(2016), the authors attempt to exploit the catalogue of events to do just this. By modelling, we refer to using the observational data to test theoretical ideas of wave behaviour by fitting an expected model. However, these resources have yet to be exploited effectively, with only simple modelling of individual observed wave events. The result of these fortuitous circumstances means that there is plenty of high quality data on kink waves, which can be used for probing the physics of the waves and the local plasma. Further, the almost continuous coverage of Solar Dynamic Observatory (SDO), supplemented with numerous ground-based data sets and Hinode data, has led to the existence of a large catalogue of wave events. In particular, the transverse kink motions of magnetic structures in the chromosphere and corona has received a great deal of attention, mainly due to their suitability for energy transfer and also their ability for providing diagnostics of the local plasma environment via coronal or solar magnetoseismology.Ĭurrent instrumentation has demonstrated the capabilities required to accurately measure the motions of the fine-scale magnetic structure, with high spatial and temporal resolution and high signal-to-noise levels. The Sun’s atmosphere is known to be replete with magnetohydrodynamic (MHD) wave phenomena and current instrumentation has enabled the measurement of the waves and their properties. Key words: Sun: corona / waves / magnetohydrodynamics (MHD) / Sun: oscillations Further, we use the model comparison to provide evidence of time-dependent wave properties of a kink oscillation, attributing the behaviour to the thermodynamic evolution of the local plasma. This supports previous analysis from Pascoe et al. The model comparison techniques provide evidence that a Gaussian damping profile provides a better description of the observed wave attenuation than the often used exponential profile. To demonstrate the methodology, an observation of an oscillating coronal loop undergoing standing kink motion is used. We also highlight the importance of including any observational trend line in the model-fitting process. In particular we discuss the Kolmogorov-Smirnoff one and two sample tests, as well as the runs test. We demonstrate that the residuals between the model and observations contain significant information about the ability for the model to describe the observations, and show how they can be assessed using various statistical tests. The methodology exploits least-squares fitting to compare models to observational data. In the process, we also aim to investigate the physics of coronal loop oscillations. The aim here is to introduce some robust statistical techniques for model comparison to the solar waves community, drawing on the experiences from other areas of astrophysics. However, the techniques employed for model comparison have generally been unsuitable and can lead to erroneous conclusions about the best model. Some studies have already begun to undertake this process. Improvements in instrumentation and the techniques used for measurement of the waves now enables subtleties of competing theoretical models to be compared with the observed waves behaviour. Observations of the solar atmosphere have shown that magnetohydrodynamic waves are ubiquitous throughout. Astronomical objects: linking to databasesĭepartment of Mathematics & Information Sciences, Northumbria University, Newcastle Upon Tyne, NE1 8ST, UKĪims.Including author names using non-Roman alphabets.
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