Measuring the magnetic field of a trans-equatorial loop system using coronal seismology
“EIT waves” are freely-propagating global pulses in the low corona which are strongly associated with the initial evolution of coronal mass ejections (CMEs). They are thought to be large–amplitude, fast–mode magnetohydrodynamic waves initially driven by the rapid expansion of a CME in the low corona. An “EIT wave” was observed on 6 July 2012 to impact an adjacent trans–equatorial loop system which then exhibited a decaying oscillation as it returned to rest. Observations of the loop oscillations were used to estimate the magnetic field strength of the loop system by studying the decaying oscillation of the loop, measuring the propagation of ubiquitous transverse waves in the loop and extrapolating the magnetic field from observed magnetograms. Observations from the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory (SDO/AIA) and the Coronal Multi-channel Polarimeter (CoMP) were used to study the event. An Empirical Mode Decomposition analysis was used to characterise the oscillation of the loop system in CoMP Doppler velocity and line width and in AIA intensity. The loop system was shown to oscillate in the 2nd harmonic mode rather than at the fundamental frequency, with the seismological analysis returning an estimated magnetic field strength of G. This compares to the magnetic field strength estimates of 1–9 G and 3–9 G found using the measurements of transverse wave propagation and magnetic field extrapolation respectively.
First observed by the Solar and Heliospheric Observatory , many theories have been proposed to interpret globally–propagating coronal disturbances (commonly called “EIT waves”). Taking their name from the Extreme ultraviolet Imaging Telescope  onboard SOHO, they are typically observed as radially expanding bright features associated with the onset of a coronal mass ejection (CME) that can traverse the solar disk in under an hour . After almost 20 years of detailed investigation and debate, a consensus is finally being reached with regard to the physics underpinning their evolution, thanks to the improved temporal and spatial resolution of the Solar and Terrestrial Relations Observatory  and more recently the Solar Dynamics Observatory .
The multitude of theories proposed to explain this phenomenon is mainly the result of conflicting observations . Initially interpreted as the coronal counterpart of the chromospheric Moreton–Ramsey wave , “EIT waves” were treated as fast–mode magneto–acoustic (MHD) waves following the example of . However, issues with this interpretation were raised by observations of stationary brightenings at the edges of coronal holes . These observations led to the suggestion that “EIT waves” were not true “waves” but instead were a brightening produced by the restructuring of the magnetic field during the eruption of a CME. It was proposed that this brightening was alternatively produced by Joule heating at the interface between the magnetic field of the erupting CME and the surrounding coronal magnetic field , continuous reconnection of small–scale magnetic loops driven by the erupting CME  or the stretching of magnetic field lines overlying an erupting flux rope . This last scenario was also supported by the relatively low observed speed of the disturbances .
However, these hypotheses have been undermined both by observations of reflection and refraction at coronal hole and active region boundaries  as well as the higher speeds measured using STEREO  and SDO . Although initially analysed using the linearised fast–mode wave equations, observations of pulse dispersion and deceleration  have led to their interpretation as large–amplitude simple waves  initially driven by the rapid expansion of the erupting CME in the low corona  before propagating freely. Note that a number of different reviews by , , ,  and more recently  discuss the different interpretations and the observations both supporting and contradicting them in detail.
More recently, the higher temporal and spatial resolution provided by the Atmospheric Imaging Assembly  has revolutionised our understanding of “EIT waves”. These improved observations are providing clear evidence that the freely propagating “EIT waves” behave as waves, in principle allowing their observed characteristics to be used as diagnostics of the physical properties of the coronal regions through which they propagate  and estimate properties such as magnetic field strength . A similar approach may also be applied on a more local scale, using the forced oscillations of coronal loops initially driven by the impact of an “EIT wave” to determine properties such as their magnetic field strength or the energy of the wave-pulse .
While the global nature of “EIT waves” greatly increases the chances of them interacting with coronal loops, these observations are dependent on a sufficiently high temporal and spatial resolution to be able to identify the oscillating loop. Despite its global field-of-view, SOHO/EIT did not have a sufficiently high temporal or spatial resolution to identify oscillating loops. This changed with the launch of the Transition Region And Coronal Explorer , whose observations were used to show that the oscillation of a coronal loop may be used to estimate its magnetic field strength . Subsequent work extended the method to observations of oscillation in Doppler motion made by the Extreme ultraviolet Imaging Spectrometer  onboard the Hinode spacecraft .
In this paper, we estimate the magnetic field of a trans–equatorial loop system using multiple independent techniques. The first approach uses the oscillation of the loop system resulting from the impact of the global EUV wave-pulse, the second uses direct observations of the magnetic field made by the by the ground–based Coronal Multi–channel Polarimeter (CoMP) instrument , while the third estimates the field strength using two independent magnetic field extrapolations from the photosphere. This paper builds on work previously presented at the International Astronomical Union (IAU) Symposium on “Solar and Stellar Flares and Their Effects on Planets” , and represent a significant advance on the previously published proceedings paper. The observations are presented in Section , with the properties of the pulse and its interaction with the surrounding corona examined in Sections and respectively. This interaction is then used to derive the magnetic field strength associated with a nearby transequatorial loop system in Section . Finally, some conclusions about the implication of these observations are drawn in Section .
2Observations & Data Analysis
The solar eruption studied here originated from NOAA active region AR 11514 on 6 July 2012 and was associated with a CME and a GOES X1.1 class flare which began at 23:01 UT. The event was well observed by multiple instruments including SDO/AIA and CoMP (see Figure ?), providing an opportunity to study the eruption in detail. As with the event of 25 February 2014 previously studied by , the global EUV wave observed here did not propagate isotropically, (see Figure ?). Instead, due to the presence of the adjacent active regions AR 11515 to the East and ARs 11513, 11516 and 11517 to the North, the “EIT wave” propagated mainly towards the south polar coronal hole along the limb as seen by SDO/AIA (this is shown in the movie attached to Figure ).
Designed to study the coronal magnetic field, CoMP provides Stokes-I measurements in the 10747 Å and 10798 Å emission lines with a field of view of 2.8 R and an image size of pixels. This gives an image sample size of 4.25 arcsec pixel at 30 s cadence . Although the seeing was not good enough for this event to estimate the full Stokes parameters (S. Tomczyk, private communication), the Stokes-I measurements can be fitted using a least–squares Gaussian fit to estimate the line intensity, width and central wavelength for each pixel. This allows the plasma parameters to be studied, giving an estimate of the temporal variations in Doppler motion and line width in the low corona.
As the “EIT wave” was observed to propagate along the solar limb from the erupting active region towards the south pole, it was not possible to use the Coronal Pulse Identification and Tracking Algorithm  to study the propagation of the pulse. Instead, following , a polar deprojection was used to determine the variation in pulse kinematics across a height range from 1.01–1.12 R (as shown in Figure ?). This height range was chosen because above 1.12 R the pulse becomes very faint in the SDO/AIA images while the CoMP observations become noisy and prone to missing data, making direct comparisons between the instruments difficult.
The leading edge of the wave–pulse was manually identified and fitted using a quadratic model at each height across the entire range, as shown for height 1.09 R in Figure ?, with the process repeated 10 times in each case to minimise uncertainty. The pulse was found to have a velocity ranging from 607–1583 km s, with a mean velocity of 1106 km s and an acceleration ranging from – m s, with a mean acceleration of m s. These estimates are much higher than the average “EIT wave” speed measured by , indicating that the pulse measured here was quite fast. The pulse also exhibited clear deceleration, evidence of broadening and was associated with a Type 2@ radio burst , suggesting that it was a large amplitude wave pulse.
For such a fast and intense pulse it is possible to follow the approach of  and estimate its initial energy using the Sedov–Taylor approximation . Although this assumes a spherically symmetric blast wave emanating from a point source (which is not strictly valid here),  and  found that the approach is suitable for analysing the onset stage of pulses being initially driven over a very short time period before propagating freely, as with the event studied here.  have also shown that the Sedov–Taylor relation provides an excellent estimate of the initial energy of the eruption assuming a blast wave propagating through a medium of variable density. Using this approach, the initial energy of the pulse was estimated to be 8.610 ergs, comparable to the previous estimate made by . While this is consistent with the observations of high initial velocity and strong pulse deceleration, it is most likely an overestimate of the true energy of the wave-pulse. As noted by , the Sedov-Taylor relation assumes a spherical blast wave emanating from a source point, which is not the case here and does not include the effect of the coronal magnetic field. As a result, this estimate should be considered as a first order approximation of the energy of the pulse.
Although the pulse can be clearly identified in the AIA 193 Å intensity observations (e.g., Figure ), it was not as apparent in the CoMP intensity observations. This is clear from panel a of Figure , where the effects of the pulse can be seen in Doppler velocity, but not the pulse itself. As a result, the CoMP observations were used to study the effects of the pulse on the surrounding corona, with the AIA 193 Å observations used to estimate the pulse kinematics.
4Interaction with trans–equatorial loop system
Although the Sedov–Taylor approximation assumes an isotropic expansion of the wave–pulse being studied, this is not the case here due to the trans–equatorial loop system to the north of the erupting active region. This is shown in Figure ? and the associated movie movie1.mov. While this feature restricts the propagation of the wave–pulse, the effects of the impact force a significant displacement of the trans–equatorial loop system from rest. This results in a large amplitude decaying oscillation in CoMP Doppler observations as the loop returns to its pre-impact position, as shown in detail in Figure ? at a specific location of the observed loop structure. As a result, it is possible to estimate the magnetic field of the loop system using a coronal seismology approach .
The temporal variation in CoMP Doppler velocity and line width and AIA percentage base difference (PBD) intensity at a height of 1.09 R and for all polar angles are shown in the left panels (a,c,e) of Figure ?. The pulse is clearest in the Doppler velocity and AIA PBD measurements (panels a & e), although there is a slight suggestion of variation in the line width measurements (panel c). The wave–pulse is first seen in the Doppler velocity observations at 23:04 UT, with a slightly blue–shifted edge moving northwards away from the erupting active region (located at 110 clockwise from solar north). It can also be seen to move towards the south pole at roughly the same time, again observed as an initially slightly blue–shifted edge. A co-temporal faint bright feature can also be identified in the PBD measurements in panel e moving both north and south away from the source active region. Although there is some indication of a slight change in the line width shown in panel c at this time, there is no clear signature of a propagating front.
Following the initial front, there is clear evidence of material being ejected with the erupting CME. This is apparent from the red–shifted outflow from the erupting active region apparent in the sector from 100–120 starting at 23:07 UT and continuing for the rest of the time period shown. This corresponds to a drop in the PBD intensity (panel e of Figure ?), indicating a drop in density and/or temperature as material is evacuated by the CME. This drop in intensity is also clear in panel f, which shows the temporal variation in PBD intensity at 95 clockwise from solar north (as for panels b and d, shown by the dashed line in panel e).
While the propagation of the pulse to the south of the erupting active region is relatively uninhibited, the propagation to the north is modified by a trans–equatorial loop system located between 85–100 clockwise from solar north (as shown in Figure ?). The variation in Doppler velocity with time in panel a of Figure ? shows that this loop system is relatively stable until the impact of the blue–shifted wave–pulse at 23:05 UT. A more strongly blue–shifted feature is then observed between 23:07 UT and 23:17 UT along the profile in panel b, which is also characterised by a very strong co-temporal increase in line width (seen in panel d). This suggests turbulent behaviour , and is consistent with the initial impact of the wave–pulse on the loop system followed by the outward motion of the associated erupting filament.
The effects of the impact of the wave–pulse on the the trans–equatorial loop system may then be seen in panel a from 23:17 UT onwards as it exhibits a series of alternating red– and blue–shifted features. This can be attributed to the loop system being displaced from its rest position by the impact of the wave–pulse and subsequently returning to rest via a decaying oscillation. This behaviour is shown most clearly in panel b of Figure ?, which corresponds to the temporal Doppler velocity profile at an angle of clockwise from solar north (indicated by the dashed line in panel a). It should also be noted that as the Doppler velocity in panel b begins to exhibit this strong oscillation, the line width drops dramatically to near the pre-event level, suggesting a near-uniform oscillation of the loop system.
This oscillatory behaviour in the Doppler velocity is consistent along the loop as shown in Figure ?, which shows the variation in Doppler velocity at a set of sampled locations (height and polar angle) along the rest of the loop system. It is clear from the temporal evolution of the Doppler velocities shown in the left panels of Figure ? that the signal weakens above 1.14 R, with clear data drop-outs apparent at 95–110. While the amplitude of the oscillation can be seen to drop with increasing height, the period and damping time are comparable in all cases, suggesting that the values quoted in Figure ? are representative of the oscillation along the loop. These observations suggest that the wave-pulse impacts the leg of the loop system in the low corona (thus leading to the larger amplitude of the oscillation at lower heights). The consistent damping time also suggests that while the loop system is perturbed by the pulse impact, it stays relatively stable and is not opened by this impact. The mass of the loop system and hence the oscillation and associated damping coefficient therefore remain constant throughout the oscillation.
4.1Empirical Mode Decomposition analysis
While the oscillatory behaviour of the Doppler velocity is very clear in panel b of Figure ?, there is some indication of a comparable (albeit extremely faint) oscillation in the line width and PBD intensity shown in panels d & f. To determine if an oscillation was present, the temporal evolution of the different signals was examined using an Empirical Mode Decomposition  analysis. This technique decomposes the original signal into a series of Intrinsic Mode Functions (IMFs) and a residual, with the associated energy distribution represented by a Hilbert-Huang spectrum. The approach involves constructing a low- and a high-envelope from the series of maxima and minima of the the signal, and then averaging the two envelopes. Under certain constraints, the resulting function is called an IMF and captures the fastest oscillating part in the signal. A new signal is then obtained by subtracting the IMF from the signal itself. This process is repeated until the updated signal shows no more oscillation, leaving the residual, . Since IMFs are time-dependent, a convenient way of representing their contribution to the signal at each time is to use an Hilbert transform as defined by , which can be used to describe the time-evolution of the (instantaneous) frequency of each IMF.
The EMD analysis was applied to the Doppler velocity, line width and PBD intensity signals shown in panels b, d & f, respectively, of Figure ?. Note that in the following analysis we focus on the impact of the wave–pulse on the trans-equatorial loop system and its resulting oscillation, leaving a more detailed study of the correlation of the various IMFs between the different signals for a dedicated future work.
Figure ? shows the output from the EMD analysis, with the bottom panel for each column giving the original signal (black) and residual (red) while the upper panels give the corresponding IMFs. The left panels show that the Doppler velocity can be decomposed into three IMFs, with the oscillatory behavior mostly captured by IMF=3, which reveals an almost constant frequency of 1.0 mHz up to about t=3000s. While this approach can provide a more accurate estimate of the frequency of the oscillation, the composing IMFs are not orthogonal functions, leading to the crosstalk observed in the second half of the time series for IMF=2 & 3. The IMF=2 contribution also shows the presence of a more complex component which is not purely oscillatory in nature. The residual also shows an oscillatory behavior on a longer period than the loop oscillation. However, the oscillation in the residual is not complete and therefore the residual is not considered to be an IMF. The difference between the oscillatory Doppler signal and this longer component is best seen using a Hilbert-Huang Transform (HHT) as shown in Figure . The left panel here shows the HHT spectrum restricted to the residual and the IMF=3. The spectral contribution of the oscillatory component from IMF= 3 is represented by the intense red strip around 1 mHz which stays almost constant in frequency until s, before strongly damping and decreasing to 0.5 mHz, (cf. the left panel of Figure ). The residual contribution appears in this plot as a periodic, low-intensity component in the lower part of the spectrum at a frequency of 0.2 mHz.
The central panels of Figure ? show the decomposed IMF for the line width shown in panel d of Figure ?. Here the high-frequency IMFs=1 & 2 capture a transient nonlinear pulse in the time period s which has a period much shorter than the loop oscillation and cannot be clearly identified in the Doppler signal (except for a small-amplitude trace in the IMF=1 of the left-hand column of Figure ?). The frequency of the IMF=2 in Figure can be seen to chirp in time from 1.5 to 3.5 mHz, whereas the evolution of the IMF=1 is less clear. However for clarity neither IMF is included in Figure . These signals are clearly different to the loop system damped oscillation (mostly captured in Figure by IMF=3), which again reproduces the component of the oscillating loop system in the IMF=3 of the Doppler velocity signal (although at a slightly more variable frequency between 0.5 and 1 mHz, see the central panel in Figure ), and a lower frequency component at about 0.4 mHz.
The IMF decomposition of the AIA signal in the right panels of Figure ? shows the highest level of complexity, partly due to the higher cadence of the AIA signal which captures more time-scales than CoMP. Despite this, both loop-system oscillation components can be identified with a clear damping signature (e.g., IMF=4), and the nonlinear signal due to the wave–pulse itself (e.g., IMF=2). In the HHT shown in the far right panel of Figure , the frequency of the oscillating mode is similar to the one generated by the IMF=3 of the CoMP line-width signal, albeit relatively weaker. Similarly, the 0.2 mHz signal is also found in the PBD intensity from AIA. The effects of the higher AIA cadence are seen in the highest-frequency IMF=1, which has the typical signature of noise and/or under-sampling (i.e., fluctuations on the highest frequency, whereas all higher IMFs are resolved signals).
The initial transients apparent in the IMF=1 of the CoMP line width and in the IMF=2 of the AIA PBD intensity are very similar in both structure and timing. The transients occur at the time the pulse reaches the trans-equatorial loop system, and appear as an oscillating wave modulated by an envelope rather than as a damped oscillation. It is intriguing that exactly such a pattern was previously assumed as the internal structure of an “EIT wave” pulse by  and we are therefore tempted to identify this transient signal as the pulse itself.
However, if our pulse velocity estimate measured in Section 3 can also be applied at the front impacting the trans-equatorial loop system, this signal would indicate a pulse much broader than that observed. Therefore, we cannot unequivocally exclude that the observed transient signals are due to other nonlinear interactions between the pulse and loop systems. The case studied here is not optimal for discriminating between these possibilities and we leave such an analysis to a future work.
5Magnetic field strength estimates
The EMD analysis suggests that the oscillation of the loop system is consistent with the fast magneto-acoustic kink mode as modelled by , with the clear Doppler velocity signal indicating a large-scale motion of the loop system towards and away from the observer. Figure ? shows a damped oscillatory component present in both the line width and PBD intensity signals that has a period comparable to that observed in the Doppler velocity signal. However, it is very small and is most likely due to the apparent brightening and dimming as the loop system moves towards and away from the observer . This interpretation also means that it may be possible to use the oscillation of the loop system to estimate its magnetic field via coronal seismology (Section Section 5.1).
Although CoMP was originally designed to measure the coronal magnetic field, the seeing was not good enough for this event to make measurements of the full Stokes-I, Q, U and V parameters. Instead, a magnetoseismology technique developed by  and  was used to estimate the magnetic field strength of the loop system (Section Section 5.2). This approach does not require any oscillation of the loop system, allowing an independent verification of the values derived from the coronal seismology technique. To provide an additional independent verification, the magnetic field was also estimated using a pair of magnetic field extrapolations derived from both GONG and HMI magnetograms (Section Section 5.3).
The coronal seismology approach most commonly used to estimate the magnetic field within an oscillating coronal loop uses the damping of the loop as it returns to its original rest position to derive the period of oscillation. This is done by fitting the damped oscillation using an exponentially decreasing cosine function of the form,
where is the amplitude, is the period, is the phase, is the damping time and is the equilibrium position. This model was applied to the variation in Doppler velocity shown in panel b of Figure ?, with the resulting fit shown by the blue line and the fitted values given in the bottom right of the panel. It is clear that the model fits the observations very well, indicating that the assumption of a kink mode oscillation is consistent with the observations. The model was then applied to the Doppler velocity along the loop system, with Figure ? showing a representative sample of profiles with the blue line in each case showing the model fit to the data. It is clear that the oscillation is exhibited along the loop system at a range of heights and locations, with the model providing an excellent fit to the data in each case.
Although the oscillation of the loop system may be interpreted as as a kink mode wave as discussed in Section 4.1, it is not oscillating at the fundamental frequency. Instead, the out of phase Doppler signal observed between the legs of the loop system (apparent between 90-100 in the Doppler velocity plots shown in Figures ? and ?) and the lack of a signal at the top of the loop system suggest that it is oscillating at the 2nd harmonic frequency. The oscillation period can therefore be used to estimate the strength of the magnetic field of the loop using the equation,
where is the magnetic field strength, is the loop length, is the period of the oscillation, is the internal density of the loop system and is the external density of the surrounding corona .
The length of the loop was estimated by fitting an ellipse to the loop identified by visual inspection in the SDO/AIA observations. This was done using the 193 Å passband, with the images processed using the Multiscale Gaussian Normalisation technique of  to highlight the loop and make it easier to identify. The process was repeated ten times to reduce uncertainty, with the loop length estimated at 7118 Mm.
The density of the loop system and the surrounding corona were estimated using the regularised inversion technique of  assuming a temperature of 1.5 MK (corresponding to the peak emission temperature of the 193 Å passband used to identify the wave–pulse). The spatial extent of the loop system was estimated using observations from the STEREO-A spacecraft to be 373 Mm. This was used as the line-of-sight along which to integrate the emission measure for both the internal and external densities of the loop system. The internal density of the loop system at the location used to identify the oscillation in Doppler velocity was found using the emission measure at that location, with a mean internal density of cm found across the loop system. In contrast, the external density was estimated using the mean density value for a 10 degree wide region of quiet Sun centered at 45 degrees clockwise from solar north at a comparable height to the measurement being made. This is indicated by the arc sector shown in Figure , and returned a mean external density of cm across the heights studied here.
Equation 2 was then used to estimate the magnetic field strength for a representative range of five oscillation periods and corresponding internal and external densities estimated along the loop. This returned an estimated magnetic field strength of G within the loop system. While this is comparable to previous estimates using coronal seismology , suggesting that the approach is valid, it is quite low. There are most likely several reasons for this discrepancy. The oscillation observed here is the 2nd harmonic rather than the fundamental mode as is typically observed . In addition, while every attempt has been made to minimise the uncertainty associated with this measurement, the large-scale nature of the loop system and the diffuse nature of the wave-pulse suggest that it is most likely a minimum uncertainty estimate.
5.2Direct measurement using CoMP
The magnetic field of the coronal loop can also be estimated from observations using magnetoseismology of the propagating transverse waves previously seen to be ubiquitous in CoMP Doppler velocities . This offers an independent approach to estimate the magnetic field strength within the loop system. Following the approach developed by , a coherence based method was used to track velocity perturbations in the Doppler velocities obtained from the 3-point 10747 Å observations taken between 20:24:14–21:30:14 UT. This allowed both the direction and speed of the propagation to be measured as shown in the top right panel of Figure ?.
The density of the loop system was estimated using the line centroid wavelength intensities from the 5-point 10747 Å and 10798 Å data taken in the period 18:43:51–19:52:42 UT. This line pair is density sensitive  and allows an estimate of the coronal density to be made for 12 pairs of 10747 Å and 10798 Å images  using the methodology outlined in . It was assumed that the variability of the density estimates between image pairs gives an reasonable estimate of the uncertainty associated with the density, not including any systematic errors associated with the uncertainties in atomic physics. The relative uncertainty in density is typically on the order of , although it reaches in regions away from the loop of interest. Note that the observed emission from 10798 Å is weaker than that from 10747 Å, and the signal to noise ratio rises at a much greater rate as a function of height in the corona. The region of high quality signal in 10798 Å is delimited by a white contour on the 10747 Å image in the top left panel of Figure ? and the estimated plasma density is shown in the bottom left panel of Figure ?.
The phase speed of the observed transverse waves is given by the kink speed,
where is the permeability of a vacuum and and refer to loop and ambient plasma values respectively . Assuming that and taking the average density , an estimate for the magnetic field is given by, The average density is used as it reflects the fact that many oscillating structures are likely present within a single CoMP pixel . As a result, both internal and ambient plasma will contribute to the observed emission. The estimated propagation speed and density may then be used to estimate the magnetic field, the results of which are displayed in the bottom right panel of Figure . The associated uncertainties are typically , reflecting the low errors associated with propagation speed determination.
5.3Magnetic field extrapolation
A final independent estimate was made using the magnetic field extrapolated from photospheric magnetogram observations, comparable with previous approaches . In this case, two Potential Field Source Surface (PFSS) extrapolations were used to estimate the magnetic field in the solar corona corresponding to the loop system impacted by the pulse (see Figure ?). The first extrapolation shown in the left panel of Figure ? used a GONG magnetogram as a basis and estimated the global corona magnetic field using the finite differences method developed by , also used in a study concerning the magnetic structure surrounding an AR . The second extrapolation (right panel of Figure ?) was obtained from the PFSS package within SolarSoft described by  using a SDO/HMI magnetogram as a basis.
Figure ? shows that the two magnetograms initially used to extrapolate the coronal magnetic field are slightly different, as would be expected given the different sensitivity and resolution of the two instruments. This discrepancy affects the resulting extrapolated magnetic fields, so that the strength of the magnetic field along the transequatorial loop system is slightly different in both cases. The GONG (SDO/HMI) extrapolations suggest a magnetic field of 5 G (10 G) in the legs of the loop system, with the magnetic field in both cases dropping to 1 G at the loop-top. Along the line of sight used in Figure ?, the extrapolations return estimates of 3.5 G and 8 G for the GONG and SDO/HMI magnetograms respectively.
Here, we have used several independent techniques to estimate the magnetic field strength within a trans-equatorial loop system following the impact of a global EUV wave-pulse. The initial impact of the wave-pulse drove a kink-mode oscillation of the loop system, allowing an estimate to be made of the magnetic field strength. This was then compared to the magnetic field strength obtained via magnetoseismology of the ubiquitous transverse waves previously observed by  and . Finally, both sets of data-driven estimates were compared to extrapolated magnetic field measurements. All estimates were found to be broadly similar, consistent with previous results. This builds on work previously presented at the IAU Symposium on “Solar and Stellar Flares and Their Effects on Planets”  by using multiple independent techniques including direct measurement using CoMP and EMD analysis of the CoMP Doppler oscillation to determine the magnetic field strength of the loop system.
While previous observations have shown coronal loop oscillations initially driven by the impact of a global EUV wave , this event is unique for several reasons. The trans-equatorial loop system was located adjacent to the erupting active region, with the result that the global EUV wave-pulse was only observed to propagate southward away from the active region. The eruption was also observed by the CoMP instrument, making it one of only a handful of events observed by CoMP . The oscillation of the loop system was only apparent in the CoMP measurements of Doppler velocity, indicating that the erupting active region was closer to the observer than the loop system along the line-of-sight.
This oscillation of the trans-equatorial loop system in CoMP Doppler velocity was identified along the loop, and was measured by fitting an exponentially decaying cosine function. It was found that while the amplitude of the oscillation decreased with height, the period and damping time were found to be comparable along the loop. This suggests that the wave-pulse initially impacted the leg of the loop, which is consistent with the large-scale nature of the loop system.
Despite the clear oscillation in CoMP Doppler velocity, no clear oscillation was observed in either the CoMP line width or the AIA intensity. However, oscillation was observed in both measurements when processed using an Empirical Mode Decomposition. This approach allowed an oscillation period and damping rate to be estimated from the line width and AIA intensity measurements, both of which are comparable to the CoMP Doppler velocity measurements, albeit with a slightly lower value. Although this suggests that the EMD approach may be beneficial for measuring oscillations in future observations, it should be noted that some component mixing was observed, which resulted in an overestimation of the oscillation frequency when fitted with a single frequency. Despite this, the signal in AIA intensity identified using the EMD analysis confirmed the kink mode nature of the oscillation.
The kink mode nature of the observed oscillation allowed an estimate to be made of the magnetic field strength within the loop system. The oscillation was measured across the loop at a range of heights and position angles, giving a mean magnetic field strength of G along the loop. This is comparable to the magnetic field strength of 1–9 G estimated using the independent magnetoseismology approach of . It is also comparable to the extrapolated magnetic field obtained from both HMI and GONG magnetograms, suggesting that the approach is valid, albeit within the limitations previously discussed by .
In addition to the oscillation of the loop system previously described, the EMD analysis may also have allowed information on the pulse itself to be discerned which is inaccessible without a time-frequency analysis. Two clear signals were identified in the CoMP line width and AIA intensity: the oscillation of the loop system and a nonlinear signal. This nonlinear signal may correspond to the global EUV wave-pulse itself, in which case it is observational confirmation of the suggestion previously made by  that global “EIT waves” may be treated as a linear superposition of sinusoidal waves within a Gaussian envelope. Alternatively it may be a complex signal resulting from the interaction of the pulse and the loop system. As this set of observations is not optimal for discriminating between these possibilities, we intend to identify and further investigate the signal in future work.
- Aschwanden, M. J., Fletcher, L., Schrijver, C. J., & Alexander, D. 1999, , 520, 880
- Aschwanden, M. J., & Schrijver, C. J. 2011, , 736, 102
- Attrill, G. D. R., Harra, L. K., van Driel-Gesztelyi, L., & Démoulin, P. 2007, , 656, L101
- Ballai, I., Erdélyi, R., & Pintér, B. 2005, , 633, L145
- Ballai, I. 2007, , 246, 177
- Ballai, I., Douglas, M., & Marcu, A. 2008, , 488, 1125
- Ballai, I., Jess, D. B., & Douglas, M. 2011, , 534, A13
- Brooks, D. H., Warren, H. P., Ugarte-Urra, I., & Winebarger, A. R. 2013, , 772, L19
- Chen, P. F., Wu, S. T., Shibata, K., & Fang, C. 2002, , 572, L99
- Chen, P. F., Fang, C., & Shibata, K. 2005, , 622, 1202
- Culhane, J. L., Harra, L. K., James, A. M., et al. 2007, , 243, 19
- Delaboudinière, J.-P., Artzner, G. E., Brunaud, J., et al. 1995, , 162, 291
- Delannée, C., & Aulanier, G. 1999, , 190, 107
- Delannée, C. 2000, , 545, 512
- Delannée, C., Török, T., Aulanier, G., & Hochedez, J.-F. 2008, , 247, 123
- Dere, K. P., Brueckner, G. E., Howard, R. A., et al. 1997, , 175, 601
- Domingo, V., Fleck, B., & Poland, A. I. 1995, , 162, 1
- Flower, D. R., & Pineau des Forets, G. 1973, , 24, 181
- Gallagher, P. T., & Long, D. M. 2011, , 158, 365
- Gopalswamy, N., Yashiro, S., Temmer, M., et al. 2009, , 691, L123
- Grechnev, V. V., Uralov, A. M., Slemzin, V. A., et al. 2008, , 253, 263
- Grechnev, V. V., Afanasyev, A. N., Uralov, A. M., et al. 2011, , 273, 461
- Guo, Y., Erdélyi, R., Srivastava, A. K., et al. 2015, , 799, 151
- Handy, B. N., Acton, L. W., Kankelborg, C. C., et al. 1999, , 187, 229
- Hannah, I. G., & Kontar, E. P. 2013, , 553, A10
- Harra, L. K., Williams, D. R., Wallace, A. J., et al. 2009, , 691, L99
- Huang, N. E., Shen, Z., Long, S. R., et al. 1998, Proceedings of the Royal Society of London Series A, 454, 903
- Kaiser, M.L., Kucera, T.A., Davilla, J.M., St. Cyr, O.C., Guhathakurta, M. & Christian, E. 2008, , 136, 5
- Kienreich, I. W., Muhr, N., Veronig, A. M., et al. 2013, , 286, 201
- Kwon, R.-Y., Kramar, M., Wang, T., et al. 2013, , 776, 55
- Landi, E., Del Zanna, G., Young, P. R., Dere, K. P., & Mason, H. E. 2012, , 744, 99
- Lemen, J. R., Title, A. M., Akin, D. J., et al. 2012, , 275, 17
- Liu, W., & Ofman, L. 2014, , 67
- Long, D. M., Gallagher, P. T., McAteer, R. T. J., & Bloomfield, D. S. 2008, , 680, L81
- Long, D. M., Gallagher, P. T., McAteer, R. T. J., & Bloomfield, D. S. 2011, , 531, A42
- Long, D. M., DeLuca, E. E., & Gallagher, P. T. 2011, , 741, L21
- Long, D. M., Williams, D. R., Régnier, S., & Harra, L. K. 2013, , 288, 567
- Long, D. M., Bloomfield, D. S., Gallagher, P. T., & Pérez-Suárez, D. 2014, , 66
- Long, D. M., Baker, D., Williams, D. R., et al. 2015, , 799, 224
- Long, D. M., Pérez-Suárez, D., & Valori, G. 2016, in A.G. Kosovichev et al. (eds.) Solar and Stellar Flares and their Effects on Planets, Proceedings IAU Symposium No. 320, 98.
- Long, D. M., Bloomfield, D. S., Chen, P. F., et al. 2017, , 292, 7
- Mandrini, C. H., Nuevo, F. A., Vásquez, A. M., et al. 2014, , 289, 4151
- Moreton, G. E. 1960, , 65, 494
- Moreton, G. E., & Ramsey, H. E. 1960, , 72, 357
- Moses, D., Clette, F., Delaboudinière, J.-P., et al. 1997, , 175, 571
- Morgan, H., & Druckmüller, M. 2014, , 289, 2945
- Morton, R. J., & McLaughlin, J. A. 2013, , 553, L10
- Morton, R. J., Tomczyk, S., & Pinto, R. 2015, Nature Communications, 6, 7813
- Morton, R. J., Tomczyk, S., & Pinto, R. F. 2016, , 828, 89
- Muhr, N., Veronig, A. M., Kienreich, I. W., et al. 2014, , 289, 4563
- Nakariakov, V. M., & Ofman, L. 2001, , 372, L53
- Nakariakov, V. M., & Verwichte, E. 2005, Living Reviews in Solar Physics, 2,
- Nitta, N. V., Schrijver, C. J., Title, A. M., & Liu, W. 2013, , 776, 58
- Patsourakos, S., Vourlidas, A., & Stenborg, G. 2010, , 724, L188
- Patsourakos, S., & Vourlidas, A. 2012, , 281, 187
- Pesnell, W. D., Thompson, B. J., & Chamberlin, P. C. 2012, , 275, 3
- Quek, S. T., Tua, P. S., & Wang, Q. 2003, Smart Materials and Structures, 12, 447
- Roberts, B., Edwin, P. M., & Benz, A. O. 1984, , 279, 857
- Schrijver, C. J., & DeRosa, M. L. 2003, , 212, 165
- Sedov, L. I. 1959, Similarity and Dimensional Methods in Mechanics, New York: Academic Press, 1959,
- Shen, Y., Liu, Y., Su, J., et al. 2013, , 773, L33
- Stangalini, M., Consolini, G., Berrilli, F., De Michelis, P., & Tozzi, R. 2014, , 569, A102
- Taylor, G. 1950, Royal Society of London Proceedings Series A, 201, 159
- Taylor, G. 1950, Royal Society of London Proceedings Series A, 201, 175
- Tian, H., Tomczyk, S., McIntosh, S. W., et al. 2013, , 288, 637
- Thompson, B. J., Plunkett, S. P., Gurman, J. B., et al. 1998, , 25, 2465
- Thompson, B. J., Reynolds, B., Aurass, H., et al. 2000, , 193, 161
- Thompson, B. J., & Myers, D. C. 2009, , 183, 225
- Tomczyk, S., McIntosh, S. W., Keil, S. L., et al. 2007, Science, 317, 1192
- Tomczyk, S., Card, G. L., Darnell, T., et al. 2008, , 247, 411
- Tomczyk, S., & McIntosh, S. W. 2009, , 697, 1384
- Tóth, G., van der Holst, B., & Huang, Z. 2011, , 732, 102
- Uchida, Y. 1968, , 4, 30
- Van Doorsselaere, T., Nakariakov, V. M., Young, P. R., & Verwichte, E. 2008, , 487, L17
- Van Doorsselaere, T., Nakariakov, V. M., & Verwichte, E. 2008, , 676, L73
- Veronig, A. M., Temmer, M., & Vršnak, B. 2008, , 681, L113
- Verwichte, E., Van Doorsselaere, T., Foullon, C., & White, R. S. 2013, , 767, 16
- Vršnak, B., & Lulić, S. 2000, , 196, 157
- Vršnak, B., & Lulić, S. 2000, , 196, 181
- Vršnak, B., & Cliver, E. W. 2008, , 253, 215
- Warmuth, A., Vršnak, B., Magdalenić, J., Hanslmeier, A., & Otruba, W. 2004, , 418, 1101
- Warmuth, A., Vršnak, B., Magdalenić, J., Hanslmeier, A., & Otruba, W. 2004, , 418, 1117
- Warmuth, A., & Mann, G. 2005, , 435, 1123
- Warmuth, A. 2007, Lecture Notes in Physics, Berlin Springer Verlag, 725, 107
- Warmuth, A. 2015, Living Reviews in Solar Physics, 12, 3
- West, M. J., Zhukov, A. N., Dolla, L., & Rodriguez, L. 2011, , 730, 122
- Yang, L., Zhang, J., Liu, W., Li, T., & Shen, Y. 2013, , 775, 39
- Zhukov, A. N. 2011, Journal of Atmospheric and Solar-Terrestrial Physics, 73, 1096