Статья

Helioseismic Studies of Differential Rotation in the Solar Envelope by the Solar Oscillations Investigation Using the Michelson Doppler Imager

J. SchouW. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305-4085H. M. AntiaTata Institute of Fundamental Research, Mumbai 400005, IndiaSarbani BasuPresent address: School of Natural Sciences, Institute for Advanced Study, Princeton, NJ 08540R. S. BogartW. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305-4085R. I. BushW. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305-4085S. M. ChitreTata Institute of Fundamental Research, Mumbai 400005, IndiaJ. Christensen‐DalsgaardInstitut for Fysik og Astronomi, Aarhus Universitet, DK-8000 Aarhus C, DenmarkM. P. Di MauroCNR-Gruppo Nazionale di Astronomia, UdR di Catania Istituto di Astronomia, Universita' di Catania, Viale A. Doria 6, I-95125 Catania, ItalyW. A. DziembowskiCopernicus Astronomical Center, ul. Bartycka 18, 03-610 Warszawa, PolandA. Eff‐DarwichHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138D. O. GoughDepartment of Applied Mathematics and Theoretical Physics, University of Cambridge, Silver Street, Cambridge, CB3 9EW, UKD. A. HaberJILA and Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309-0440J. T. HoeksemaW. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305-4085R. HoweAstronomy Unit, Queen Mary and Westfield College, University of London, E1 4NS, UKS. G. KorzennikHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138А. Г. КосовичевW. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305-4085R. M. LarsenDatalogisk Institut, Aarhus Universitet, DK-8000 Aarhus C, DenmarkF. P. PijpersP. H. ScherrerW. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305-4085T. SekiiInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UKT. D. TarbellLockheed Martin Advanced Technology Center, Org. H1-11, Building 252, 3251 Hanover Street, Palo Alto, CA 94304A. M. TitleLockheed Martin Advanced Technology Center, Org. H1-11, Building 252, 3251 Hanover Street, Palo Alto, CA 94304M. J. ThompsonAstronomy Unit, Queen Mary and Westfield College, University of London, E1 4NS, UKJuri ToomreJILA and Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309-0440

1998en

ABI

Аннотация

The splitting of the frequencies of the global resonant acoustic modes of the Sun by large-scale Ñows and rotation permits study of the variation of angular velocity) with both radius and latitude within the turbulent convection zone and the deeper radiative interior. The nearly uninterrupted Doppler imaging observations, provided by the Solar Oscillations Investigation (SOI) using the Michelson Doppler Imager (MDI) on the Solar and Heliospheric Observatory (SOHO) spacecraft positioned at the Lagrangian point in continuous sunlight, yield oscillation power spectra with very high signal-to-L 1noise ratios that allow frequency splittings to be determined with exceptional accuracy. This paper reports on joint helioseismic analyses of solar rotation in the convection zone and in the outer part of the radiative core. Inversions have been obtained for a medium-l mode set (involving modes of angular degree l extending to about 250) obtained from the Ðrst 144 day interval of SOI-MDI observations in 1996. Drawing inferences about the solar internal rotation from the splitting data is a subtle process. By applying more than one inversion technique to the data, we get some indication of what are the more robust and less robust features of our inversion solutions. Here we have used seven di†erent inversion methods. To test the reliability and sensitivity of these methods, we have performed a set of controlled experiments utilizing artiÐcial data. This gives us some conÐdence in the inferences we can draw from

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Идентификаторы

DOI: 10.1086/306146

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Цитирований: 3Использованных источников: 0

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