Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992cait.rept.....h&link_type=abstract
Final Technical Report, 1 Oct. 1988 - 30 Nov. 1991 California Inst. of Tech., Pasadena.
Astronomy and Astrophysics
Astronomy
Astronomical Spectroscopy, Brightness Temperature, Magnetic Flux, Microwave Spectra, Radio Spectra, Solar Activity, Solar Corona, Solar Spectra, Thermal Mapping, Antenna Design, Astronomical Observatories, Frequency Synthesizers, Image Resolution, Parabolic Reflectors, Radiation Sources
Scientific paper
In studies of solar active regions and bursts, the ability to obtain spatially resolved radio spectra (brightness temperature spectra) opens a whole new range of possibilities for study of the solar corona. For active regions, two-dimensional maps of brightness temperature over a wide range of frequencies allows one to determine temperature, column density, and magnetic field strength over the entire region in a straightforward, unambiguous way. For flares, the time-dependent electron energy distribution, number of accelerated electrons, and magnetic field strength and direction can be found. In practice, obtaining complete radio images at a large number of frequencies is a significant technical challenge, especially while keeping costs down. Our instrument at Owens Valley Radio Observatory provided the starting point for a modest attempt at meeting this goal. We proposed to build three additional, very low-cost 2-m antennas which, when combined with our existing two 27-m dishes, expands the array to 5 elements. This modest increase in number of solar dedicated antennas, from 2 to 5, increases our maximum number of physical baselines from 1 to 10 and allows the instrument to do true imaging of solar microwave sources, both bursts and active regions. Combined with the technique of frequency synthesis, the new array has up to 450 effective baselines, giving imaging capability that approaches that of a sub-arrayed VLA. The prototype antenna design was finalized and the antenna was put into operation in Nov. 1989.
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