Other
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992acm..proc..329k&link_type=abstract
In Lunar and Planetary Inst., Asteroids, Comets, Meteors 1991 p 329-332 (SEE N93-19113 06-90)
Other
Austin Comet, Comet Nuclei, Comet Tails, Solar Activity Effects, Solar Wind, Space Plasmas, Japan, Observatories, Radial Flow
Scientific paper
The plasma tail of Comet Austin (1989c1) showed remarkable disturbances because of the solar maximum periods and its orbit. Figure 1 shows photographs of Comet Austin taken in Shibata, Japan, on 29 Apr. 1990 UT, during about 20 minutes with the exposure times of 90 to 120 s. There are two main features in the disturbance; one is many bowed structures, which seem to move tailwards; and the other is a large-scale wavy structure. The bowed structures can be interpreted as arcade structures brushing the surface of both sides of the cometary plasma surrounding the nucleus. We identified thirteen structures of the arcades from each of the five photographs and calculated the relation between the distance of each structure from the cometary nucleus, chi, and the velocity, upsilon. The result is shown. This indicates that the velocity of the structures increases with distance. This is consistent with the result obtained from the observation at the Kiso Observatory.
Konno Ichishiro
Kozuka Yukio
Numazawa Shigemi
Saito Takao
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