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Steady and Fluctuating Parts of Sun’s Internal Magnetic Field

Published online by Cambridge University Press:  12 April 2016

M.H. Gokhale  and
K.M. Hiremath
M.H. Gokhale
Affiliation:
Indian Institute of Astrophysics, Bangalore 560 034, India
K.M. Hiremath
Affiliation:
Indian Institute of Astrophysics, Bangalore 560 034, India

Abstract

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We have modeled the ‘steady’ part of sun’s internal poloidal magnetic field in the form of a central dipole and a central hexapole with strengths (0.6±0.1) and embedded in an asymptotically uniform field Bo. A small deviation from isorotation seems to indicate:(i) a slow build-up of toroidal field near the base of the convection zone and (ii) presence of torsional MHD perturbations in the outer radiative core, with latitudinal structure and time scales which may be similar to those of solar activity.

Type
I. Setting the stage: Sun, Stars Galaxies and the Universe
Information
International Astronomical Union Colloquium , Volume 137: Inside the Stars , 1993 , pp. 66 - 68
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

Christensen-Dalsgaard, J., & Schou, J. 1988, in Seismology of the Sun and Sun-like Stars, ed. Domingo, V. and Rolfe, E.J. ESA: SP-286, p. 149.Google Scholar
Ferraro, V.C.A. 1937, M. N.R.A.S., 97, 457.Google Scholar
Gokhale, M.H., Javaraiah, J., Kutty, K.N.. & Varghese, B.A. 1992, Solar Phys, 138, 35.Google Scholar
Stenflo, J.O. 1988, Astrophys. & Space Sci., 144, 321.CrossRefGoogle Scholar