Other
Scientific paper
May 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003spd....34.1101k&link_type=abstract
American Astronomical Society, SPD meeting #34, #11.01; Bulletin of the American Astronomical Society, Vol. 35, p.826
Other
1
Scientific paper
Two different types of models have been proposed to describe the quiet solar chromosphere: Simulating the dynamics and the temperature structure resulting from shock waves gives a negative average temperature gradient with respect to height (∇ z T <0) and violent temperature fluctuations (δ T ˜ 10,000 K); modeling based on the emergent spectrum gives a positive gradient (∇ z T>0,\ z>0.5 Mm) and modest fluctuations (δ T ˜ 300 K). Clearly, these two models are incompatible with one another. The model of the dynamics claims that the traditional temperature structure of the chromosphere (∇ z T>0) is an illusion created by time averaging of the emission. But the dissipation and radiative emission associated with the dynamics make only a minor contribution to chromospheric heating and the emergent radiation. In addition, in a typical supergranulation cell, the dynamics is confined to 10 to 20 regions (grains) with a combined filling factor ranging from 1% in the photosphere to 50% in the upper chromosphere. In the middle chromosphere (z=1 Mm), 90% to 95% of the medium falls outside the calcium grains and thus, according to the dynamical model, has no chromosphere, i.e., ∇ z T <0.
This paper discusses observational constraints on the temperature structure of the quiet solar chromosphere.
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