Non-specular meteor trail diagnostics

Details Non-specular meteor trail diagnostics Non-specular meteor trail diagnostics

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsa41a..04d&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SA41A-04

Physics

2439 Ionospheric Irregularities, 6245 Meteors

Scientific paper

Plasma simulations demonstrate that meteor trails are unstable to growth of gradient-drift Farley-Buneman (GDFB) waves that become turbulent and generate large B-field aligned irregularities (FAI). These simulations and our analysis indicate that the non-specular echos, that can extend between 5-10 km in altitude range, are reflections from plasma instability generated FAI. We present models showing that the specific altitude range of trail instability depends on meteor and atmospheric properties. This variability will allow researchers to infer neutral temperature, neutral wind velocity, and meteoric velocity and composition in completely new ways. We demonstrate some of these non-specular trail diagnostic techniques using radar observations from the ALTAIR and Piura radar facilities. Finally, we present examples of a low altitude variety of non-specular echos that may be related to PMSE.

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