Radio synthesis imaging during the GRO solar campaign

Details Radio synthesis imaging during the GRO solar campaign Radio synthesis imaging during the GRO solar campaign

Feb 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992nascp3137..514g&link_type=abstract

In NASA. Goddard Space Flight Center, The Compton Observatory Science Workshop p 514 (SEE N92-21874 12-90)

Computer Science

Frequency Synthesizers, Gamma Ray Observatory, Imaging Techniques, Microwave Frequencies, Solar Arrays, Solar Flares, Solar X-Rays, Brightness Temperature, Maximum Entropy Method, Microwave Emission, Solar Wind, Spectral Resolution

Scientific paper

The Owens Valley (OVRO) Solar Array was recently expanded to 5 antennas. Using frequency synthesis, the 5-element OVRO Solar Array has up to 450 effective baselines, which can be employed as necessary to make maps at frequencies in the range 1 to 18 GHz. Fortuitously, the last of the 5 antennas was completed and brought into operation on 7 Jun., just in time for the Gamma Ray Observatory (GRO)/Max 1991 observing campaign. Many events were observed jointly with OVRO and the BATSE experiment on GRO, including the six larger events that are presented in tabular form. Unfortunately, the X flares that occurred during the campaign all occurred outside the OVRO time range. The UV coverage of the newly expanded solar array, combined with frequency synthesis, should give a more complete view of solar flares in the microwave range by providing simultaneous spatial and spectral resolution. A promising application of MEM (maximum entropy) is also being pursued that will use smoothness criteria in both the spatial and spectral domains to give brightness temperature maps at each observed frequency (up to 45 frequencies every 10 s). Such maps can be compared directly with the theory of microwave emission to yield plasma parameters in the source - notably the number and energy distribution of electrons, for comparison with the x ray and gamma ray results from GRO.

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