The granulation sensitivity of helioseismology lines

Details The granulation sensitivity of helioseismology lines The granulation sensitivity of helioseismology lines

Dec 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.286..251r&link_type=abstract

In ESA, Seismology of the Sun and Sun-Like Stars p 251-255 (SEE N89-25819 19-92)

Physics

1

Helioseismology, Line Spectra, Photosphere, Solar Granulation, Solar Spectra, Solar Oscillations, Solar Temperature, Surface Layers, Ultraviolet Radiation

Scientific paper

The sensitivity of the Ni I 676.78 nm Global Oscillation Network Group line and the K I 769.9 nm resonance line to the temperature fluctuations present in the solar granulation are discussed. The temperature contrasts due to granulation are probably small in the upper photosphere where the cores of these two helioseismology lines are formed. However, the cores are sensitive also to the granulation temperature contrasts in the deep photosphere, through nonlocal NLTE effects in their formation. The largest effects are due to the ultraviolet radiation field, which is strongly modulated by the granulation in the deep layers where it escapes and carries these contrasts upwards to the line formation height. The resulting NLTE mechanisms and their influence on the two lines are considered.

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