The flare data were compiled primarily from the flare lists of the IAU Quarterly Bulletin and a magnetic tape obtained from the Institute for Telecommunication Sciences and Aeronomy (ITSA). This tape was assembled from the CRPL-F Part B series (1955 through 1964) and included sub-flare reports. Altogether, 84,600 reports were compiled. In preparing the revised tape, tests were made for errors that were introduced at various stages in the handling of the data. Some errors were detected by comparing the entries for flare time, position, and importance of the flare reports found in both the CRPL and IAU flare lists. Only slightly more than one-third of all reports were so compared, but these included practically all flares of importance> or = 1 during the period 1955 through 1962. Errors in reported flare areas were detected by matching reports between the two flare lists and by testing the areas as a function of central distance. This check uncovered flare reports in which the measured and corrected areas were reversed. Other errors were detected by checking for consistency of the information within each flare report. These various tests disclosed a 12.5 percent error in the flare reports of the CRPL-F Part B series, and an 11.2 percent error in the Quarterly Bulletin flare list. After correction of all identified errors, the revised magnetic tape listing may still contain a 5 percent error. Most of these discrepancies are in the sub-flare reports.

This is a summary of the ten years (1955-1964) of observations of solar flares reported by 61 observatories. The flare reports have been published predominantly in the IAU Bulletin and CRPL-F Series Part B. This report summarizes the types of information contained in the flare reports, and the frequency of some parts of these reports as functions of many parameters. The results reflect the need for closer cooperation and coordination of participating observatories in recording and reporting solar flare data.

The solar radio sweep-frequency observations and hours of patrol from five rad radio observatories for the period 1955 through 1964 have been compiled, edited, and put onto two magnetic tapes. One tape contains the hours of radio patrol from the observatories at Ann Arbor, Bigpine, Boulder, Sydney and Fort Davis. Another tape contains the sweep-frequency observations in the meter and dekameter wavelengths of the radio spectrum from these observatories. The sources, methods of reduction, and the format and content of the data on tape are described. Statistics related to various distributions of the radio spectral activity reported by each station are discussed and demonstrate an urgent need for standard policies in detecting, scaling, classifying, and reporting these data.

A decade of data on the operation of the international solar flare patrol has been collected and analyzed. These data were compiled from World Data Centers A and C, and from the individual observatories. Tests were made to correct errors introduced in the recording and handling of the data. This paper describes the data sources, error editing program employed, and the magnetic tape which has been prepared and contains the available hours of H-alpha patrol from 55 observatories for the period 1955-1964. A few tables are included showing some of the information available from the tape.

Lists citations with abstracts for aerospace related reports obtained from world wide sources and announces documents that have recently been entered into the NASA Scientific and Technical Information Database.

A flare event list that is consistent with flare patrol times is prerequisite to a reliable, unbiased estimate of flare occurrence per unit patrol time. A comparison of the flare occurrence times and flare patrol times reported by 52 solar observatories during the period of 1955 to 1964 discloses that 12.3 percent of the flare reports (Importance = or > 1) have no reported patrol coverage. Elimination of these 'unpatrolled' flare reports reduces the number of individual flare events in the data sample by 9.7 percent. This means that flare occurrence per unit patrol time computed from the raw flare and flare patrol data is overestimated by this same percentage. In addition to eliminating 'unpatrolled' flare reports, appropriate adjustments are made in the 'patrolled' flare data so as to make each observatory's reported flare times completely consistent with its reported patrol times.