Physics
Scientific paper
May 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976rspta.281..295f&link_type=abstract
(Royal Society, Discussion on the Physics of the Solar Atmosphere, London, England, Jan. 14, 15, 1975.) Royal Society (London),
Physics
2
Convective Flow, Photosphere, Solar Atmosphere, Solar Granulation, Solar Magnetic Field, Atmospheric Models, Boundary Layers, Doppler Effect, Magnetic Field Configurations, Oscillating Flow, Solar Interior
Scientific paper
The photosphere is essentially a relatively thin boundary layer between two fundamentally different plasma regimes. The solar interior is characterized by high density, high opacity, high beta, and convective instability; the outer solar atmosphere has the opposite properties. Convection in the interior provides the ultimate driving force for all of the dynamic and magnetic structure of the solar atmosphere, yet when we view the photosphere, we can observe only the upper boundary of the convection zone. Instead, we observe primarily its various after-effects: overshoot, wave propagation, and confinement of the magnetic field. These observable phenomena are described with a view toward diagnosing the essential physics above and below the photosphere. The convective modes, granulation and supergranulation, are reviewed briefly; the oscillatory modes are discussed in somewhat more detail. Finally, the magnetic structure of the photosphere is described.
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