Frazier (1972)
criticized the conclusions of Veeder and Zirin (1970) and of Foukal (1971) on the relation of chromospheric morphology to magnetic fields. No sooner was this answered by Foukal and myself (Foukal and Zirin, 1972) when a second, more strident criticism by Frazier (directly preceding in this journal) of a more recent paper by myself (Zirin, 1972) was submitted. Solar physics is not furthered by the invective he has used, and further argument only makes the matter worse; but I feel I have to answer Dr Frazier's points to clarify the status of the He: B relations both for him and the solar physics community. Frazier specifically accuses me of (1) hasty generalization; (2) lack of proof; (3) misquotation, and (4) confusion of terms. I plead 'not guilty' to all four.
(1) Hasty generalization: the relations between Ha and B have been presented in a series of papers (Zirin, 1971; Zirin, 1972; Foukal, 1971a, b;Prata, 1971) which show the development of the relations as better data became available. So far as the results of these specific papers are concerned, it is moot to discuss whether a few cinematogram-magnetogram pairs define a relationship, because great numbers of magnetograms are now available. For example, the Leighton-Smithson videomagnetograph operates, with a flip mirror, on one of the Big Bear refractors, producing hundreds of He:B pairs each day. No significant deviation from the rules set forth by Zirin (1972) has appeared. However, in general, there will always be a few 'best' pairs available, which will enable us to extend the relationship further. On every Ha: B pair dozens of different features may be seen. As was pointed out by Veeder and Zirin (1970), the relationship of each He:B feature is repeatable and typical, so that what Frazier terms 'hasty generalization' in fact provides very good rules for studying further data. It is always a difficult matter to stop and analyze the data at hand rather than wait for something better in the future. The ongoing analysis permits one to interpret currently available data and to properly channel the obtaining and interpreting of new data. For example, it was early apparent from the slow time change of Ha features and the He:B relations that magnetic features changed slowly. Had this been properly recognized, the new magnetographs would not have had to be designed for rapid repetition. In fact, most of these instruments are now used with relatively long intervals between magnetograms because the fields do change only slowly.
It should be obvious to Frazier that behind each set of data we have published there was considerably more that was not included because of the overcrowding of the journals. A short trip to Pasadena or an inquiry to us could have brought this before him.