This lecture commemorates the memory, so recent, of our esteemed and much-loved colleague, Steve Smerd, who died in Sydney a few days before Christmas day last year. The fact that there was a spontaneous move to pay our respects in this unusual way, dedicating an international scientific symposium to honour his memory, must mean that we are dealing with a special individual as a scientist. What do we remember about Steve, the scientist, that was special? I do not think it will be es pecially for his writings and publications. Although these included some that were definitive and highly significant, they were rather few in number. Although he has so much to tell Steve was not a good commu nicator through the written word. Though strictly logical, in a teutonic sort of way, his sentences had the tendency of never quite terminating, and their comprehension sometimes demanded of the reader the same kind of determined concentration as is required in the solution of a second order differential equation; he needed, and usually has, a co-author or a helper. To his Sydney-based colleagues by far his most famous writ ings were universally known as T the unpublished works of S.F. Smerd 1these, the mightly efforts that never quite came to the public eye, were voluminous indeed. No, Steve's method of communication was not through writing, but rather through a kind of oral evangelism. Paul Simon of Meudon Observatory, himself the holder of holy orders, once told me that a visit from Steve was like a visit from the Pope himself. It was not the fact that Steve was sometimes inclined to pontificate, but rather that, though a modest and self-effacing man, he spoke with such author ity and omniscient confidence about everything that one was left in no doubt that here indeed was the true word spoken by the priest from on high. Steve had many interests. I think always of his intense interest in politics which I described on another, more solemn occasion, as lying somewhere between old-fashioned liberalism and old-fashioned socialism. But his abiding interest above all else was the central point of his profession-the Sun. And in talking of the Sun and its basic under standing he interacted marvellously with his colleagues the world over. That is what makes him so special. He was always close to the observa-5
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 £ second and freqency intervals of about 5Mc/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 (ikm) 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 incor porated to facilitate the reduction of the complex data recorded.In its modified form, the equipment was put into operation on 1958 June 4, and the observations described here were taken during the ensuing 5 weeks. TYPE III BURSTSThe first problem to be investigated concerns the physical interpretation of the short-lived bursts of spectral type III. These bursts, which often occur in groups near the beginning of solar flares, are characterized by a rapid drift across the spectrum of the frequency of maximum intensity: the sweep from 70 to 40 Mc/s, for instance, occurs in about 1 to 3 seconds. We wished to test by direct means the suggestion [2,3] that the frequency drift is due to the excitation of plasma oscillations of frequencies that decrease with time as the exciting agency travels outward through regions of decreasing electron density in the solar corona. Assuming the usual estimates of electron den sity in the corona, the velocity of the exciting agency is calculated to be between 3 x 10 4 and 10 5 km/second. The method was to search for transverse motions of the sources across the sun's disk: if the theory is correct the transverse velocity should often be comparable with the inferred radial velocities, especially in the case of disturbances near the limb.Using the swept-frequency interferometer, the positions of a number of 176 available at https://www.cambridge.org/core/terms. https://doi
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