Determining the Length of the Magnetotail From GEOTAIL, POLAR, and WIND Observations of Tapered Tail Low Frequency Bursts

Details Determining the Length of the Magnetotail From GEOTAIL, POLAR, and WIND Observations of Tapered Tail Low Frequency Bursts Determining the Length of the Magnetotail From GEOTAIL, POLAR, and WIND Observations of Tapered Tail Low Frequency Bursts

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsm22a..06a&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SM22A-06

Other

2704 Auroral Phenomena (2407), 2740 Magnetospheric Configuration And Dynamics, 2744 Magnetotail, 2772 Plasma Waves And Instabilities, 2784 Solar Wind/Magnetosphere Interactions

Scientific paper

One of the more interesting phenomena detected by the GEOTAIL and POLAR Plasma Wave Instruments (PWIs) and the WIND Radio Science Experiment (WAVES) are the auroral kilometric radiation (AKR) low frequency (LF) bursts. These electromagnetic emissions are the low frequency extension of AKR and are most frequently observed during the most geomagnetically disturbed times. In the solar wind the LF bursts are observed to extend in frequency down to the local electron plasma frequency (Fpe) with increasing time delay the lower the frequency. In the magnetosphere the LF bursts often display a tapered tail that has maximum time delay at a distinct frequency which we shall call Ftt. The LF bursts then show increasing time delay as Ftt is approached from frequencies above it and from frequencies below it. When one of the spacecraft is in the solar wind and another is in the magnetosphere during a LF burst observation, we see that Ftt almost always appears equal to the solar wind Fpe in the near past (some few hours). It is speculated that AKR generated in the Earth's magnetospheric auroral region at frequencies below the magnetosheath plasma frequency (2Fpe near the nose) is reflected and refracted down the tail since it cannot penetrate the magnetosheath directly. As it travels down the tail, AKR of a given frequency finally reaches a point where the tail magnetosheath plasma frequency is equal to it and it can propagate into the solar wind. Ftt is believed to be the AKR frequency which is equal to the local solar wind plasma frequency at the point down the tail where the magnetosheath frequency and local solar wind plasma frequency are equal and where waves of this frequency are broadly scattered. Upstream in situ measurements of the solar wind Fpe and the flow speed allow us to determine how far down the tail the local solar wind Fpe and Ftt are equal. The results so far have ranged from 200 Re to 2000 Re.

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