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The transverse motions of the sources of solar radio bursts

Published online by Cambridge University Press:  14 August 2015

J. P. Wild ,
K. V. Sheridan  and
G. H. Trent
J. P. Wild
Affiliation:
Radiophysics Laboratory, Commonwealth Scientific and Industrial Research Organization, Sydney, Australia
K. V. Sheridan
Affiliation:
Radiophysics Laboratory, Commonwealth Scientific and Industrial Research Organization, Sydney, Australia
G. H. Trent
Affiliation:
Radiophysics Laboratory, Commonwealth Scientific and Industrial Research Organization, Sydney, Australia

Extract

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Observations of the spectrum of solar radio bursts at meter wavelengths have indicated the desirability of measuring positions on the sun's disk not only as a function of time but also as a function of frequency. With this objective in view, we are now using a swept-frequency interferometer to determine the east-west disk coordinate of the transient solar sources at time intervals of ½ second and freqency intervals of about 5 Mc/s within the frequency range 40 to 70 Mc/s. The accuracy to which the centroid of the source is located is about ±1 minute of arc. In its initial form [1], the interferometer contained two aerials separated by a distance of 1 km. As a result of preliminary tests, two major additions have been made: (1) a second interferometer of much smaller spacing (¼ km) has been added to resolve the usual ambiguities associated with two-aerial interferometry, and (2) an automatic system of lobe-switching and phase-calibration has been incorporated to facilitate the reduction of the complex data recorded.

Type
Part II: The Sun
Information
Symposium - International Astronomical Union , Volume 9: Paris Symposium on Radio Astronomy , 1959 , pp. 176 - 185
Copyright
Copyright © Stanford University Press 1959 

References

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