelength we fix the pixel size resolution to 0R and show the case of ray 1 with a viewing angle of 45° for the top panel and the case of ray 2 with a viewing angle of 0° for the middle and bottom panels. The normalisation values are the same as in Fig. 13. 

Open with DEXTER  
In the text 
Fig. 15 Model comparison of the temporal variation of the spectral line broadening. The line width (upper panels) and (logarithm of) the nonGaussianity χ^{2} parameter (lower panels) resulting from the Gaussian fits to the specific intensity I_{λ}(t) for the 0R pixel size case are presented. From left to right the first two panels correspond to rays 1 and 2 for the 0° angle case. The last two panels correspond to rays 1 and 2 for the 45° angle case. Different line styles denote the different models studied in this work, as indicated in the legend. The normalisation values are the time averages of the corresponding quantities for ray 1 and 0° viewing angle. 

Open with DEXTER  
In the text 
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