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Published via the yankee Geophysical Union as a part of the Special guides Series.

nobody might dispute that 1985 and 1986 have been particular occasions for cometary learn. In September 1985 ISEE-3 transited the magnetotail of comet Giacobini-Zinner and supplied the 1st close-up clinical view of a cometary surroundings. part a yr later a world fleet of spacecraft outfitted with cutting-edge instrumentation gave us a "once-in-a-lifetime" examine comet Halley.


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Comet Encounters: IA Copyright American Geophysical Union 123 Special Publications Comet Encounters Vol. 27 GEOPHYSICAL RESEARCH LETTERS, VOL. 4, PAGES 411-414, APRIL 1986 THE INTERACTION OF HEAVY IONS FROM COMET P/GIACOBINI-ZINNER WITH THE SOLAR WIND T. R. Sanderson and K-P. Wenzel Space Science Department of ESA, Estec, Noordwijk P. Daly Max-P1anck-Institut fUr Aeronomie, Kat1enburg-Lindau S. W. H. Cowley and R. J. Hynds Imperial College of Science and Technology, London E. J. Smith Jet Propulsion Laboratory, Calif.

10- 7 sec- I is still consistent with our observations. 10 22 sec-~. g. Divine, 1984). 5 and 2 above the curves. , 1986), caused by the compression of solar wind stream lines in these regions. e. by factors of 2 to 5) in the production rate of water-group molecules over periods of ~1 hour. Distribution Functions. The shapes of the distribution functions of picked-up cometary ions are determined by the solar wind-cometary ion interaction processes. The fact that our analysis resul ts in smooth spec tral shapes of the timeaveraged distribution functions, f, indicates that the assumption of near-isotropy in the ion rest-frame (which moves at the local solar wind speed) is basically correct.

These variations and the asymmetry will be addressed in more detail later in this section. We believe that the ions we have measured belong predominantly to the water group. Our instrument is unable to differentiate ion mass, but our observations, as will be seen later, are clearly consistent with a pick-up origin for the ions, if the ions belong to this groups. , 1986] have given conclusive evidence that the most abundant ions are tnose from the water group. Such ions, originating as neutrals from the comet's atmosphere, can travel great distances from the comet before being ionised and then picked-up by the moving interplanetary magnetic field, appearing with spectra and angular distributions consistent with our measurements.

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