The EISCAT meteor-head method – a review and recent observations A. Pellinen-Wannberg Swedish Institute of Space Physics, Kiruna, Sweden
Abstract. Since the very first meteor observations at EISCAT in December 1990, the
experimental method has improved significantly. This is due to a better
understanding of the phenomenon and a recent major upgrade of the EISCAT
signal processing and data storage capabilities. Now the simultaneous
spatial-time resolution is under 100 m-ms class. To illuminate the meteor
target for as long as possible and simultaneously get as good altitude
resolution as possible, various coding techniques have been used, such as
Barker codes and random codes with extremely low side lobe effects. This
paper presents some background and the current view of the meteor head echo
process at EISCAT as well as the observations which support this view, such
as altitude distributions, dual-frequency target sizes and vector
velocities. It also presents some preliminary results from recent very high
resolution tristatic observations.
Citation: Pellinen-Wannberg, A.: The EISCAT meteor-head method – a review and recent observations, Atmos. Chem. Phys., 4, 649-655, doi:10.5194/acp-4-649-2004, 2004.