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• W3147372130 abstract "Measurements of the cosmic-ray intensity have now been made for most of the past solar cycle at balloon altitudes near the north geomagnetic pole. Such experiments have been conducted during the summer months, but these data are thought to represent a relatively true measure of cosmic rays in the vicinity of the earth for that particular phase of the solar cycle, since large solar flare activity was absent when these flights were made. It is found (1) that the energy density of cosmic rays in the vicinity of the earth was 40 per cent less in 1958-1959 than in 1954; (2) that the new particles present in 1954 that were not present in 1951 were almost entirely those absorbed in 200 g cm -• of the atmosphere; (3) that after the cosmic-ray maximum of 1954 the first particles to disappear wore very absorbable, having an absorption length of about 60 g cm-•; (4) that as the solar cycle progressed the particles removed became increasingly energetic, until those that disappeared between 1957 and 1958 were absorbed about like primaries of mean rigidity 9 bv; (5) that the particles now reappearing after the cosmic-ray minimum of 1958-1959 have close to the same rigidity as those removed before the cosmic-ray minimum was reached, when the intensity was approximately the same; (6) that, if the general solar activity can be measured by the Zurich sunspot numbers, there appears to be a 9to 12-month lag of cosmic-ray change from being anticorrelated with solar activity; and (7) that sunspot numbers averaged over periods like a quarter of a year appear to be a better measure of solar activity as it relates to cosmic-ray intensity than similarly averaged planetary magnetic character figures. Introduction. The present series of measurements has extended over the decade 1951 to 1961, with but two years, 1952 and 1953, missing. Previous measurements in 1936-1937 give information about cosmic-ray intensity during an earlier period when the sun was at a maximum of activity. In the years 1936-1937, 1951, 1954, and 1958 latitude surveys were made; in the years 1955, 1956, 1957, 1959, 1960, and 1961 measurements were made near the north geomagnetic pole only. With the conclusion of the 1961 experiments it becomes possible to point out some general characteristics of the changes that have occurred in cosmic rays at balloon altitudes for the period being considered. The instrumentation used in the 1951-1961 series of balloon flights consisted of similar apparatus, particularly designed for simple telemetering of data. That used previously was photographically recording. However, since all the instruments were carefully compared with laboratory standards, it is believed that direct comparisons of the data may be made to q-1 per cent over the 25 years in which such measurements have been made. The instruments used have been described Now at the Jet Propulsion Laboratory. elsewhere [Neher and Johnston, 1956]. The ionization due to cosmic rays is measured by thinwalled ion chambers, up to heights of about 100,000 feet. Such data provide a measure of the total energy per unit of area brought into the top of the atmosphere and information about the way in which the radiation that changes from one year or period to another is absorbed in the atmosphere. For the present discussion, in which the intensity of cosmic rays in the vicinity of the earth's orbit is to be studied, four requirements must be met. (1) We need to be reasonably certain that no short-term changes are occurring. Thus it is desired to avoid the effects of solar bursts of high-energy particles as well as Forbush decreases. (2) We must make measurements as close to the top of the earth's atmosphere as possible. (3) A base station at relatively high geomagnetic latitudes is necessary for making measurements simultaneously with the roving station where latitude surveys are made. This allows most changes in the primary radiation to be accounted for. Such a procedure was followed in the 1951, 1954, and 1958 surveys. (4) To study the low-energy primary particles we must make measurements not only at high altitudes but also in high latitudes. 1309 1310 NEtIER AND ANDERSON Cosmic rays at Thule •or the years 1959, 1960, 1961. Measurements of the intensity of cosmic rays at Thule, Greenland, (kin 88oN) for the years before 1959 have been published elsewhere [Neher, 1956, 1957, 1959; Neher, Peterson, and Stern, 1953]. For the years 1959, 1960, and 1961 some of the pertinent data for the balloon flights that were made are given in Table 1. Also given in the table is the ionization at the maximum of the ionization versus depth curves. In 1959 there was less than 4-0.8 per cent variation from the average for the 6 flights made at Thule over a period of 17 days. In 1960 the intensity was not as constant, but the maximum departure of the ionization from the average, at the maximum of ionization, was 4.1 per cent. To illustrate the internal consistency and accuracy of the data obtained on a single flight, the results of August 7, 1961, are plotted in Figure 1. In this flight the balloon reached a pressure of 8.3 gcm -•-, which corresponds to a standard atmosphere height of somewhat more TABLE 1. Data from Balloon Flights Made at Thule, Greenland (Xm 88oN), for the Years 1959, 1960, 1961 Date Time when Balloon Maximum Reached Ionization, Minimum Minimum ions cm -• Pressure, Pressure, see -• atm -• GMT gcm -•' of air 1959 July July Aug. Aug. Aug. Aug. 1960 July July July Aug. Aug. Aug. Aug. Aug. 1961 July Aug. Aug. Aug. Aug. Aug. 29 31 6 9 12 15 26 28 30 2 6 8 10 12 29 1 3 5 7 9 1655 1655 1546 1622 1508 1637 0900 0823 0853 0810 0803 0719 0729 0715 0832 0807 0756 0849 0730 0806 15 5 23 8 16 2 95 18.0 80 11 0 15 0 10 0 11 5 160 49 0 13 1 19 I 10 0 94 91 10 9 83 89 249 5 249 8 248 3 251 3 250 9 251 8 283 3 281 4 282 4 283 2 292 4" @default.
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• W3147372130 date "2007-01-01" @default.
• W3147372130 modified "2023-09-27" @default.
• W3147372130 title "Cosmic Rays at Balloon Altitudes and the Solar Cycle" @default.
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