Scattering characteristics of high-resolution meteor head echoes detected at multiple frequencies

Details Scattering characteristics of high-resolution meteor head echoes detected at multiple frequencies Scattering characteristics of high-resolution meteor head echoes detected at multiple frequencies

Oct 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002jgra..107.1295c&link_type=abstract

Journal of Geophysical Research (Space Physics), Volume 107, Issue A10, pp. SIA 9-1, CiteID 1295, DOI 10.1029/2002JA009253

Physics

27

Radio Science: Radio Wave Propagation, Planetology: Solar System Objects: Asteroids And Meteoroids, Planetology: Solar System Objects: Meteors, Radio Science: Ionospheric Physics (2409)

Scientific paper

Meteor data collected at the Kwajalein Missile Range (KMR) during the peak of the 1998 Leonid storm comprise the only simultaneous observations of meteor head echoes and trails using seven frequencies (very high frequency (VHF), ultrahigh frequency (UHF), L-, S-, C-, Ka-, and W-band spanning 160 MHz to 95 GHz). The primary sensor was the ARPA Long-Range Tracking and Instrumentation Radar (ALTAIR) radar operating at 160 MHz with 30 m range resolution and 422 MHz with 7.5 m range resolution, including both interferometric and polarization capabilities. This paper presents an analysis of this high-resolution data set with the following results: First, these observations support the theory that head echo scattering arises from an ionized region with a density sufficiently high that its plasma frequency exceeds the radar frequency (overdense reflection). Second, radar cross section (RCS) decreases rapidly with decreasing wavelength because higher frequencies must penetrate further into the increasing density of the plasma surrounding the meteoroid to reach its reflection point. Third, head echo angle measurements indicate that most of the observed meteors are sporadics not originating from the Leonid radiant. Fourth, polarization ratios showed that head echo reflections result from plasmas with a circular cross section. Fifth, the highest RCS values are detected near 105 km altitude, where the meteoroid gives up the most kinetic energy during its decent. This paper presents the first analyses of a three-frequency head echo as well as the polarization ratios and RCS characteristics from numerous two-frequency head echoes, which will allow us to develop a better understanding of meteor physics.

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