{"status":"ok","message-type":"work","message-version":"1.0.0","message":{"indexed":{"date-parts":[[2025,8,6]],"date-time":"2025-08-06T12:27:07Z","timestamp":1754483227672},"reference-count":46,"publisher":"American Geophysical Union (AGU)","issue":"A1","license":[{"start":{"date-parts":[[2012,9,20]],"date-time":"2012-09-20T00:00:00Z","timestamp":1348099200000},"content-version":"vor","delay-in-days":8663,"URL":"http:\/\/onlinelibrary.wiley.com\/termsAndConditions#vor"}],"content-domain":{"domain":[],"crossmark-restriction":false},"short-container-title":["J. Geophys. Res."],"published-print":{"date-parts":[[1989,1]]},"abstract":"<jats:p>The properties of 50\u2010 to 100\u2010s low\u2010frequency plasma waves and the parent 65\u2010 to 95\u2010keV H<jats:sub>2<\/jats:sub>O group ion pitch angle distributions are presented for spatial regions distant (3.5\u20107.0 \u00d7 10<jats:sup>5<\/jats:sup> km) from comet Giacobini\u2010Zinner where the cometary ion densities are low and the solar wind interaction is weak. The presence of interplanetary discontinuities in this interval causes the interplanetary magnetic field angle \u03b1 <jats:inline-graphic xmlns:xlink=\"http:\/\/www.w3.org\/1999\/xlink\" xlink:href=\"graphic\/jgra9150-math-0001.gif\" xlink:title=\"equation image\" \/>\nto vary over a range from \u223c35\u00b0 to 90\u00b0, allowing the possible generation of several new wave modes which are theoretically expected, but as yet undetected. It is determined that when <jats:italic>x<\/jats:italic> = 45\u00b0 \u00b1 20\u00b0 (Parker spiral orientations), the waves are typically elliptically polarized and propagate at 20\u00b0\u201050\u00b0 relative to <jats:bold>B<\/jats:bold><jats:sub>0<\/jats:sub>. The wave properties are, however, not limited to the above range. They can exhibit even more extreme polarizations and propagation directions. The waves have periods near the H<jats:sub>2<\/jats:sub>O group ion cyclotron period and are left\u2010hand polarized in the spacecraft frame. In the relatively rare instances when wave steepening is detected, the steepened edge is near the trailing portion of the wave. The wave period, sense of polarization, and steepening are consistent with the properties of waves detected closer to the comet and identify them as being generated by the right\u2010hand resonant instability. The high degree of ellipticity is in sharp contrast to waves detected closer to the comet, however. The energetic ions are not isotropic in pitch angle (in the plasma frame), in general agreement with recent numerical modeling. When \u03b1 increases to 70\u00b0\u201090\u00b0, the right\u2010hand resonant mode is observed to cut off, as theoretical studies indicate. However, the left\u2010hand cyclotron resonant mode is not detected. Although the detected energetic 65\u2010 to 95\u2010keV ion fluxes are enhanced during these intervals (because of the instantaneous pickup by the solar wind), particle pitch angle scattering away from the initial ring distribution is very weak, consistent with the observed absence of resonant cyclotron waves.<\/jats:p>","DOI":"10.1029\/ja094ia01p00018","type":"journal-article","created":{"date-parts":[[2008,2,6]],"date-time":"2008-02-06T18:52:14Z","timestamp":1202323934000},"page":"18-28","source":"Crossref","is-referenced-by-count":30,"title":["Low\u2010frequency plasma waves and ion pitch angle scattering at large distances (&gt;3.5 \u00d7 10<sup>5<\/sup> km) from Giacobini\u2010Zinner: Interplanetary magnetic field \u03b1 dependences"],"prefix":"10.1029","volume":"94","author":[{"given":"Bruce T.","family":"Tsurutani","sequence":"first","affiliation":[]},{"given":"D. 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