Selected High-Resolution Strip Scans of the 10.7-CM Sun.

Polarization interferometer for 2800 MHz solar noise studies with a 0.5? fan beam

“…The exact intensity at the limbs has not been determined because of the continual presence of active regions during this phase of the solar cycle. However, from previous studies, it is expected that the limb brightening will not be prominent on strip scans and that its existence will be largely contained in the extended width of the radio profile (Covington et al, 1962). At the time of the last sunspot minimum which occurred on 1964, 23 July, the total flux for this unique solar condition was 67.5 flux units.…”

“…This is illustrated in Figure 5 through the addition of the sunspot sketch to the same scale as the radio drift curve. As in previous studies of radio regions at this wavelength (Covington et al, 1962), the radio sphere of 1.02 solar radii must be considered. Further associations of the reamining radio regions, as well as for the three bright regions must be found from a study of other features such as the calcium plages.…”

“…A high resolution grating antenna designed for solar observations in the band from 2650 MHz to 2950 MHz and located at the Algonquin Radio Observatory, Lake Traverse, Ont., has been described by Covington et al (1967). This consists of an array of 32 three-meter parabolic reflectors with an aperture of 212.6 m and produces a fan beam 1.5' E-W by 2 ~ N-S without phase modulation.…”

“…In conjunction with proper switching of the radiometer output, this provides three channels to record output scans with different Stokes' parameters. The analysis is based upon that developed for the array of 32 elements (Covington et al, 1967) and the antenna patterns are summarized in Table I. Column 1 symbolizes the different orientations of the electric vectors in the two interferometer elements, while column 2 indicates the phase shift introduced by the (~2 modulator.…”