Issue 
A&A
Volume 566, June 2014



Article Number  A90  
Number of page(s)  13  
Section  The Sun  
DOI  https://doi.org/10.1051/00046361/201423718  
Published online  26 June 2014 
Magnetoseismological insights into the penumbral chromosphere and evidence for wave damping in spicules
Department of Mathematics & Information SciencesNorthumbria University, Newcastle Upon Tyne, NE1 8ST, UK
email: richard.morton@northumbria.ac.uk
Received: 27 February 2014
Accepted: 12 May 2014
Aims. The observation of propagating magnetohydrodynamic kink waves in magnetic structures and measurement of their properties (amplitude, phase speed) can be used to diagnose the plasma conditions in the neighbourhood of the magnetic structure via magnetoseismology. We aim to reveal properties of the chromosphere/transition region above the sunspot penumbra using this technique.
Methods. Hinode SOT observed a sunspot as it was crossing over the limb, providing a unique side on view of the atmosphere above a sunspot. The presence of large spiculelike jets is evident in Ca ii H images. The jets are found to support transverse wave motions that displace the central axis of the spicules, which can be interpreted as the kink wave. The properties of a specific wave event are measured and used to determine the magnetic and density stratification along the structure. In addition, we measure the width of the spicule and the intensity profile along the structure in order to provide a test for the magnetoseismological results.
Results. The measurements of the wave properties reveal an initial rapid increase in amplitude with height above the solar surface, followed by a decrease in amplitude. The magnetoseismological inversions suggests this initial increase corresponds to large changes in density and magnetic field strength. In addition, we provide the first measurements of spicule width with height, which confirm that the spicule under goes rapid expansion. The measured rates of expansion show good agreement with the results from the magnetoseismology. The observed rapid variations in plasma parameters are suggested to be partly due to the presence of a gravitational stratified, ambient atmosphere. Combining width measurements with phase speed measurements implies the observed decrease in wave amplitude at greater heights can be explained by wave damping. Hence, we provide the first direct evidence of wave damping in chromospheric spicules and the quality factor of the damping is found to be significantly smaller than estimated coronal values.
Key words: magnetohydrodynamics (MHD) / waves / Sun: chromosphere / sunspots / Sun: oscillations
© ESO, 2014
1. Introduction
The observation of magnetohydrodynamic (MHD) wave phenomenon in the solar atmosphere has become a common occurrence in the last two decades (see, e.g. Banerjee et al. 2007; De Moortel 2009; Mathioudakis et al. 2013, for reviews). The observations have established that waves are ubiquitous in many different structures, e.g. coronal loops (Tomczyk et al. 2007), spicules (De Pontieu et al. 2007), fibrils (Morton et al. 2012a), prominences (Hillier et al. 2013). Aside from their potential importance for heating the atmospheric plasma, the waves can also be exploited for magnetoseismology (Nakariakov & Verwichte 2005; De Moortel & Nakariakov 2012).
Magnetoseismology is still a relatively fledging field of solar research and is growing in popularity, applicability, and examples (Uchida 1970; Roberts et al. 1984; Banerjee et al. 2007). The basic principles are based on the assumption that MHD waves are guided by localised magnetic structures in the solar atmosphere, with imaging observations appearing to support the existence of such features, for example coronal loops (e.g. Aschwanden & Nightingale 2005) or chromospheric fibrils/spicules (Rutten 2006). The confinement of certain wave modes to the magnetic structure means that the wave properties (e.g. period, amplitude, phase speed) are determined by the local plasma parameters, i.e. those of the supporting structure and the local ambient plasma. Hence, measurement of the wave properties and their inversion can reveal information about the conditions in the neighbourhood of the observed wave, typically information that is difficult to measure from radiation, be that emission measure, polarisation, etc.
To date, there has been significant effort focused on the theoretical development of the field (Andries et al. 2009; Ruderman & Erdélyi 2009; De Moortel 2009), inspired by the TRACE observations of oscillating coronal loops (Nakariakov et al. 1999; Aschwanden et al. 1999) and propagating intensity disturbances (De Moortel et al. 2002). A wave mode that has received significant interest is the fast kink mode, characterised by the physical displacement of the supporting wave guide in the direction perpendicular to the magnetic field (Spruit 1982; Edwin & Roberts 1983). However, the early observational examples of the kink wave mode were related to large amplitude, standing modes excited by flare blast waves. Although their potential for magnetoseismology has been demonstrated (e.g. Nakariakov & Ofman 2001; Arregui et al. 2007; Verth et al. 2008; Goossens et al. 2008; Verwichte et al. 2010a, 2013b), the large wavelengths associated with standing modes (i.e. two times the typical coronal loop length) leads to additional complexities, e.g. consideration of the curvature of the coronal loop (Van Doorsselaere et al. 2004, 2009; Ruderman 2009) and nonplanarity (Ruderman & Scott 2011). Further, the loop also spans a number of density and magnetic scale heights which can lead to variations in the crosssectional area (e.g. Ruderman 2009; Erdélyi & Morton 2009).
More recently, the advent of highresolution spectral and imaging instrumentation (e.g. Hinode Solar Optical Telescope (SOT), ROSA at the Dunn Solar Telescope, CRiSP at the Swedish Solar Telescope) has led to the observations of ubiquitous propagating kink waves in the chromosphere (He et al. 2009a,b; Pietarila et al. 2011; Okamoto & De Pontieu 2011; Kuridze et al. 2012; Morton et al. 2012a). In spite of the vast amount of observed propagating wave phenomenon and the many data sets (e.g. the numerous Ca ii limb data sets), very little use has been made of this rich vein of potential information for magnetoseismology. This opportunity has not escaped all, for example, Verth et al. (2011) provide the first magnetoseismological diagnostic of the quiet chromosphere using SOT Ca ii observations, obtaining estimates for the density and magnetic field gradients and the ionization fraction with height. Further, Kuridze et al. (2013) has applied similar techniques to observations of kink waves in chromospheric mottles. The volume of data and opportunity for the study of the chromosphere and Transition Region via magnetoseismology will no doubt be increased by the highresolution data from the Interface Regions Imaging Spectrograph.
The observation and corresponding magnetoseismology of both standing and propagating waves is not trivial. Typically, significant simplifying assumptions are made about the structure that supports the observed wave during the derivation of theory and estimated values for parameters are used as inputs for the seismological inversion (e.g. density contrasts between internal and ambient plasmas). It is then not clear how accurate the derived magnetoseismological estimates of the various plasma parameters are, relying only on previous estimates of the parameters as guidance. On this note, Verwichte et al. (2013a) has demonstrated the correspondence between values of magnetic field strength derived from magnetoseismology and from magnetic field extrapolations of the same coronal loop. While such a comparison can be achieved for coronal features, the modelling of chromospheric magnetic fields from magnetograms is still an uncertain and ongoing process due to the nonpotentiality of the chromospheric fields (Jing et al. 2011; Meyer et al. 2013). Further, imprudent interpretations of magnetoseismological results can lead to erroneous conclusions about local plasma conditions. For example, failure to consider the influence of wave damping when exploiting the amplitudes of propagating waves for magnetoseismology will undoubtedly lead to underestimates of density and magnetic field gradients.
Here we present a unique observation of wave phenomena in a chromospheric plasma that provides a test of the theoretically derived relations that have been used previously for magnetoseismology exploiting propagating waves (Verth et al. 2011; Morton et al. 2012b; Kuridze et al. 2013). The waves are observed in spiculelike jets that exist in the penumbral region of a sunspot. The jets reach much higher into the solar atmosphere than the surrounding spicules associated with the plage, suggesting that the jets follow the strong magnetic field above the sunspot. In addition, the almost vertical magnetic field lines associated with the sunspot means that the spiculelike features are easier to observe and study in comparison to their plage counterparts, minimising the typical confusion associated with inclined spicules crossing each other. For further details on the jets and the active region, see Morton (2012).
The spicules demonstrate evidence for oscillatory motions which we are able to measure, obtaining amplitudes and phase speeds as a function of height. The magnetic field gradient along the spicule is estimated via magnetoseismology, along with the plasma gradient. In addition, there is also a measurable change in the width of the spicule with height, which enables an independent test for the seismologically estimated magnetic field gradient. It is demonstrated that the measured wave amplitude is likely subject to the effects of damping, hence, we provide the first direct evidence of damped kink waves in the chromosphere. The quality factor of the damping is found to be much smaller than those previously measured in the corona, implying that there is an enhanced damping of waves in the chromosphere and supporting indirect measurements of enhanced damping in the chromosphere/transition region (Morton et al. 2014).
In addition, this result highlights that if the measured amplitude is solely relied upon for magnetoseismological inversion, it would provide incorrect information about the local plasma conditions. Using a combination of the measured width and phase speed, a more realistic estimate for the variation in local plasma parameters is obtained. In general, the following investigation provides the first seismological estimates for the plasma conditions in the upper penumbral chromosphere.
Fig. 1
Hinode SOT field of view. The image also shows the position of the Ca ii limb (black solid line), and the central axis of the spicule (solid white). Crosscuts are taken perpendicular to this central axis. 
2. Observations and data reduction
The data were obtained by Hinode Solar Optical Telescope (SOT  Suematsu et al. 2008) at 01:11:00 UT 21 November 2006 till 02:00:00 UT on the same day. Hinode /SOT viewed a region on the west limb with the Ca ii H broadband filter, which has a pixel size of 0.054′′ but is diffraction limited to 0.2′′ (145 km). The cadence of the data is 8 s. We performed the usual processing routine for SOT data sets with fg_prep.pro. However, the data still possess a significant drift over time and jitter. The drift is first corrected for by tracking the limb over the time series and removing the trend. Next, the remaining jitter is removed by careful alignment of the data using crosscorrelation. The remaining frame to frame movement is found to have a rootmeansquare value of 0.1 pixels.
In the time series, Hinode was following the active region 10 923. Hinode tracked its progress across the disk and the active region has been the subject of a number investigations (e.g. Katsukawa et al. 2007; Tian et al. 2009b). In the data series used here, the sunspot is about to cross the limb (Fig. 1) allowing a novel sideon view of the sunspots structure. The images clearly show vertical and inclined magnetic fields emanating from the region into the lower corona (Morton 2012). In the following, we pay particular attention to one of these spicule or spiculelike jets, which is highlighted in Fig. 1. The spicule is found to support a MHD fast kink wave, which will be the focus of the following investigation.
Fig. 2
The observed kink motion. The left hand column panel shows timedistance diagrams from various crosscuts. Each crosscut shown is separated by 800 km, with the lowest crosscut on the top row. The right hand column shows the results of the Gaussian fits (crosses) with the σ error bars on the measured position. The solid line is the result of the damped sinusoidal fit. The given distance corresponds to the position along the crosscut and the time is seconds from 01:20:51 UT. 
Fig. 3
Measured wave properties. The left panel displays the measured displacement amplitude (stars) as a function of height in the atmosphere relative to τ_{5000} = 1. The vertical bars shows the σ error on the measured quantity. The solid black line corresponds to the cubic fit to the amplitude profile and the dashed lines show the 2σ (95%) confidence level of the fit. The middle panel displays the lag value measured from crosscorrelation of neighbouring timedistance diagrams separated by 40 km (red stars) and 80 km (black diamonds). The red and black solid lines are the corresponding exponential fits to measured lags. The right hand panel displays the phase speed calculated from the fits to the lag data points. The red and black dashed lines correspond to the σ confidence levels for the phase speeds. 
3. Methods
The techniques used to measure the wave and spicule properties are now described, an account of sources of error and error propagation is also given and a brief overview of the relevant magnetoseismological theory is provided.
3.1. Wave fitting
Following previous publications (Morton et al. 2012a, 2013; Morton & McLaughlin 2013), timedistance diagrams are used to analyse the observed wave motion. An unsharp mask (USM) procedure is applied to each frame in order to enhance the spicule compared to the background emission. A timeaveraged image of the spicule is used to determine the main axis of the structure and we note the angle between the jet and the normal to the surface is 28.6 degrees. Each time frame is interpolated (cubic) to a grid a factor of 6 × 6 greater than the original and forty crosscuts are placed perpendicular to the main axis of the spicule, each separated by ~78 km. Once the crosscuts are determined, the results are rescaled to the original spatial sampling and the timedistance diagrams are created. The interpolation step is used to help reduce any differences between each crosscut position and separations that may arise during the mapping of intensities due to the discrete spatial sampling. Crosscuts are also generated in the same manner from the nonUSM data, which are used for error calculation. Examples of the generated timedistance diagrams are shown in Fig. 2.
To fit the wave observed in the timedistance diagram, a Gaussian function is fit to the crosssectional flux profile in each timeframe. The central position of the fitted Gaussian is taken to represent the centre of the spicule. As noted in Morton & McLaughlin (2013), to accurately determine the errors on the measured central position of the spicule, the fitting function has to be supplied with the associated errors in the values of intensity. In order to assess the uncertainty for SOT , the procedure laid out in Aschwanden et al. (2000) and Yuan & Nakariakov (2012) is followed. For each flux value, F, associated with a pixel, we combine the uncertainties in units of data number (DN). The errors arise from photon Poisson noise, dark current noise, flatfield noise, electronic readout noise, compression noise, and subtraction noise. The total error is given by The photon noise is dependent upon the gain, G, of the CCD and the flux of photons received. Shimizu et al. (2007) gave the value of the gain for the BFI as G = 64 e/DN, and the photon noise is given by the usual relation .
In order to assess the dark current and flat field noise, the dark and flat field files were used to generate histograms of the dark/flat values. The CCD is composed of two separate sections with different dark currents and flat field values. A Gaussian was fit to the distribution generated from each section. The standard deviation of the two dark and flat field values are 0.21 DN, 0.298 DN and 0.16 DN, 0.16 DN, respectively. In order not to underestimate the errors, the largest value for the dark current is taken.
To estimate readout noise, fg_prep was run without readout calibration performed. This was subtracted from the fully calibrated data and the residual values were plotted in a histogram and a Gaussian fit gave the standard deviation as 0.51 DN.
The Hinode data is compressed with a 12bit jpeg data compression algorithm using Q table 95. Kobelski et al. (2014) suggest that the jpeg compression used on Hinode XRT images introduces uncertainties of 1.5 DN. Similar ranges of DN are obtained for XRT and SOT images suggesting compression would provide similar errors. To avoid underestimation of the error we set the compression noise at 2 DN.
Digitisation of the signal from the analogtodigital converter provides three lots of 0.5 DN uncertainty (raw, darks and flats), hence, .
The total error is then given by (3)and the error on intensity values are then calculated for each USM timedistance diagram from the corresponding nonUSM crosscut. Once calculated, the errors are supplied to the Gaussian fitting routine to provide the error on the position of central axis of spicule.
The error on the central position is then summed in quadrature with the uncertainty from the alignment procedure (0.1 pixels) to give the total error on the determined central position of the spicule. On doing this for each time slice in a timedistance diagram, we obtain a series of data points related to the motion of the spicule in time (Fig. 2). We fit these data points with a sinusoidal function multiplied by an exponential, namely (4)where ξ is the transverse displacement, P is the period of the oscillation, φ is the phase, and τ is the damping/amplification term depending upon the sign of τ. The measured amplitude in each timedistance diagram is plotted in Fig. 3
Fig. 4
Measured and estimated spicule widths as a function of height in the atmosphere relative to τ_{5000} = 1. The diamond data points are the spicule widths determined form the fitting of a Gaussian to the crosssectional flux profile. The crosses are the estimates for the physical diameter of the spicule calculated from the modelling (referred to as the estimated width). The error bars correspond to the standard error. 
3.2. Spicule width measurements
In order to provide a comparison for the magnetoseismological results (Sect. 4.3), the width of the spicule is measured at different heights. Similar to the wave fitting, a Gaussian plus a linear function is fit to the crosssectional flux profile in each time slice in a timedistance diagram. A measure of the halfwidth of the spicule is given by the σ value of the Gaussian. Averaging the σ values over time and taking the standard error of the mean provides the data points and error bars in Fig. 4.
It is well known that the measured width of solar structures in images is, however, not the actual radius of the structure (Watko & Klimchuk 2000; DeForest 2007; Brooks et al. 2013). The ability to determine the actual radius is impeded by the finite spatial resolution and the point spread function (PSF) of the telescope. In addition, the observed radiation from optically thick lines, such as Ca II H, is affected by the geometry of the structure in which the radiation originates, adding further complications. To assess how some of these limitations affect the measured radius, we provide an estimate of the influence of resolution and PSF on the difference between actual and measured radius, following a similar approach to Watko & Klimchuk (2000).
First, a monolithic structure of length L with circular crosssection of radius r is defined on a 1000 × 1000 × 1000 grid with each grid cube representing 4 × 4 × 4 km^{3}. Each grid cube inside the structure is given the same value on an arbitrary intensity scale. The values are then summed in a direction perpendicular to the direction of the central axis providing a twodimensional image of the structure. This method implicitly assumes that the plasma is optically thin and radiation from each volume element can be summed to give the lineofsight intensity.
The PSF for SOT BFI is particularly complicated and has only been determined previously for particular values of wavelength (WedemeyerBöhm 2008; Mathew et al. 2009). The ideal PSF for Gband is given by Suematsu et al. (2008) as 0.2′′, and WedemeyerBöhm (2008) noted that the ideal PSF varies with the inverse of wavelength. Using this, the ideal PSF for 396.85 nm is calculated as ~0.166′′.
The 2D image of the structure is then interpolated to a grid with grid points equal in size to the SOT pixel size, i.e. 39.1 × 39.1 km^{2}. This image is then convolved with an Airy function of width 3.07 pixels in an order to replicate the PSF. The width of the structure in this new image is then fitted with a Gaussian and the σ measured. Doing this for a number of different radii, we build up a series of data points providing the difference between measured σ and actual radii. Fitting the data points with a quadratic provides a relation between the two quantities which we use to determine an estimate for the radius.
It is clear that this technique is subject to many idealising assumptions, however, a more thorough and accurate method would require advanced models of Ca ii line formation and a complete determination of the PSF at 396.85 nm. Such additions are outside the scope of this work. The current results should be taken as a guide to the expected influence of the PSF on the measured radius and the “actual” radius of the spicule. We refer to the quantity obtained via this technique as the estimated radius (width).
3.3. Propagation speed determination
The propagation speed of the wave is also determined by exploiting the timedistance diagrams. The basis of the technique relies on crosscorrelation of neighbouring timedistance diagrams. The apparent shift of the wave motion in the time direction provides the signal lag between the two images, for which the propagation speed is then given by (5)where dx is the distance between the crosscuts used to generate the timedistance diagrams, dt is the time difference between each pixel, and T is the lag value.
In order to improve the accuracy of the phase speed determination, the timedistance diagrams are first interpolated so that they are mapped onto a grid twice the size of the original, hence each pixel has dimensions 19.6 km by 4 s. The uncertainty on each measurement from the crosscorrelation is unknown, although it is believed to be <0.1 pixel. The second step is the application of crosscorrelation for a sliding window in the time direction giving multiple measurements of the lag time. The lag value is calculated as the average value of the measurements and the error is taken as the standard error of the results.
In Fig. 3, the lag values calculated for the timedistance diagrams separated by ~80 km are displayed. In addition, timedistance diagrams are generated for additional crosscuts placed midway between the previous crosscuts. This provides 80 crosscuts separated by ~40 km. Again, these are interpolated and the lag is calculated. Multiplying these additional values by two we obtain lags of similar magnitude to those found for the ~80 km separated crosscuts (see Fig. 3). This provides confidence that the obtained lag values are genuine.
The values of measured lags are close to 0.1 pixels, with standard deviations for the ~80 km lags ranging between 0.006−0.08 pixels, with an average of 0.03 pixels. For the ~40 km lags, the measured lags are ~0.05 pixels with standard deviations ranging between 0.003−0.03 pixels, with an average of 0.01 pixels.
Next, a weighted fit of an exponential function to the lag data points is performed. A fit of a linear function was also performed but the exponential function was found to have a smaller χ^{2} value. The residual values to the fit have rootmeansquare amplitudes of 0.035 and 0.021 for the ~80 km and ~40 km separations, respectively. Both of these values are larger than the average standard deviations, which indicates that some systematic error is present in the analysis. It is difficult to determine exactly where the systematic errors enter, one option is this occurs during the determination of crosscut position, i.e. an uncertainty in the relative position of each crosscut. This error could possibly be reduced if the data is interpolated to a larger grid when initially creating the crosscuts and timedistance diagrams.
Bearing this in mind, the propagation speed and associated errors are determined using Eq. (5), with T given by the fit and uncertainties are the σ errors to the fit, dt is 4 ± 0.05 s and dx = 80 ± 7 km or dx = 40 ± 7 km. The error in dt is given by the accuracy of the clock onboard Hinode , which gives times rounded to 0.1 s. The uncertainty in dx is taken from knowing the position of the crosscut to 1/6 of a pixel, i.e. from the initial interpolation. It is found that the propagation speeds determined for both sets of lags largely agree within σ errors (Fig. 3).
3.4. Theoretical considerations
Having measured the amplitude and propagation speed as a function of distance along the spicule, these quantities can be used to estimate gradients in magnetic field and plasma density. The WKB approximation for the wave equation governing a kink wave propagating along a stratified flux tube (Verth & Erdélyi 2008; Ruderman et al. 2008; Morton et al. 2012b) gives the solution, (6)where (7)Here, c_{k}(z) is kink phase speed, C is some constant, ω = 2π/P is the angular frequency of the wave, R(z) is the radius of the flux tube, ⟨ B ⟩ is the local average magnetic field strength, ⟨ ρ ⟩ is the local average density, and μ_{0} is the magnetic permeability. A similar technique is used in Verth et al. (2011), although they solve the governing equation under the assumption the phase speed changes exponentially with respect to z. Note that these equations are derived in the thin tube approximation, i.e. where the wavelength is much longer than the radius of the waveguide. The wavelength, λ, is given by the product of the period and the phase speed of the wave. From Figs. 2 and 3, the wavelength can be calculated to be on the order of 10 000 km, hence, the ratio of r/λ ~ 0.03 (using the measurements in Fig. 4) and the thin tube approximation is satisfied for the current observation.
Equation (6) gives the expected amplitude evolution for a propagating wave if it is assumed that the influence of wave damping mechanisms can be neglected. However, there is evidence indicating that wave damping occurs in observations of waves in solar plasmas (e.g. Aschwanden et al. 1999; Tomczyk & McIntosh 2009). It is generally considered that resonant absorption is responsible for the observed damping, with a good agreement between observations and theory (Ruderman & Roberts 2002; Verwichte et al. 2010b; De Moortel & Pascoe 2012; Terradas et al. 2010; Soler et al. 2011b, 2013). Soler et al. (2011b) derived the function that describes the evolution of the amplitude for propagating kink waves with the inclusion of resonant absorption. Consideration of their Eq. (38) suggests that Eq. (6) would be modified as follows, (8)where the damping length is (9)and ξ_{E} is the quality factor and f = 1 /P is the frequency of the wave.
For now, it is assumed that damping can be neglected and magnetoseismological relations useful for inversions of the measured wave properties are derived. Upon dividing Eq. (6) by itself evaluated at z = 0 and rearranging, the following is obtained (10)This relation allows the estimation of the magnetic expansion along the flux tube using the measured values of amplitude and propagation speed.
To calculate the uncertainty in R, Eq. (13) is written in terms of the independently measured quantities, namely (11)where c_{k} is taken to equal c_{p}, and following standard rules for error propagation, (12)where δy is the σ error associated with the quantity y. Similar equations can be derived for the magnetic field, B, (13)with the associated uncertainty (14)Further, the gradient of the density can be obtained by combing Eqs. (6), (7), where it is easily found that (15)and (16)The variation in amplitude of the wave can be seen to be a proxy for the variation in density.
Fig. 5
Flows along the spicule. The image shows a timedistance diagram generated from the unsharp masked data and taken parallel to the spicule axis. The straight lines highlight the measured upflows and the measured flow speeds are given. The time is shown in seconds from 01:18:11 UT. 
Before continuing, we note that the equations given in this section were derived assuming that the plasma in the waveguide is static, i.e. there are no flows along the waveguide. Spicules by their very nature are jets, hence, there will be plasma flow along the waveguide at the time of the measurements. At present, there is no extension to the magnetoseismological tools shown here that includes the influence of flows. However, insights into the magnitude of the influence of the flow on the measured parameters can be obtained from, e.g., Nakariakov & Roberts (1995), TerraHomem et al. (2003), Morton & Erdélyi (2009), Ruderman (2010, 2011), Morton et al. (2011), Soler et al. (2011a). For example, the equations in Soler et al. (2011a) suggest that the phase velocity is modified by terms on the order of (U/c_{k})^{2} (e.g., their Eqs. (9) and (11)). From considering the governing wave equations with flows incorporated, the terms introduced by the flow are also on the order of (U/c_{k})^{2} or .
Flows along various spicules in the current data set were found to have an average value of ~28 km s^{1} (Morton 2012). In Fig. 5, we show a timedistance diagram generated from the unsharpmasked data. The crosscut is this time placed parallel to the axis of the spicule of interest here. This reveals the pattern of flows along the spicule. At the time the wave occurs (approximately 300−500 s in Fig. 5), the measurable flow speeds are between 20−30 km s^{1}. Hence, this means that the affect due to the flow on the wave is small, (U/c_{k})^{2}< 0.05, and can be neglected for now. An advanced theory of wave propagation with magnetoseismological tools that incorporates the influence of flow will be required to confirm the validity of this assumption. Furthermore, such a theoretical framework will be highly desirable for future studies of chromospheric waves.
3.5. Intensity measurements
As well as incorporating the width measurements of the spicule for comparison to magnetoseismological estimates of expansion and magnetic field gradients, an estimate of the density scale heights is achievable via other means. Previous studies suggest that the emission gradient can act a guide to the density gradient along the spicule (e.g. Makita 2003; Bjølseth 2008; Judge & Carlsson 2010). The assumption is made that the spicule plasma can be treated essentially as an optically thin media, meaning the intensity is proportional to the density and the source function. Assuming a constant source function means the intensity scale height equals the density scale height. In the calculations of Judge & Carlsson (2010), the mean spicule source function, calculated locally by collisional excitation and scattering of radiation from the photosphere, decreases by less than a factor of 2 over 3 Mm. Hence, the measured intensity scale height can only be used as a guide rather than a definitive measurement of the plasma density scale height.
First, we determine the intensity along the spicule by placing a crosscut parallel to its axis and averaging the values over the time period for which the oscillation is measured. In addition, it is of interest to see how the intensity changes as a function of height for the penumbra as well as the neighbouring plage region. To measure the intensity scale heights for the surrounding atmosphere, crosscuts are taken at an angle to the limb and averaged over a relatively narrow spatial window but an extended temporal window. The intensity scale heights are calculated using (17)As this involves taking derivatives of the intensity, discontinuities lead to large variations in the scale height. To suppress these effects, a smoothing of the intensity profiles is performed. The intensities and scale heights for the different features are shown in Fig. 7.
Using the pointing information from the observations log, the polar coordinate values of each pixel location are determined with respect to disk centre. The angle between the crosscuts and the normal to the tangent of an arc of constant radius is then obtained, and used later to determine the radial height of pixels in crosscuts and correct the values of intensity scale heights to give H(r), i.e. the scale height as a function of radial distance. As mentioned in Sect. 3.1, the angle between the spicule and normal to the surface is 28.6 degrees.
For later comparison with existing models of penumbral atmospheres (e.g. Fontenla et al. 2006), it becomes necessary to determine the exact height above the photosphere the radiation is emitted. Following the standard convention, our solar surface (height = 0 km) is defined as the height at which the optical depth equals one for light emitted at 5000 Å. It has been demonstrated by Bjølseth (2008) that the Ca ii formation height at the limb is approximately 825 km above this level. In the definition of the Ca ii limb given by Bjølseth (2008), she identifies the Ca ii limb as the point at which the intensity scale height reaches a minimum value, which occurs almost immediately after a steep drop in the value of intensity scale height. For the current data, this definition does not give realistic results and would place the limb high into the atmosphere. This is most likely due to the apparent closed nature of the Ca ii features seen in the plage regions surrounding the sunspot, which provide an extended emission profile above the limb with low variance. To identify the limb, we make use of the visible sunspot umbra. The sunspot has a significantly shortened umbra because it has rotated almost off disk and is crossing the limb, no discernible chromospheric emission is obvious on the far side of the sunspot except possibly the stalks of some jets. The position of the farside of the umbra (i.e. the side due to cross the limb first) is taken as the height of the Ca ii limb. On relating the intensity profiles with this position, the Ca ii limb occurs close to where the intensity begins to drop off rapidly (Fig. 7), after initial intensity bumps from the closed structures in the plage and the bright jets in the penumbral region. For the intensity scale heights, it can be seen that the steep drop off in scale height occurs just below the height of 825 km, with the rate of change of scale height decreasing significantly above this value. Although the minimum values of scale height do not occur near 825 km, the presence of the steep change in scale height below this value provides confidence that the position of the Ca ii limb has been identified reasonably well.
4. Results
4.1. Wave measurements
In Fig. 2, a number of timedistance diagrams are shown, starting with the lowest altitude crosscut (top row) and each of the succeeding timedistance diagrams are from successive crosscuts separated by 800 km. The periodic transverse displacement of the spicule is clearly seen and it is also noticeable that the amplitude of the disturbance increases between the first and second rows. The right hand panels show the corresponding fits to the feature in the timedistance diagrams. It is chosen to fit the wave only for two cycles, additional cycles are evident but the fit result have greater uncertainties.
In Fig. 3, the displacement amplitude measured in all 40 timedistance diagrams is plotted in the first panel. We remind the reader that the all measured quantities are given as a function of height in the solar atmosphere above the τ_{5000} = 1 height. This is different from the distance along the spicule, which can be calculated as (height − 1880)/cos(28.6) km. The amplitude can be seen to increase by a factor of two over the first 800 km, then begins to decrease. We speculate in Sect. 5 as to what is responsible for the observed decrease in amplitude and it’s implications for the magnetoseismological results. The given amplitude profile is fitted with a cubic polynomial, which we note has a smaller than a quadratic fit.
Fig. 6
Magnetoseismological estimates of plasma gradients as a function of height in the atmosphere relative to τ_{5000} = 1. The left hand panel shows the magnetoseismologically determined radial expansion (solid line) with the 95% confidence level shown (dashed lines). The diamonds and crosses show the expansion inferred from the measurements of the Gaussian width and modelling (estimated), respectively, with standard errors given. The middle panel shows magnetoseismological estimate for the gradient of the magnetic field (solid) and the inferred magnetic expansion (crosses). The right hand panel is the density gradient determined using the measured displacement amplitude (solid) with 95% confidence intervals (dashed), and a combination of the modelled (estimated) width and measured phase speed (crosses). The red lines are exponential fits to the data points. 
Fig. 7
Spatially and temporally averaged intensity profiles (left panel) for the penumbra (black solid), the plage (blue dash) and the spicule (red dashdot) as a function of height in the atmosphere relative to τ_{5000} = 1. The right panel shows the calculated intensity scale heights for each feature. 
In the second and third panels of Fig. 3, the measured lag between timedistance diagrams and the calculated propagation speeds are shown, respectively. The wave is found to be upwardly propagating with no sign of reflection. It has been suggested that a mixture of upward and downward propagating waves can exists in coronal hole spicules (Okamoto & De Pontieu 2011), although the dominant fraction are upwardly propagating. At present, we cannot say whether the situation is similar for active region waves.
The average lag values measured for the ~80 km (black stars) and ~40 km (red stars) separations are given. The ~40 km lag values have been multiplied by a factor of two to enable a direct comparison with the ~80 km lag values. It is evident that the two sets of values demonstrate a very good agreement. The two sets of lag values are then individually subject to a weighted fit using an exponential function. Linear and quadratic functions were also fit to the data points but had greater values than the exponential fit. The fitted function and the calculated σ uncertainties for the fit parameters are then used to calculate the phase speed and associated error. In Fig. 3, the σ confidence bound is shown for each of the calculated phase speeds, showing an overlap in values between the two measurements. In the following calculations, we will use the results from the ~80 km crosscut separation as the residuals between the exponential fit and the data points are relatively smaller (Sect. 3.3).
4.2. Width measurements
We now discuss the results of the width measurements before discussing the magnetoseismology results. Figure 4 displays the measured width of the spicule as a function of distance and measured widths are close to the spatial resolution of SOT (approximately 0.2′′ = 145 km at 3968 Å). It is clear that the measured values show evidence for expansion along the structure, which to the best of our knowledge has not been observed directly along a spicule structure before. The expansion factor reaches a value of Γ = 2.2. Figure 4 also displays the estimated diameter of the spicule after taking into account instrumental effects discussed in Sect. 3.2. The variation in the estimated width of the structure can be seen to greater (Γ = 3) than that of the halfwidth measured from the Gaussian fit. It is unclear how the use of an idealised PSF compared to a fully calibrated PSF (e.g. WedemeyerBöhm 2008) would influence the current results. The calculated width should be taken as a guide to the actual expansion.
4.3. Magnetoseismology
The magnetoseismological results are obtained by exploiting the measured displacement amplitude and phase speed from the 80 km crosscut separation. Instead of the data points, the fitted functions to ξ and c_{k} are used as inputs for the equations. To derive the expansion of the spicule, the measurements are substituted into Eq. (10) and the errors are calculated using Eq. (12). The results are plotted in the first panel of Fig. 6, along with the 95% confidence level. It is found that the spicule expands with height, which corroborates the width measurements. Overplotting the measured and estimated expansion, it can be seen that there is a relatively good agreement between the estimated expansion and the expansion estimate from magnetoseismology. This is especially the case for the first 1000 km, however, the estimated expansion appears to increase to a much greater degree over the last 2000 km. The measured expansion shows much less agreement with the magnetoseismological results than the estimated expansion.
Next, the gradient of the magnetic field and errors are obtained using Eqs. (13) and (14) and plotted in the middle panel of Fig. 6. A initial rapid decrease in magnetic field strength is found and, as with expansion, the gradient flattens out after 700 km. In addition, the gradient in the magnetic field obtained from the estimated width is over plotted. As expected from comparing the radii results, the magnetoseismological and estimated results initially show a good agreement and then the results diverge with height. The variation in magnetic field strength from the estimated results is subject to a twopart exponential fit in order to determine scaleheights.
The final panel in Fig. 6 shows the gradient in the density along the spicules, which is obtained from the fit to the amplitude and Eqs. (15) and (16). It is found that the magnetoseismological estimate suggests that the density decreases with height. The gradient of the density displays a strange profile, indicating the density begins to increase with height after 2500 km. We believe this is an artefact of our theoretical assumptions in Sect. 3.4 and will discuss the nature of the increase in Sect. 5. Further, we remind readers that the density profile is the average density profile of the internal and external densities. Hence, Fig. 6 probably does not correspond to the density variation along the spicule alone.
In advance of this discussion, another method is used to estimate the average gradient in density. From Eq. (7), it is evident that upon being able to measure the expansion of the spicule and the phase speed of the wave propagating along the structure, the gradient in the density can be sought via inversion of the measured quantities. To this end, the measured phase speed and estimated width are used in Eq. (7) and the results are over plotted in Fig. 6. The general trend for the density is now found to decrease along the entire length of the spicule, although the rate of change decreases significantly after the first few hundred kilometres. This density is subject to a twopart exponential fit in order to determine average scaleheights.
4.4. Intensity measurements
The intensity measurements have been discussed briefly in Sect. 3.5, mainly in relation to the location of the τ_{5000} = 1 height with respect to the Ca ii measurements. In Fig. 7, the left hand panel shows the intensity above the limb for a plage region, the penumbral region and also for the spicule of interest. The plage emission can be seen to be brighter than the penumbral region and this is evident from looking at the emission in Fig. 1. The jets above the penumbra and umbra are sparsely populated in comparison to the plage, leading to the lower intensity values. This was noted in Morton (2012, see Fig. 7 in that paper). The peak of the emission close to the Ca ii limb (~800 km) appears to occur at marginally lower heights in the penumbra than for the plage, indicating the possibility of a lower height of the chromosphere in the active region. This point will be discussed in further detail in the Sect. 5.
The spicule emission initially equals the average emission above the penumbra but diverges after ~1500 km, and is observed to be greater than that of the corresponding average plage and penumbral atmospheres at larger heights.
On calculating the scaleheights for each region, it is found for all regions the scale height is typically greater than 2 Mm which is larger than the predicted scale heights for a gravitationally stratified plasma at 0.01 − 0.02 MK, i.e. 250 − 500 km. These results are typical for the chromosphere as seen at the limb and are related to the extended spicular emission (Bjølseth 2008; Pereira et al. 2012). Under the assumption of an optically thin medium, the density should also have similar scale heights.
5. Discussion
5.1. Expansion of the magnetic field
We begin by discussing the estimate of magnetic field expansion. Both the measured width and magnetoseismological measurements display evidence for a rapid expansion over the first few hundred kilometres (atmospheric height of 1800−2500 km). It has been previously noted from spectropolarimetric studies above sunspots that the penumbral magnetic fields drops relatively rapidly between the photosphere and chromosphere. Rueedi et al. (1995) measures a factor of 2 decrease between photospheric (Si i) and chromospheric (He i 10 830 Å) magnetic fields strengths. Further, Leka & Metcalf (2003) measure the majority of magnetic scaleheights to be <Mm between photospheric (Fe i) and chormospheric (Na i D1) measurements. Model atmospheres would imply the chromospheric lines used in these studies are likely to form in either the low chromosphere, with Na i formed <1 Mm in magnetic concentrations (e.g. Leenaarts et al. 2010) or, upper chromosphere, with He i 10 830 Å showing evidence for the onset of fibrillar structures (Schad et al. 2013) suggesting it samples similar heights to Hα and Ca II IR (~1.5 − 2 Mm). However, the initial decrease in magnetic field strength measured here is more rapid than those reported in these previous studies, requiring a magnetic scale height of 0.35 ± 0.05 Mm.
The magnetoseismological results show that the spicule then contracts slightly, although the error bars do not rule out that the structure remains at a constant radius and magnetic field strength. This results is in apparent contradiction to the measurement of the estimated spicule width, which imply that the expansion after the first 1000 km is much more gradual and has a scale height of 2.5 ± 0.3 Mm. The discrepancy between the two results could be due to a variety of reasons. One possibility is related to the assumption that the measurement of the width of the spicules crosssectional flux profile provides an estimate of the width of the magnetic structure. The plasma is not necessary optically thin at the limb and the emitted radiation is linked to the geometry of the structure. Coupled with this is the assumption that the structure expands uniformly in all directions with height. On the other hand, the explanation may lie with wave damping. In general, the observed variation in amplitude of a wave will be the result of competition between the variation in plasma parameters along the structure, i.e. Eq. (8), and the influence of wave damping due to, e.g. resonant absorption (Terradas et al. 2010; Verth et al. 2010; Pascoe et al. 2011, 2012). Considering the good agreement between the general trends obtained for the estimated width and the magnetoseismological results during the initial 1000 km, the first option seems less likely as an explanation. However, it may be one of the contributing factors to any small scale differences between the two techniques. We will return to the discussion of wave damping later and demonstrate that this is a consistent hypothesis for the observed variation between the two techniques.
5.2. The density gradient
Next, we discuss the estimates for the density gradient. The magnetoseismological results show similar trends in density to the change in magnetic field, i.e. an large initial decrease in the density followed by an increase in density over heights of 3000 km. Again, we will attribute the increase to wave damping. Upon using a combination of the estimated width (which is assumed to provide a reasonable estimate for the change in magnetic field strength) and the derived phase speed, it is seen that the density continues to decrease with height, however at a reduced rate (i.e. implying an increased scale height). Again, we note that the derived variation of density in Fig. 6c is an average variation of the internal and external quantities. The estimated average scale height for the second phase of density decrease is 3.2 ± 1.0 Mm, which is close to the measured values of intensity scale height. An exponential fit to the initial phase of density decrease provides a scale height of 0.19 ± 0.04 Mm, although the over plotted fit in Fig. 6 demonstrates an exponential does not represent the results adequately. With respect to previous results, the assumption of an optically thin plasma is typically made for density estimates from observations in Ca ii (see discussion in Sect. 3.5). To the best of our knowledge, such observational measurements haven’t been made for chromospheric plasmas above sunspots and their penumbra.
5.3. A gravitationally stratified background atmosphere
The presented observations and results raise the question: can the observed initial rapid decrease in both magnetic field strength and density be explained by a physical model? We begin by reemphasising that the seismological changes in both density and magnetic field actually represent the average changes in each quantity (see Eq. (7)). The relative agreement between the spicule width measurements and the magnetoseismological results for the first ~500 km suggest that the internal magnetic field is subject to a rapid decrease. By proxy, we assume that the initial density decrease obtained from the magnetoseismology is also physical. The implied initial scale height is then somewhat at odds with that derived from the Ca II emission (Fig. 7). However, this difference can be partly reconciled if we hypothesise that the ambient plasma which surrounds the spicule is that of an unseen external atmosphere, whose plasma properties demonstrate a variation that corresponds closely to a gravitationally stratified atmosphere in hydrostatic equilibrium. Judge & Carlsson (2010) demonstrated that the presence of such an atmosphere would not be visible in Hinode Ca II images of the limb. They suggested the presence of the spicular material in the Ca II bandpass is due to the spicule plasma being subject to Dopper shifts from combined flows and wave motions. We note that their results were derived for plasma in a coronal hole but the general result should still be true for active region spicules.
We provide a simple model to demonstrate how such a scenario could lead to the measured variation in density. The density is given by (18)where H is the density scale height. We assume that the spicule originates in the low chromosphere and initially the internal and external densities are approximately similar in magnitude, i.e. ρ_{i} ≈ ρ_{e}, and that the external medium has a small initial scale height corresponding to the density change associated with a Transition Region. A density scale height value of H_{ex} = 25 km is selected such that the external density decreases by a factor of 100 over the Transition Region to produce a typical chromospheric to coronal density transition. After 100 km, the density scale height in the external medium is assumed to have a typical lowcoronal value of H_{ex} = 20 000 km (i.e. T ≈ 0.4 MK), i.e. (19)Guided by the Ca II emission, we assume that spicule material has a constant scale height of H_{s,1} = 3000 km. We normalise the density so the magnitudes of the density are not required. The calculated variation in average density is shown in Fig. 8. It is seen that the presence of an unseen external hydrostatic atmosphere and a slowly changing spicular density would then provide a result that is qualitatively similar to that in Fig. 6. However, the magnitude of the initial decrease can only be realised if it is assumed that the spicule density also initially decreases relatively rapidly, as seen if the internal spicule density height is (20)If we are to maintain the assumption of a correspondence between emission scale height and density, then this would imply that an initial steep intensity gradient is somehow masked in the lower atmosphere. This could well be the case if a number of short, spicule like features contribute to the emission in the lower atmosphere and mask any drop in intensity. Alternatively, it could be that the observed spicule intensity is prescribed by the source functions with little correspondence to the density (Judge & Carlsson 2010).
Fig. 8
Modelling the predicted density profile along a spicule from magnetoseismology. The data points are the measured change in average density along the spicule. The red dash line is a normalised density profile (H_{e}) for the ambient plasma, designed as a simplified model of the classic hydrostatic solar atmosphere. The blue dashdot lines show two different normalised internal (spicule) density profiles (H_{s,1},H_{s,2}). The solid black lines show the average normalised density profiles calculated using the different internal density profiles. 
Fig. 9
Evidence for wave damping. The plot shows the amplitude measured from the spicule oscillations (blue stars) and the amplitude determined from the estimated expansion and the phase speed measurements (black crosses). The error bars are the σ errors for each quantity. The black solid lines correspond to exponential fits to each amplitude profile. The diamonds shows the expected amplitude from wave damping. 
If the presence of a hydrostatically stratified atmosphere is indeed what the magnetoseismological estimates demonstrate, then the results show the Transition Region of the external plasma above the penumbra occurs at a height of around 1800 − 2000 km above the τ_{5000} = 1 layer. On comparison to the atmospheric model of Fontenla et al. (2006) for a penumbral region (model R), the observed height is around 300 km higher than the predicted height. The Transition Region (and chromosphere) are predicted to occur at lower heights above regions of increasing magnetic activity, approximately 1500 km. At present, the magnitude of error related to our determination of the position of the Ca ii limb is unclear. This is due to the adhoc technique that had to be used (see Sect. 3.5).
This result is not at odds with observations in Tian et al. (2009b) and Morton (2012), which demonstrate that the Transition Region above sunspots is higher than the Transition Region above plage regions. However, the conclusions of the previous results would need to be amended to incorporate the current findings. The spiculelike jets do lift chromospheric and Transition Region material higher into the atmosphere than the corresponding plage spicules, as is evidenced by the greater heights reached by the penumbral spicules (see, Morton 2012). However, this is against the background of an ambient, almost “hydrostatic” plasma. The presence of an external “hydrostatic” plasma, along with the reduced opacity above sunspots, may help explain the limited self reversals observed in Lymanα lines above penumbras when compared to quiet Sun profiles (Tian et al. 2009a,b; Curdt et al. 2008).
5.4. Evidence for wave damping
Now, we consider whether the discrepancy between the measured spicule width and the magnetoseismological results can be explained by wave damping. Assuming that the measured estimated expansion provides the correct change in area (and magnetic field strength) along the spicule, then, using Eq. (11), the expected change in wave amplitude from the variation of the magnetic gradients and phase speed can be calculated. The result is plotted in Fig. 9 and the height scale on the xaxis now corresponds to distance along the spicule. It can be seen that the measured variation in magnetic field strength and phase speed suggest that the amplitude of the wave should increase with height almost continuously, in contradiction with the measured amplitude. On comparing the two amplitude profiles we can then estimate the damping rate in the chromosphere. To simplify the situation, we ignore the amplitude measured in the section of the spicule identified with the external Transition Region. In addition, it is assumed that the damping length is constant, rather than a function of distance as given in Eq. (9). First, both the amplitude profiles are fitted with an exponential profile of the form
where the subscripts m or c correspond to the measured or calculated values, respectively. Assuming an exponential damping profile, the rate of damping, L_{D}, can be calculated from
and provides a damping length of L_{D} = 5500 km. Multiplying the undamped amplitude profile by the exponential with the derived damping length provides the diamonds in Fig. 9. The quality factor for the damping is calculated to be ξ = 0.34 for a phase speed of 200 km s^{1} and P = 80 s.
From these results, it would suggest that there is a relatively strong damping in the spicule feature. The quality factor obtained here is significantly smaller than the majority of those previously measured in damped coronal loop oscillations, both for propagating (2.69 – Verth et al. 2010) and standing (ξ> 1 – Verwichte et al. 2013b) modes.
The quality factor is a frequency dependent quantity, so to compare to previous results in different frequency regimes, it is better to use the quantity α introduced in Morton et al. (2014), which is calculated to be α = L_{D}/P = 0.07 Mm/s. For estimates of damping between the chromosphere and corona, Morton et al. (2014) give the value of α ≈ 0.2, which is essentially the value averaged over a height of 15 Mm. Considering Eq. (9), it is evident that α will likely increase with height due to the expected trend for the kink (Alfvén) speed to increase between the chromosphere and corona. Hence the average value in Morton et al. (2014) will incorporate a range of α values. The value of α we obtain here supports the idea of the enhanced damping of waves propagating through the lower solar atmosphere when compared to wave damping observed in the corona. This is likely to be due to a smaller measured phase speed of kink waves in the chromosphere and an increased density contrast for chromospheric jets in the corona compared to coronal loops, leading to a smaller quality factor (see, e.g., Eq. (9)).
Note that, at present, other damping mechanisms aside from resonant absorption cannot be ruled out as acting on the observed wave. For example, in partially ionised plasmas such as the chromosphere, collisions between ions and neutrals can lead to a damping of the waves (e.g., De Pontieu et al. 2001; Soler et al. 2012). However, the influence of ionneutral collisions appears negligible compared to resonant absorption for the current observation (see, Soler et al. 2012).
6. Conclusions
Over the last decade, the use of magnetoseismological inversion techniques to probe the solar plasma has increased. However, the ability to test the accuracy of results is difficult, mainly because the magnetoseismology is used to estimate otherwise difficult or unmeasurable quantities. The example of a spicule oscillation presented here provides a unique opportunity to compare the magnetoseismological results to values measured using independent techniques. The comparison between the independent methods shows a good agreement for the variation in spicule plasma parameters when the effects of wave damping are negligible compared to variations in plasma quantities. When damping dominates the variation in wave amplitude, there is a disagreement between the two independent measures. Hence, this highlights the importance of carefully taking account the various competing mechanisms that can affect the amplitude of the wave, in order to ensure that magnetoseismology results provide an accurate description of the variations in plasma parameters through the solar atmosphere.
In carefully measuring wave properties and taking into account the competing mechanisms, we have been able to provide the first direct evidence of kink wave damping in chromospheric spicules. The derived damping lengths are much shorter than those reported from coronal observations of damped kink waves and support the suggestion of an enhanced damping of waves in the lower solar atmosphere (Morton et al. 2014). The presence of enhanced wave damping would also help to explain the strange magnetoseismological predictions for the density variations in Verth et al. (2011) and Kuridze et al. (2013).
In addition, both direct and magnetoseismological measurement suggest the presence of a strongly stratified atmosphere. On comparing the magnetoseismological estimates of density scale height to intensity scale heights in Ca ii, this might suggest a contradiction between the two techniques. However, this contradiction can be negated if we assume that there is an unseen strongly stratified ambient plasma in which the weakly stratified spicule exists. The ambient atmosphere would be close to the classic hydrostatic model of the solar atmosphere, with a significant density gradient in the Transition Region. The notion that an approximately hydrostatic atmosphere that would be unseen in SOT Ca ii was initially put forward by Judge & Carlsson (2010).
Overall, the study presented here highlights the rich vein of information the still remains to be mined from the numerous Hinode and ground based images of the chromosphere. While difficulties still remain in more direct measurements of chromospheric plasma properties, the ubiquitous nature of MHD kink waves provides an alternative diagnostic option. However, it is worth restating, care is needed when using magnetoseismological techniques to diagnose the chromosphere and the assumptions used to derive the diagnostic relations between observables and plasma properties, e.g. Eqs. (6) and (7), should be always be revisited when interpreting the results of inversions.
Acknowledgments
R.M. is grateful to Northumbria University for the award of the Anniversary Fellowship and thanks D. Brooks and G. Verth for useful discussions. The author acknowledges IDL support provided by STFC. This work was aided by a Royal Astronomical Society Travel Grant.
References
 Andries, J., van Doorsselaere, T., Roberts, B., et al. 2009, Space Sci. Rev., 149, 3 [NASA ADS] [CrossRef] [Google Scholar]
 Arregui, I., Andries, J., Van Doorsselaere, T., Goossens, M., & Poedts, S. 2007, A&A, 463, 333 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Aschwanden, M. J., & Nightingale, R. W. 2005, ApJ, 633, 499 [NASA ADS] [CrossRef] [Google Scholar]
 Aschwanden, M. J., Fletcher, L., Schrijver, C. J., & Alexander, D. 1999, ApJ, 520, 880 [NASA ADS] [CrossRef] [Google Scholar]
 Aschwanden, M. J., Tarbell, T. D., Nightingale, R. W., et al. 2000, ApJ, 535, 1047 [NASA ADS] [CrossRef] [Google Scholar]
 Banerjee, D., Erdélyi, R., Oliver, R., & O’Shea, E. 2007, Sol. Phys., 246, 3 [NASA ADS] [CrossRef] [Google Scholar]
 Bjølseth, S. 2008, Masters Thesis, Oslo Univ. [Google Scholar]
 Brooks, D. H., Warren, H. P., UgarteUrra, I., & Winebarger, A. R. 2013, ApJ, 772, L19 [NASA ADS] [CrossRef] [Google Scholar]
 Curdt, W., Tian, H., Teriaca, L., Schühle, U., & Lemaire, P. 2008, A&A, 492, L9 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 De Moortel, I. 2009, Space Sci. Rev., 149, 65 [NASA ADS] [CrossRef] [Google Scholar]
 De Moortel, I., & Nakariakov, V. M. 2012, Roy. Soc. London Philos. Trans. Ser. A, 370, 3193 [Google Scholar]
 De Moortel, I., & Pascoe, D. J. 2012, ApJ, 746, 31 [NASA ADS] [CrossRef] [Google Scholar]
 De Moortel, I., Ireland, J., Hood, A. W., & Walsh, R. W. 2002, A&A, 387, L13 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 De Pontieu, B., Martens, P. C. H., & Hudson, H. S. 2001, ApJ, 558, 859 [NASA ADS] [CrossRef] [Google Scholar]
 De Pontieu, B., McIntosh, S. W., Carlsson, M., et al. 2007, Science, 318, 1574 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 DeForest, C. E. 2007, ApJ, 661, 532 [NASA ADS] [CrossRef] [Google Scholar]
 Edwin, P. M., & Roberts, B. 1983, Sol. Phys., 88, 179 [NASA ADS] [CrossRef] [Google Scholar]
 Erdélyi, R., & Morton, R. J. 2009, A&A, 494, 295 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Fontenla, J. M., Avrett, E., Thuillier, G., & Harder, J. 2006, ApJ, 639, 441 [NASA ADS] [CrossRef] [Google Scholar]
 Goossens, M., Arregui, I., Ballester, J. L., & Wang, T. J. 2008, A&A, 484, 851 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 He, J., Marsch, E., Tu, C., & Tian, H. 2009a, ApJ, 705, L217 [NASA ADS] [CrossRef] [Google Scholar]
 He, J.S., Tu, C.Y., Marsch, E., et al. 2009b, A&A, 497, 525 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Hillier, A., Morton, R. J., & Erdélyi, R. 2013, ApJ, 779, L16 [NASA ADS] [CrossRef] [Google Scholar]
 Jing, J., Yuan, Y., Reardon, K., et al. 2011, ApJ, 739, 67 [Google Scholar]
 Judge, P. G., & Carlsson, M. 2010, ApJ, 719, 469 [NASA ADS] [CrossRef] [Google Scholar]
 Katsukawa, Y., Berger, T. E., Ichimoto, K., et al. 2007, Science, 318, 1594 [NASA ADS] [CrossRef] [Google Scholar]
 Kobelski, A. R., Saar, S. H., Weber, M. A., McKenzie, D. E., & Reeves, K. K. 2014, Sol. Phys., 289, 2781 [NASA ADS] [CrossRef] [Google Scholar]
 Kuridze, D., Morton, R. J., Erdélyi, R., et al. 2012, ApJ, 750, 51 [NASA ADS] [CrossRef] [Google Scholar]
 Kuridze, D., Verth, G., Mathioudakis, M., et al. 2013, ApJ, 779, 82 [NASA ADS] [CrossRef] [Google Scholar]
 Leenaarts, J., Rutten, R. J., Reardon, K., Carlsson, M., & Hansteen, V. 2010, ApJ, 709, 1362 [NASA ADS] [CrossRef] [Google Scholar]
 Leka, K. D., & Metcalf, T. R. 2003, Sol. Phys., 212, 361 [NASA ADS] [CrossRef] [Google Scholar]
 Makita, M. 2003, Publications of the National Astronomical Observatory of Japan, 7, 1 [NASA ADS] [Google Scholar]
 Mathew, S. K., Zakharov, V., & Solanki, S. K. 2009, A&A, 501, L19 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Mathioudakis, M., Jess, D. B., & Erdélyi, R. 2013, Space Sci. Rev., 175, 1 [NASA ADS] [CrossRef] [Google Scholar]
 Meyer, K. A., Mackay, D. H., van Ballegooijen, A. A., & Parnell, C. E. 2013, Sol. Phys., 286, 357 [NASA ADS] [CrossRef] [Google Scholar]
 Morton, R. J. 2012, A&A, 543, A6 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Morton, R. J., & Erdélyi, R. 2009, ApJ, 707, 750 [NASA ADS] [CrossRef] [Google Scholar]
 Morton, R. J., & McLaughlin, J. A. 2013, A&A, 553, A10 [Google Scholar]
 Morton, R. J., Ruderman, M. S., & Erdélyi, R. 2011, A&A, 534, A27 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Morton, R. J., Verth, G., Jess, D. B., et al. 2012a, Nat. Commun., 3, 1315 [NASA ADS] [CrossRef] [Google Scholar]
 Morton, R. J., Verth, G., McLaughlin, J. A., & Erdélyi, R. 2012b, ApJ, 744, 5 [NASA ADS] [CrossRef] [Google Scholar]
 Morton, R. J., Verth, G., Fedun, V., Shelyag, S., & Erdélyi, R. 2013, ApJ, 768, 17 [NASA ADS] [CrossRef] [Google Scholar]
 Morton, R. J., Verth, G., Hillier, A., & Erdélyi, R. 2014, ApJ, 784, 29 [NASA ADS] [CrossRef] [Google Scholar]
 Nakariakov, V. M., & Ofman, L. 2001, A&A, 372, L53 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Nakariakov, V. M., & Roberts, B. 1995, Sol. Phys., 159, 213 [NASA ADS] [CrossRef] [Google Scholar]
 Nakariakov, V. M., & Verwichte, E. 2005, Liv. Rev. Sol. Phys., 2, 3 [Google Scholar]
 Nakariakov, V. M., Ofman, L., Deluca, E. E., Roberts, B., & Davila, J. M. 1999, Science, 285, 862 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Okamoto, T. J., & De Pontieu, B. 2011, ApJ, 736, L24 [NASA ADS] [CrossRef] [Google Scholar]
 Pascoe, D. J., Wright, A. N., & De Moortel, I. 2011, ApJ, 731, 73 [NASA ADS] [CrossRef] [Google Scholar]
 Pascoe, D. J., Hood, A. W., de Moortel, I., & Wright, A. N. 2012, A&A, 539, A37 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Pereira, T. M., De Pontieu, B., & Carlsson, M. 2012, ApJ, 759, 16 [NASA ADS] [CrossRef] [Google Scholar]
 Pietarila, A., Aznar Cuadrado, R., Hirzberger, J., & Solanki, S. K. 2011, ApJ, 739, 92 [NASA ADS] [CrossRef] [Google Scholar]
 Roberts, B., Edwin, P. M., & Benz, A. O. 1984, ApJ, 279, 857 [NASA ADS] [CrossRef] [Google Scholar]
 Ruderman, M. S. 2009, A&A, 506, 885 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Ruderman, M. S. 2010, Sol. Phys., 267, 377 [NASA ADS] [CrossRef] [Google Scholar]
 Ruderman, M. S. 2011, Sol. Phys., 271, 41 [NASA ADS] [CrossRef] [Google Scholar]
 Ruderman, M. S., & Erdélyi, R. 2009, Space Sci. Rev., 149, 199 [NASA ADS] [CrossRef] [Google Scholar]
 Ruderman, M. S., & Roberts, B. 2002, ApJ, 577, 475 [NASA ADS] [CrossRef] [Google Scholar]
 Ruderman, M. S., & Scott, A. 2011, A&A, 529, A33 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Ruderman, M. S., Verth, G., & Erdélyi, R. 2008, ApJ, 686, 694 [NASA ADS] [CrossRef] [Google Scholar]
 Rueedi, I., Solanki, S. K., & Livingston, W. C. 1995, A&A, 293, 252 [NASA ADS] [Google Scholar]
 Rutten, R. J. 2006, in Solar MHD Theory and Observations: A High Spatial Resolution Perspective, eds. J. Leibacher, R. F. Stein, & H. Uitenbroek, ASP Conf. Ser., 354, 276 [Google Scholar]
 Schad, T. A., Penn, M. J., & Lin, H. 2013, ApJ, 768, 111 [Google Scholar]
 Shimizu, T., Kubo, M., Tarbell, T. D., et al. 2007, in New Solar Physics with SolarB Mission, eds. K. Shibata, S. Nagata, & T. Sakurai, ASP Conf. Ser., 369, 51 [Google Scholar]
 Soler, R., Terradas, J., & Goossens, M. 2011a, ApJ, 734, 80 [NASA ADS] [CrossRef] [Google Scholar]
 Soler, R., Terradas, J., Verth, G., & Goossens, M. 2011b, ApJ, 736, 10 [NASA ADS] [CrossRef] [Google Scholar]
 Soler, R., Andries, J., & Goossens, M. 2012, A&A, 537, A84 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Soler, R., Díaz, A. J., Ballester, J. L., & Goossens, M. 2013, A&A, 551, A86 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Spruit, H. C. 1982, Sol. Phys., 75, 3 [NASA ADS] [CrossRef] [Google Scholar]
 Suematsu, Y., Tsuneta, S., Ichimoto, K., et al. 2008, Sol. Phys., 249, 197 [NASA ADS] [CrossRef] [Google Scholar]
 TerraHomem, M., Erdélyi, R., & Ballai, I. 2003, Sol. Phys., 217, 199 [NASA ADS] [CrossRef] [Google Scholar]
 Terradas, J., Goossens, M., & Verth, G. 2010, A&A, 524, A23 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Tian, H., Curdt, W., Marsch, E., & Schühle, U. 2009a, A&A, 504, 239 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Tian, H., Curdt, W., Teriaca, L., Landi, E., & Marsch, E. 2009b, A&A, 505, 307 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Tomczyk, S., & McIntosh, S. W. 2009, ApJ, 697, 1384 [NASA ADS] [CrossRef] [Google Scholar]
 Tomczyk, S., McIntosh, S. W., Keil, S. L., et al. 2007, Science, 317, 1192 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Uchida, Y. 1970, PASJ, 22, 341 [NASA ADS] [Google Scholar]
 Van Doorsselaere, T., Debosscher, A., Andries, J., & Poedts, S. 2004, A&A, 424, 1065 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 van Doorsselaere, T., Verwichte, E., & Terradas, J. 2009, Space Sci. Rev., 149, 299 [NASA ADS] [CrossRef] [Google Scholar]
 Verth, G., & Erdélyi, R. 2008, A&A, 486, 1015 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Verth, G., Erdélyi, R., & Jess, D. B. 2008, ApJ, 687, L45 [NASA ADS] [CrossRef] [Google Scholar]
 Verth, G., Terradas, J., & Goossens, M. 2010, ApJ, 718, L102 [NASA ADS] [CrossRef] [Google Scholar]
 Verth, G., Goossens, M., & He, J.S. 2011, ApJ, 733, L15 [NASA ADS] [CrossRef] [Google Scholar]
 Verwichte, E., Foullon, C., & Van Doorsselaere, T. 2010a, ApJ, 717, 458 [NASA ADS] [CrossRef] [Google Scholar]
 Verwichte, E., Marsh, M., Foullon, C., et al. 2010b, ApJ, 724, L194 [NASA ADS] [CrossRef] [Google Scholar]
 Verwichte, E., Van Doorsselaere, T., Foullon, C., & White, R. S. 2013a, ApJ, 767, 16 [NASA ADS] [CrossRef] [Google Scholar]
 Verwichte, E., Van Doorsselaere, T., White, R. S., & Antolin, P. 2013b, A&A, 552, A138 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Watko, J. A., & Klimchuk, J. A. 2000, Sol. Phys., 193, 77 [NASA ADS] [CrossRef] [Google Scholar]
 WedemeyerBöhm, S. 2008, A&A, 487, 399 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Yuan, D., & Nakariakov, V. M. 2012, A&A, 543, A9 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
All Figures
Fig. 1
Hinode SOT field of view. The image also shows the position of the Ca ii limb (black solid line), and the central axis of the spicule (solid white). Crosscuts are taken perpendicular to this central axis. 

In the text 
Fig. 2
The observed kink motion. The left hand column panel shows timedistance diagrams from various crosscuts. Each crosscut shown is separated by 800 km, with the lowest crosscut on the top row. The right hand column shows the results of the Gaussian fits (crosses) with the σ error bars on the measured position. The solid line is the result of the damped sinusoidal fit. The given distance corresponds to the position along the crosscut and the time is seconds from 01:20:51 UT. 

In the text 
Fig. 3
Measured wave properties. The left panel displays the measured displacement amplitude (stars) as a function of height in the atmosphere relative to τ_{5000} = 1. The vertical bars shows the σ error on the measured quantity. The solid black line corresponds to the cubic fit to the amplitude profile and the dashed lines show the 2σ (95%) confidence level of the fit. The middle panel displays the lag value measured from crosscorrelation of neighbouring timedistance diagrams separated by 40 km (red stars) and 80 km (black diamonds). The red and black solid lines are the corresponding exponential fits to measured lags. The right hand panel displays the phase speed calculated from the fits to the lag data points. The red and black dashed lines correspond to the σ confidence levels for the phase speeds. 

In the text 
Fig. 4
Measured and estimated spicule widths as a function of height in the atmosphere relative to τ_{5000} = 1. The diamond data points are the spicule widths determined form the fitting of a Gaussian to the crosssectional flux profile. The crosses are the estimates for the physical diameter of the spicule calculated from the modelling (referred to as the estimated width). The error bars correspond to the standard error. 

In the text 
Fig. 5
Flows along the spicule. The image shows a timedistance diagram generated from the unsharp masked data and taken parallel to the spicule axis. The straight lines highlight the measured upflows and the measured flow speeds are given. The time is shown in seconds from 01:18:11 UT. 

In the text 
Fig. 6
Magnetoseismological estimates of plasma gradients as a function of height in the atmosphere relative to τ_{5000} = 1. The left hand panel shows the magnetoseismologically determined radial expansion (solid line) with the 95% confidence level shown (dashed lines). The diamonds and crosses show the expansion inferred from the measurements of the Gaussian width and modelling (estimated), respectively, with standard errors given. The middle panel shows magnetoseismological estimate for the gradient of the magnetic field (solid) and the inferred magnetic expansion (crosses). The right hand panel is the density gradient determined using the measured displacement amplitude (solid) with 95% confidence intervals (dashed), and a combination of the modelled (estimated) width and measured phase speed (crosses). The red lines are exponential fits to the data points. 

In the text 
Fig. 7
Spatially and temporally averaged intensity profiles (left panel) for the penumbra (black solid), the plage (blue dash) and the spicule (red dashdot) as a function of height in the atmosphere relative to τ_{5000} = 1. The right panel shows the calculated intensity scale heights for each feature. 

In the text 
Fig. 8
Modelling the predicted density profile along a spicule from magnetoseismology. The data points are the measured change in average density along the spicule. The red dash line is a normalised density profile (H_{e}) for the ambient plasma, designed as a simplified model of the classic hydrostatic solar atmosphere. The blue dashdot lines show two different normalised internal (spicule) density profiles (H_{s,1},H_{s,2}). The solid black lines show the average normalised density profiles calculated using the different internal density profiles. 

In the text 
Fig. 9
Evidence for wave damping. The plot shows the amplitude measured from the spicule oscillations (blue stars) and the amplitude determined from the estimated expansion and the phase speed measurements (black crosses). The error bars are the σ errors for each quantity. The black solid lines correspond to exponential fits to each amplitude profile. The diamonds shows the expected amplitude from wave damping. 

In the text 
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