What we know about the sun's internal rotation from solar oscillations

Philip R. Goode, W. A. Dziembowski, S. G. Korzennik, E. J. Rhodes

Research output: Contribution to journalArticlepeer-review

81 Scopus citations

Abstract

The six available 5 minute period oscillation data sets have been inverted using the same method to determine the robust properties of the internal rotation rate of the Sun. The comprehensive result is that the rotation rate in the equatorial plane declines going inward between the surface and 0.6 of the radius and, with less certainty in the same region, the polar rate increases going inward. In other words, the surface-like differential rotation decreases with depth. The bulk of these changes occurs near the base of the convection zone. Going inward in the equatiorial plane from 0.6 to 0.4 of the radius, the rotation appears to be flat. Beneath 0.4 of the radius, we can make no appealing case for a rapidly rotating core. There is evidence that the internal rotation has changed systematically through this solar activity cycle. We also make a suggestion as to how oscillation data should be presented.

Original languageEnglish (US)
Pages (from-to)649-657
Number of pages9
JournalAstrophysical Journal
Volume367
Issue number2
DOIs
StatePublished - Feb 1 1991

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Keywords

  • Sun: oscillations
  • Sun: rotation

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