Solar radio bursts have long been observed using dynamic spectra (records of intensity vs. time and frequency), and it is only recently that joint spectroscopic and (fixed frequency) imaging experiments have been conducted. An extremely exciting possibility is imaging-spectroscopy of solar radio bursts over an octave, or more, of bandwidth using a broad-band UHF system at the prime focus. Using such techniques, it will be possible to constrain the point of origin and the subsequent propagation of both electron beams (type III bursts) and MHD shocks (type II bursts) in the solar corona. As such, it offers a powerful tool for probing coronal dynamics, beam propagation, and shock acceleration.
Unlike other proposals for feeds at the prime focus, a broad-band UHF system does not need to be a high performance system. As such, it may require the fewest modifications to the quadrupod and FRM. On the other hand, it imposes demanding specifications on other aspects of the project, requiring:
1 MHz and a time resolution as
small as 10 ms, which may require the use of a ``burst mode''.
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