Spectrometry of minor planets. The possible reason for changes in reflection spectrum of 1 Ceres.

Details Spectrometry of minor planets. The possible reason for changes in reflection spectrum of 1 Ceres. Spectrometry of minor planets. The possible reason for changes in reflection spectrum of 1 Ceres.

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995sosyr..29...32g&link_type=abstract

Solar System Research, Vol. 29, No. 1, p. 32 - 40

Astronomy and Astrophysics

Astrophysics

Minor Planets: Spectrometry, Minor Planets: Reflectance Spectra, Minor Planets: Surface Structure

Scientific paper

Possible reasons for changes in the Ceres spectrum recorded on December 25 to 26, 1989, at Shemakha Astrophysical Observatory are discussed. The changes are so large that Ceres "shifts" itself into the optical class D3 (in the Barucchi classification) or T (in Tedesco classification). It has not been possible to find mistakes which could distort the results of the observations. It is shown that in December 1989, the spectrum of the north hemisphere of Ceres was obtained, and, contrary to the observations performed earlier, it was at the moment of absolute maximum solar irradiation intensity of the asteroid surface. Since the Ceres north pole is simultaneously the pole of heat, the assumption was made that the change in the asteroid's optical characteristics were caused by intense sublimation of hoar on its surface.

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