Physics
Scientific paper
Jun 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975soph...42..395m&link_type=abstract
Solar Physics, vol. 42, June 1975, p. 395-420.
Physics
55
Atmospheric Models, Chromosphere, Photosphere, Solar Atmosphere, Solar Flares, Solar Spectra, Astronomical Models, Atmospheric Heating, Balmer Series, Emission Spectra, Inhomogeneity, K Lines, Line Spectra, Shock Heating, Temperature Distribution, Ultraviolet Spectra
Scientific paper
Homogeneous plane-parallel model atmospheres for solar flares have been constructed to approximately simulate observations of flares. The wings of the Ca II lines have been used to derive flare upper photosphere models, which indicate temperature increases of about 100 K over the temperature distribution in the pre-existing facula at a height of 300 km. In the case of flares covering sunspots the temperature rise seems to occur much higher in the atmosphere. We find that with increasing flare importance the heights of the upper chromosphere and transition region occur lower in the solar atmosphere, accounting for the factor of 60-600 increase in pressure in these regions relative to the quiet sun. The Ca II line profiles agree with observations only by assuming a macrovelocity distribution that increases with height. Also, the chromospheric parts of flares appear to be highly inhomogeneous. We show that shock and particle heated flare models do not agree with the observations and propose a thermal response model for flares. In particular, it appears that heating in the photosphere is an essential aspect of flares.
Linsky Jeffrey L.
Machado Marcos E.
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