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Differential Rotation and Dynamics of the Solar Interior

Thompson1, Toomre, Anderson

  • 1M. J. Thompson and R. Howe are in the Astronomy Unit, Queen Mary and Westfield College, University of London, Mile End Road, London E1 4NS, UK. J. Toomre, M. DeRosa, and D. A. Haber are at the Joint Institute for Laboratory Astrophysics, University of Colorado, Boulder, CO 80309-0440, USA. E. R. Anderson, J. W. Harvey, F. Hill, and J. W. Leibacher are at the National Solar Observatory (NSO), National Optical Astronomy Observatories (NOAO), Post Office Box 26732, Tucson, AZ 85726-6732, USA. H. M. Antia and S. M. Chitre are at the Tata Institute of Fundamental Research, Bombay 400005, India. G. Berthomieu, T. Corbard, and J. Provost are at the Observatoire de la Cote d'Azur, 06304 Nice Cedex 4, France. D. Burtonclay and P. R. Wilson are in the School of Mathematics, University of Sydney, Sydney, NSW 2006, Australia. J. Christensen-Dalsgaard and F. P. Pijpers are at the Theoretical Astrophysics Center, Aarhus University, DK-8000 Aarhus C, Denmark. C. R. Genovese is in the Department of Statistics, Carnegie Mellon University, Pittsburgh, PA 15213, USA. D. O. Gough and T. Sekii are in the Institute of Astronomy, University of Cambridge, Cambridge CB3 0HA, UK. S. G. Korzennik is at the Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA. A. G. Kosovichev and J. Schou are at Hansen Experimental Physics Laboratory Annex, Stanford University, Stanford, CA 94305-4085, USA. E. J. Rhodes Jr. is in the Department of Physics and Astronomy, University of Southern California, Los Angeles, CA 90089, USA. P. B. Stark is in the Department of Statistics, University of California, Berkeley, CA 94720-3860, USA.

Science (New York, N.Y.)
|May 31, 1996
PubMed

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Summary
This summary is machine-generated.

Global oscillation frequencies reveal solar interior rotation. Observations show surface latitude-dependent rotation extends through the convection zone, with a distinct shear layer near the surface.

Area of Science:

  • Helioseismology
  • Solar Physics
  • Solar Interior Dynamics

Background:

  • Solar rotation varies with latitude and depth.
  • Understanding internal rotation is key to solar dynamo models.
  • Global oscillation frequencies are influenced by internal flows.

Purpose of the Study:

  • To investigate solar interior rotation using frequency splitting.
  • To map the variation of rotation with radius and latitude.
  • To analyze the structure of solar rotation.

Main Methods:

  • Analysis of global oscillation frequencies from the Global Oscillation Network Group (GONG) data.
  • Utilizing high-quality oscillation power spectra from nearly uninterrupted observations.
  • Deriving frequency splittings to infer internal rotation rates.

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Main Results:

  • Confirmed that latitude-dependent rotation at the solar surface extends through most of the convection zone.
  • Identified an adjustment layer at the base of the convection zone where rotation becomes latitudinally independent.
  • Detected a distinct shear layer in solar rotation just below the surface at low to mid-latitudes.

Conclusions:

  • Solar interior rotation is complex, with distinct layers and transitions.
  • The findings provide crucial data for solar dynamo and interior models.
  • Helioseismology offers a powerful tool for probing the Sun's interior structure and dynamics.