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Solar equatorial rotation rate inferred from inversion of frequency splitting of high-degree modes

Published online by Cambridge University Press:  03 August 2017

Frank Hill ,
Douglas Gough ,
Juri Toomre  and
Deborah A. Haber
Frank Hill
Affiliation:
National Solar Observatory, National Optical Astronomy Observatories, Tucson, AZ 85726-6732, USA
Douglas Gough
Affiliation:
Institute of Astronomy, and Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Cambridge CB3 0HA, England
Juri Toomre
Affiliation:
Joint Institute for Laboratory Astrophysics, and Department of Astrophysical, Planetary and Atmospheric Sciences, University of Colorado, Boulder, CO 80309-0440, USA
Deborah A. Haber
Affiliation:
Joint Institute for Laboratory Astrophysics, and Department of Astrophysical, Planetary and Atmospheric Sciences, University of Colorado, Boulder, CO 80309-0440, USA

Abstract

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The equatorial rotation rate has been inferred as a function of depth through the outer 16 Mm of the Sun from observations of high-degree five-minute oscillations. An optimal averaging inversion procedure due to Backus & Gilbert (1970) has been applied to frequency splittings measured from power spectra obtained using Doppler data spanning three and five consecutive days. The resulting rotation curves have proven to be much more stable than the curves obtained from data sets of single days. The results imply that the solar rotation rate increases with depth by 0.023 μHz reaching a maximum at about 2 Mm below the surface, then decreases by 0.037 μHz down to 16 Mm.

Type
Chapter 1: Observations of Solar Oscillations
Information
Symposium - International Astronomical Union , Volume 123: Advances In Hello- and Asteroseismology , 1988 , pp. 45 - 48
Copyright
Copyright © Reidel 1988 

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