The energy balance and pressure in the solar transition zone for network and active region features

Details The energy balance and pressure in the solar transition zone for network and active region features The energy balance and pressure in the solar transition zone for network and active region features

Oct 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...233..741n&link_type=abstract

Astrophysical Journal, Part 1, vol. 233, Oct. 15, 1979, p. 741-743, 745-755.

Astronomy and Astrophysics

Astronomy

25

Energy Dissipation, Plasma Spectra, Solar Spectra, Ultraviolet Astronomy, Electron Density (Concentration), Emission Spectra, Far Ultraviolet Radiation, High Resolution, Radiation Pressure

Scientific paper

The electron pressure and energy balance in the solar transition zone are determined for about 125 network and active region features on the basis of high spectral and spatial resolution extreme ultraviolet spectra. Si III line intensity ratios obtained from the Naval Research Laboratory high-resolution telescope and spectrograph during a rocket flight are used as diagnostics of electron density and pressure for solar features near 3.5 x 10 to the 4th K. Observed ratios are compared with the calculated dependence of the 1301 A/1312 A and 1301 A/1296 A line intensity ratios on electron density, temperature and pressure. Electron densities ranging from 2 x 10 to the 10th/cu cm to 10 to the 12th/cu cm and active region pressures from 3 x 10 to the 15th to 10 to the 16th/cu cm K are obtained. Energy balance calculations reveal the balance of the divergence of the conductive flux and turbulent energy dissipation by radiative energy losses in a plane-parallel homogeneous transition zone (fill factor of 1), and an energy source requirement for a cylindrical zone geometry (fill factor less than 0.04).

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