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LOI/SOHO Constraints on Oblique Rotation of the Solar Core

Published online by Cambridge University Press:  08 February 2017

L. Gizon ,
T. Appourchaux  and
D.O. Gough
L. Gizon
Affiliation:
W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford CA 94305, U.S.A.
T. Appourchaux
Affiliation:
ESA / ESTEC, P.O. Box 299, 2200 AG Noordwijk, The Netherlands
D.O. Gough
Affiliation:
Institute of Astronomy, and Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Madingley Road, Cambridge CB3 0HA, U.K. HEPL, Stanford University, Stanford CA 94305, U.S.A.

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The axis of rotation of the Sun's surface is inclined from the normal to the ecliptic by 7°.25. Is that true also of the rotation of the rest of the Sun? Knowledge of the direction of the angular momentum is pertinent to studies of the formation of the solar system. Moreover, Bai and Sturrock (1993) have recently interpreted temporal variations in the spatial distribution of solar flares as the outcome of the interaction of the Sun's envelope with an obliquely rotating core. We report here an attempt to determine the principal seismic axes of oscillation of the dipole and quadrupole p modes from LOI data obtained as a component of the VIRGO investigation on the spacecraft SOHO. We find that formally their most likely orientation is somewhat closer to being normal to the ecliptic than is the axis of the surface rotation. However, the uncertainty in the determination well encompasses the possibility of them being parallel to the surface rotation axis, yet it does not reject (at a level marginally greater than one standard deviation) the possibility that the Sun's angular momentum is parallel to that of the rest of the solar system.

Type
I. Global Structure and Evolution of the Solar and Stellar Interior
Information
Symposium - International Astronomical Union , Volume 185: New Eyes to See Inside the Sun and Stars , 1998 , pp. 37 - 40
Copyright
Copyright © Kluwer 1998 

References

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