Photospheric Observations of Surface and Body Modes in Solar Magnetic Pores

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 designati...

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Bibliographic Details
Published in:The Astrophysical journal 2018-04, Vol.857 (1), p.28
Main Authors: Keys, Peter H., Morton, Richard J., Jess, David B., Verth, Gary, Grant, Samuel D. T., Mathioudakis, Mihalis, Mackay, Duncan H., Doyle, John G., Christian, Damian J., Keenan, Francis P., Erdélyi, Robertus
Format: Article
Language:English
Subjects:
Astrophysics
Fluid flow
magnetic fields
Magnetohydrodynamic waves
Magnetohydrodynamics
magnetohydrodynamics (MHD)
Photosphere
Photospheric observations
Pores
Signatures
Solar atmosphere
Sun: activity
Sun: evolution
Sun: oscillations
Sun: photosphere
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Summary: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 for 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 that 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, as well as that surface modes appear to carry more energy than those displaying signatures of body modes. We find frequencies in the range of ∼2-12 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 from those presented here.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/aab432