Magnetic Field in the Sun’s Interior from Oscillation Data
Solar oscillations provide a probe of the internal magnetic field of the Sun if the field has sufficient intensity. Using the oscillation data of Libbrecht, we find evidence for a 2 ± 1 megagauss quadrupole toroidal field centered at 0.7 of the solar radius which is barely beneath the base of the convection zone. This field, by its location and symmetry, may be associated with the dynamo that drives the Sun’s 22-year activity cycle.
KeywordsConvection Zone Differential Rotation Toroidal Field Oscillation Data Internal Magnetic Field
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- Brown, T.M., Christensen-Dalsgaard, J., Dziembowski, W.A., Goode, P.R., Gough, D.O., and Morrow, C.A.1989, Ap.J., in press.Google Scholar
- Christensen-Dalsgaard, J. and Shou, J. 1988, Seismology of the Sun and Sun-like Stars, 149, E.J. Rolfe (Ed.), ESA, Noordwijk, The Netherlands.Google Scholar
- Parker, E.N. 1987, The Internal Solar Angular Velocity, 289, B. Durney and S. Sofia (Eds.), Reidel, Dordrecht, The Netherlands.Google Scholar
- Smirnov, A.Y. 1989, this volume.Google Scholar
- Spruit, H.C. 1987, The Internal Solar Angular Velocity, 185, B. Durney and S. Sofia (Eds.), Reidel, Dordrecht, The Netherlands.Google Scholar