Comparative analysis of ultraviolet observations of Halley's comet on ASTRON astrophysical station before and after perihelion

Details Comparative analysis of ultraviolet observations of Halley's comet on ASTRON astrophysical station before and after perihelion Comparative analysis of ultraviolet observations of Halley's comet on ASTRON astrophysical station before and after perihelion

Nov 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987rpsct...3...76b&link_type=abstract

In its JPRS Report: Science and Technology. USSR: Space p 76 (SEE N88-16063 08-42) Transl. into ENGLISH from Pisma v Astronomich

Astronomy and Astrophysics

Astronomy

Astronomical Models, Brightness Distribution, Halley'S Comet, Perihelions, Spectrum Analysis, Astronomical Satellites, Spaceborne Astronomy, Ultraviolet Astronomy

Scientific paper

Spectrophotometric observations of Halley's comet were made in Dec. 1985 using the UV telescope on the ASTRON station. Important conclusions could be drawn using more than 100 spectra of the comet at different distances from the nucleus and three photometric sections of the peripheral parts of the coma in the band OH (O-O) 3085 A. There is a thermal inertia of the nucleus; its temperature and rate of sublimation of molecules from a unit surface prior to perihelion is lower than at the same heliocentric distances after perihelion. Other factors may also be responsible: a change in nucleus reflectivity after passage through perihelion and differences in its orientation relative to the Sun before and after perihelion. Since during one transit the nucleus radius decreases by only about 1.5 m, some explanation must be found for the great photometric effect observed from transit to transit. The only possible explanation for the brightness reduction is a decrease in nucleus albedo as a result of degradation of its surface, with accumulation of large dust particles and the formation of stable mineral crust.

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