Abstract
Simultaneous measurements of the magnetic fields in the photosphere and chromosphere were used to investigate if magnetic flux is submerging at sites between adjacent opposite polarity magnetic network elements in which the flux is observed to decrease or ‘cancel’. These data were compared with chromospheric and coronal intensity images to establish the timing of the emission structures associated with these magnetic structures as a function of height. We found that most of the cancelation sites show either that the bipole is observed longer in the photosphere than in the chromosphere and corona (44%) or that the timing difference of the disappearance of the bipole between these levels of the atmosphere is unresolved. The magnetic axis lengths of the structures associated with the cancelation sites are on average slightly smaller in the chromosphere than the photosphere. These observations suggest that magnetic flux is retracting below the surface for most, if not all, of the cancelation sites studied.
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Harvey, K.L., Jones, H.R., Schrijver, C.J., Penn, M.J. (2000). Does Magnetic Flux Submerge at Flux Cancelation Sites?. In: Engvold, O., Harvey, J.W. (eds) Physics of the Solar Corona and Transition Region. Springer, Dordrecht. https://doi.org/10.1007/978-94-017-3429-5_3
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DOI: https://doi.org/10.1007/978-94-017-3429-5_3
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