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Differential Rotation and Dynamics of the Solar Interior

By M. Thompson, J. Toomre, E. Anderson, H. Antia, G. Berthomieu, D. Burtonclay, S. Chitre, J. Christensen-Dalsgaard, T. Corbard, M. DeRosa, C. Genovese, D. Gough, D. Haber, J. Harvey, F. Hill, R. Howe, S. Korzennik, A. Kosovichev, J. Leibacher, F. Pijpers, J. Provost, E. Rhodes, J. Schou, T. Sekii, P. Stark and P. Wilson


International audienceSplitting of the Sun's global oscillation frequencies by large-scale ows can be used to investigate how rotation varies with radius and latitude within the solar interior. The nearly uninterrupted observations by GONG yield oscillation power spectra with high duty cycle and signal-to-noise ratio. Frequency split-tings derived from GONG observations con rm that the variation of rotation rate with latitude seen at the surface carries through much of the convection zone, at the base of which is an adjustment layer leading to latitudinally independent rotation at greater depths. A distinctive shearing layer just below the surface is discernible at low to mid latitudes

Topics: [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR]
Publisher: 'American Association for the Advancement of Science (AAAS)'
Year: 1996
DOI identifier: 10.1126/science.272.5266.1300
OAI identifier: oai:HAL:hal-02895778v1
Provided by: HAL-INSU
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