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Magnetic structure of sunspot under the photosphere

Published online by Cambridge University Press:  21 October 2010

Elena A. Kirichek
Affiliation:
Central (Pulkovo) Observatory, Russian Academy of Sciences, St. Petersburg, 196140Russia email: [email protected]
Alexandr A. Solov'ev
Affiliation:
Central (Pulkovo) Observatory, Russian Academy of Sciences, St. Petersburg, 196140Russia email: [email protected]
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In recent years, the local helioseismology has become a highly effective tool for investigating subphotospheric layers of the Sun, which can yield fairly detailed distributions of the subphotospheric temperatures and large-scale plasma flows based on the spectra of the oscillations observed at the photospheric layers and the observed peculiarities of propagation of magnetoacoustic waves in this medium (Zhao et al. (2001), Kosovichev (2006)). Unfortunately, the effects of temperature and the magnetic field on the wave propagation speed have not yet been separated Kosovichev (2006), so that the structure of the sunspot magnetic field in deep layers, beneath the photosphere, remains a subject of purely theoretical analysis. In his analysis of some theoretical models of the subphotospheric layers of sunspots based on recent helioseismological data, Kosovichev (2006) concluded that Parker's (“spaghetti”) cluster model Parker (1979) is most appropriate. In this model, the magnetic flux in the sunspot umbra is concentrated into separate, strongly compressed, vertical magnetic flux tubes that are interspaced with plasma that is almost free of magnetic field; the plasma can move between these tubes.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2010

References

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