Intensity, velocity and temperature fluctuations in the upper solar photosphere

Details Intensity, velocity and temperature fluctuations in the upper solar photosphere Intensity, velocity and temperature fluctuations in the upper solar photosphere

May 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....57..159a&link_type=abstract

Astronomy and Astrophysics, vol. 57, no. 1-2, May 1977, p. 159-167.

Astronomy and Astrophysics

Astrophysics

7

Photosphere, Radiant Flux Density, Solar Atmosphere, Solar Spectra, Solar Temperature, Velocity Distribution, High Resolution, Modulation Transfer Function, Power Spectra, Spectral Resolution, Temperature Distribution

Scientific paper

High-spatial-resolution photographic spectra of the Mg I 4571-A line at 10 solar disk positions from center to limb are reduced to yield intensity and velocity (line-shift) fluctuations along the spectrograph slit for a height of about 300 km above the continuum level. The data obtained are used to compute rms intensity and velocity fluctuations corrected for instrument smearing. Comparison of the results with those of Cannon and Wilson (1971) reveals a flatter distribution of the rms intensity fluctuation as a function of heliocentric angle and a 60% larger fluctuation at the disk center. It is inferred that the correlation between velocity and intensity fluctuations exhibits a large-scale random structure. The intensity-fluctuation data are analyzed by calculating the emergent intensity from a three-dimensional atmosphere having a sinusoidal checkerboard pattern of temperature with a height-dependent amplitude, taking into account fluctuations in electron pressure. The range of solutions for temperature fluctuations is found to indicate that there are causes other than oscillations for the temperature fluctuations in the upper photosphere.

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