Differential Rotation and Dynamics of the Solar Interior
M. J. ThompsonM. J. Thompson and R. Howe are in the Astronomy Unit, Queen Mary and Westfield College, University of London, Mile End Road, London E1 4NS, UKJuri ToomreJ. Toomre, M. DeRosa, and D. A. Haber are at JILA, University of Colorado, Boulder, CO 80309-0440, USAE. AndersonE. 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, USAH. M. AntiaH. M. Antia and S. M. Chitre are at the Tata Institute of Fundamental Research, Bombay 400005, IndiaG. BerthomieuG. Berthomieu, T. Corbard, and J. Provost are at the Observatoire de la Cote d'Azur, 06304 Nice Cedex 4, FranceD. BurtonclayD. Burtonclay and P. R. Wilson are in the School of Mathematics, University of Sydney, Sydney, NSW 2006, AustraliaS. M. ChitreH. M. Antia and S. M. Chitre are at the Tata Institute of Fundamental Research, Bombay 400005, IndiaJ. Christensen‐DalsgaardJ. Christensen-Dalsgaard and F. P. Pijpers are at the Theoretical Astrophysics Center, Aarhus University, DK-8000 Aarhus C, DenmarkT. CorbardG. Berthomieu, T. Corbard, and J. Provost are at the Observatoire de la Cote d'Azur, 06304 Nice Cedex 4, FranceMarc L. DeRosaJ. Toomre, M. DeRosa, and D. A. Haber are at JILA, University of Colorado, Boulder, CO 80309-0440, USAChristopher R. GenoveseC. R. Genovese is in the Department of Statistics, Carnegie Mellon University, Pittsburgh, PA 15213, USAD. O. GoughD. O. Gough and T. Sekii are in the Institute of Astronomy, University of Cambridge, Cambridge CB3 0HA, UKD. A. HaberJ. Toomre, M. DeRosa, and D. A. Haber are at JILA, University of Colorado, Boulder, CO 80309-0440, USAJ. W. HarveyE. 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, USAF. HillE. 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, USAR. HoweM. J. Thompson and R. Howe are in the Astronomy Unit, Queen Mary and Westfield College, University of London, Mile End Road, London E1 4NS, UKS. G. KorzennikS. G. Korzennik is at the Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAА. Г. КосовичевA. G. Kosovichev and J. Schou are at Hansen Experimental Physics Laboratory Annex, Stanford University, Stanford, CA 94305-4085, USAJ. W. LeibacherE. 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, USAF. P. PijpersJ. Christensen-Dalsgaard and F. P. Pijpers are at the Theoretical Astrophysics Center, Aarhus University, DK-8000 Aarhus C, DenmarkJ. ProvostG. Berthomieu, T. Corbard, and J. Provost are at the Observatoire de la Cote d'Azur, 06304 Nice Cedex 4, FranceE. J. RhodesE. J. Rhodes Jr. is in the Department of Physics and Astronomy, University of Southern California, Los Angeles, CA 90089, USAJ. SchouA. G. Kosovichev and J. Schou are at Hansen Experimental Physics Laboratory Annex, Stanford University, Stanford, CA 94305-4085, USAT. SekiiD. O. Gough and T. Sekii are in the Institute of Astronomy, University of Cambridge, Cambridge CB3 0HA, UKPhilip B. StarkP. B. Stark is in the Department of Statistics, University of California, Berkeley, CA 94720-3860, USAP. R. WilsonD. Burtonclay and P. R. Wilson are in the School of Mathematics, University of Sydney, Sydney, NSW 2006, Australia
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Аннотация
Splitting of the sun's global oscillation frequencies by large-scale flows can be used to investigate how rotation varies with radius and latitude within the solar interior. The nearly uninterrupted observations by the Global Oscillation Network Group (GONG) yield oscillation power spectra with high duty cycles and high signal-to-noise ratios. Frequency splittings derived from GONG observations confirm 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 shear layer just below the surface is discernible at low to mid-latitudes.
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