Solar oscillations and convective flows as probes of structure in the subphotosphere

Details Solar oscillations and convective flows as probes of structure in the subphotosphere Solar oscillations and convective flows as probes of structure in the subphotosphere

Apr 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987jila.rept.....t&link_type=abstract

Final Report, 2 Feb. 1983 - 31 Jul. 1986 Joint Inst. for Lab. Astrophysics, Boulder, CO.

Astronomy and Astrophysics

Astrophysics

Convective Flow, Convective Heat Transfer, Flux (Rate), Magnetic Fields, Photosphere, Solar Activity, Solar Oscillations, Sun, Thermodynamic Properties, Buoyancy, Detection, Diagrams, Displacement, Flow Stability, Frequency Stability, Horizontal Orientation, Inversions, Mapping, Observation, Splitting, Velocity

Scientific paper

Application of inverse theory to the observation of high-degree five-minute solar oscillations has led to the detection of horizontal flows below the solar surface that are a combination of solar rotation and giant convection cells. The distinctive displacements in the centroids of the ridges evident in the power diagrams of the oscillations from one observing day to the next arise from different patterns of giant cells being rotated into view. Such observation of frequency splittings for the high degree oscillation modes, combined with refinements in the inversion of the data using optimal averaging and spectral expansions, has shown that helioseismology should permit detailed mapping of velocity and thermal structures below the solar surface. Extensive theoretical studies of fully compressible magnetoconvection have shown that flows are indeed able to concentrate magnetic fields into concentrated flux sheets that are substantially evacuated of gas. The magnetic buoyancy instabilities have been extensively studied.

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