Abstract
The 5 minute oscillations in a sunspot umbra are the response of the sunspot to forcing by the 5 minute p-modes in the surrounding convection zone (Thomas 1981). This interaction of solar p-modes with a sunspot can be used to probe the structure of a sunspot beneath the visible surface of the Sun (Thomas, Cram, and Nye 1982). Here we report briefly the results of both an observational study and a simple theoretical analysis of this interaction. A full account of these results will be published elsewhere (Abdelatif, Lites, and Thomas 1986; Abdelatif and Thomas 1987).
The National Center for Atmospheric Research is sponsored by the National Science Foundation.
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References
Abdelatif, T. E., Lites, B. W., and Thomas, J. H. 1986, Astrophys. J., in press.
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Thomas, J. H., Cram, L. E., and Nye, A. H. 1982, Nature, 297, 485.
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© 1988 International Astronomical Union
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Thomas, J.H., Lites, B.W., Abdelatif, T.E. (1988). Sunspot Seismology. In: Christensen-Dalsgaard, J., Frandsen, S. (eds) Advances in Helio- and Asteroseismology. International Astronomical Union / Union Astronomique Internationale, vol 123. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-4009-3_40
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DOI: https://doi.org/10.1007/978-94-009-4009-3_40
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