Brightness of the solar F-corona
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We discuss our present knowledge about the brightness of the solar <I>F</I>-corona in the wavelength range from the visible to the middle infrared. From the general trend of the observational data, the <I>F</I>-corona is regarded as the continuous extension of the zodiacal light at smaller elongation of the line of sight. A contribution of thermal emission from dust is indicated by the increasing <I>F</I>-coronal brightness in comparison to the solar spectrum towards longer wavelength. As compared with the <I>F</I>-coronal brightness, the polarization and color in the visible regime are not well determined due to the high sensitivity of these quantities to the observational accuracy. Aside from observational problems, our present interpretation of the <I>F</I>-coronal brightness is also limited due to ambiguities in the inversion of the line of sight integral. Nevertheless, the measurements and model calculations of the brightness can be used to deduce some physical properties of dust grains. We show that the hump of the near-infrared brightness at 4 solar radii, which was sometimes observed in the corona, is related rather to the physical properties of dust grains along the line of sight than to the existence of a dust ring as previously discussed. We also show that the appearance or disappearance of the near-infrared peak in the coronal brightness cannot be described in any periodic cycle for each wavelength range.
- Journal of geomagnetism and geoelectricity
Journal of geomagnetism and geoelectricity 50(6), 493-499, 1998-07
The Seismological Society of Japan, Society of Geomagnetism and Earth, Planetary and Space Sciences, The Volcanological Society of Japan , The Geodetic Society of Japan , The Japanese Society for Planetary Sciences