Photospheric observations of surface and body modes in solar magnetic pores
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Over the past number of years, great strides have been made in identifying the various low-order magnetohydrodynamic wave modes observable in a number of magnetic structures found within the solar atmosphere. However, one aspect of these modes that has remained elusive, until now, is their designation as either surface or body modes. This property has significant implications on how these modes transfer energy from the waveguide to the surrounding plasma. Here, for the first time to our knowledge, we present conclusive, direct evidence of these wave characteristics in numerous pores which were observed to support sausage modes. As well as outlining methods to detect these modes in observations, we make estimates of the energies associated with each mode. We find surface modes more frequently in the data, and also that surface modes appear to carry more energy than those displaying signatures of body modes. We find frequencies in the range of ~2 to 12 mHz with body modes as high as 11 mHz, but we do not find surface modes above 10 mHz. It is expected that the techniques we have applied will help researchers search for surface and body signatures in other modes and in differing structures to those presented here.
Keys , P H , Morton , R J , Jess , D B , Verth , G , Grant , S D T , Mathioudakis , M , Mackay , D H , Doyle , J G , Christian , D J , Keenan , F P & Erdélyi , R 2018 , ' Photospheric observations of surface and body modes in solar magnetic pores ' Astrophysical Journal , vol 857 , no. 1 , 28 . DOI: 10.3847/1538-4357/aab432
© 2018, American Astronomical Society. This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.3847/1538-4357/aab432
DescriptionP.H.K. and R.J.M. are grateful to the Leverhulme Trust for the award of Early Career Fellowships. D.B.J. wishes to thank the UK Science and Technology Facilities Council (STFC) for the award of an Ernest Rutherford Fellowship alongside a dedicated Research Grant. D.B.J. and S.D.T.G. also wish to thank Invest NI and Randox Laboratories Ltd. for the award of a Research & Development Grant (059RDEN-1) that allowed this work to be undertaken. M.M. and F.P.K. acknowledge support from the STFC Consolidated Grant to Queen's University Belfast. R.E. acknowledges the support received from the Royal Society. Armagh Observatory is funded by the Northern Ireland Department of Communities. Observations were obtained at the National Solar Observatory, operated by the Association of Universities for Research in Astronomy, Inc. (AURA), under cooperative agreement with the National Science Foundation.
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