A serious long-term attempt to study the corona using radar was made between 1961 and 1969, but it was unsuccessful because the characteristics of the radar echo could not be explained. In retrospect it was not possible to adequately model the radar echoes because we did not know enough about the corona at that time. Further observations became impossible as radar astronomy evolved and the technique has been almost forgotten. In this chapter we propose to revive the solar radar technique. We discuss the theory, review the early observations, provide a tenable explanation of them, propose new experiments, and outline the likely development of the technique.
KeywordsSolar Wind Solar Activity Coronal Mass Ejection Coronal Hole Radar Cross Section
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