Physics
Scientific paper
Aug 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990nascp3086...50s&link_type=abstract
In its Climate Impact of Solar Variability p 50-56(SEE N91-12456 03-92)
Physics
Advection, Chromosphere, Energy Transfer, Faculae, Magnetic Effects, Photosphere, Solar Magnetic Field, Solar Physics, Stellar Envelopes, Sunspots, Gas Cooling, Irradiance, Surface Temperature
Scientific paper
Sunspots and faculae were modeled using a modified stellar envelope code. Downflow velocities of 50 m/sec can achieve a 1,000 K drop in the surface temperature of the photosphere and reduce the surface irradiance to half its value. Concurrently, a 600 km Wilson depression forms that is associated with the enhanced density of the cooler gases. Similar upflow velocities provide for slightly enhanced temperatures and 150 km uplifted surfaces for faculae. The calculations show that, to first approximation, sunspot and facular structures (in density, temperature and pressure) can be obtained by simply vertically shifting the undisturbed photospheric materials to form wells and hillock geometries, respectively. However, the chromospheric manifestations of these features can be quite different owing to the influence of the magnetic field and flow.
Mayr Hans G.
Schatten Kenneth H.
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