Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...269..395s&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 269, no. 1-2, p. 395-402.
Astronomy and Astrophysics
Astrophysics
9
Chromosphere, Cool Stars, Photosphere, Stellar Activity, Stellar Magnetic Fields, Solar Activity, Solar Atmosphere, Solar Magnetic Field
Scientific paper
The two-step explanation of the observed nonlinearity of relationships between photospheric magnetic and chromospheric radiative flux densities of cool stars starts with the sensitivity of the emission of individual flux tubes on the mean magnetic flux density. I argue that the relationship between flux densities for individual flux tubes is virtually the same as that found empirically from solar data with a spatial resolution of a few arcsec. For this I use a simple model in which the chromospheric radiative output of a flux tube is assumed to be a function only of the area a into which the flux tube can expand above the canopy, determined by the positions of the surrounding flux tubes. The scatter about the mean relationship that is expected from the random positioning of flux tubes within a resolution element is small compared to the observed scatter. The latter must therefore be caused largely by time variability, by effects of the detailed geometry, and possibly by a range in flux-tube diameters. The second step in explaining the nonlinearity of stellar flux-flux relationships involves effects of nonrandom positioning on larger scales on the averaging over the entire solar or stellar disk.
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