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Solar coronal magnetic fields derived using seismology techniques applied to omnipresent sunspot waves

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dc.contributor.author Jess, D. B
dc.contributor.author Reznikova, V. E
dc.contributor.author Ryans, R. S. I
dc.contributor.author Christian, D. J
dc.contributor.author Keys, P. H
dc.contributor.author Mathioudakis, M
dc.contributor.author Mackay, D. H
dc.contributor.author Krishna Prasad, S
dc.contributor.author Banerjee, D
dc.contributor.author Grant, S. D. T
dc.contributor.author Yau, S
dc.contributor.author Diamond, C
dc.date.accessioned 2020-11-17T14:20:54Z
dc.date.available 2020-11-17T14:20:54Z
dc.date.issued 2016-02
dc.identifier.citation Nature Physics, Vol. 12, No. 2, pp. 179-185 en_US
dc.identifier.issn 1745-2481
dc.identifier.uri http://prints.iiap.res.in/handle/2248/7145
dc.description Restricted Access © Macmillan Publishers Limited http://dx.doi.org/10.1038/nphys3544 en_US
dc.description.abstract Sunspots on the surface of the Sun are the observational signatures of intense manifestations of tightly packed magnetic field lines, with near-vertical field strengths exceeding 6,000 G in extreme cases. It is well accepted that both the plasma density and the magnitude of the magnetic field strength decrease rapidly away from the solar surface, making high-cadence coronal measurements through traditional Zeeman and Hanle effects difficult as the observational signatures are fraught with low-amplitude signals that can become swamped with instrumental noise. Magneto-hydrodynamic (MHD) techniques have previously been applied to coronal structures, with single and spatially isolated magnetic field strengths estimated as 9–55 G (refs 4,5,6,7). A drawback with previous MHD approaches is that they rely on particular wave modes alongside the detectability of harmonic overtones. Here we show, for the first time, how omnipresent magneto-acoustic waves, originating from within the underlying sunspot and propagating radially outwards, allow the spatial variation of the local coronal magnetic field to be mapped with high precision. We find coronal magnetic field strengths of 32 ± 5 G above the sunspot, which decrease rapidly to values of approximately 1 G over a lateral distance of 7,000 km, consistent with previous isolated and unresolved estimations. Our results demonstrate a new, powerful technique that harnesses the omnipresent nature of sunspot oscillations to provide magnetic field mapping capabilities close to a magnetic source in the solar corona. en_US
dc.language.iso en en_US
dc.publisher Nature Publishing Group en_US
dc.subject Solar physics en_US
dc.subject Stars en_US
dc.title Solar coronal magnetic fields derived using seismology techniques applied to omnipresent sunspot waves en_US
dc.type Article en_US


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