摘要:

The results from the GM counter telescope on. board the Imp 1 satellite are presented. The detector system consisted of four pancake‐type GM counters forming two mutually perpendicular telescopes and an omnidirectional detector. Comparison of the intensity measured by the two perpendicular telescopes reveals an anisotropy in the recovery phase of the 11‐year variation. Time variations of the omnidirectional intensity were correlated with the planetary indexKp, and inferences about interplanetary field irregularities and solar wind cavity structures are presented. These results are shown to be in general agreement with Parker's description of the cosmic‐ray modulation by the solar

ISSN:0148-0227    

DOI:10.1029/JZ070i009p02005

年代:1965

数据来源: WILEY

摘要:

Protons in the range 1 Mev

ISSN:0148-0227    

DOI:10.1029/JZ070i009p02021

年代:1965

数据来源: WILEY

摘要:

The spatial distribution and energy spectrum of trapped protons observed by Injun 1 (1961) are in agreement with the suggestion that low energy protons found atL>1.6 result from the radioactive decay of neutrons produced in the polar atmosphere by solar protons. Large fluxes of 1‐ to 15‐Mev protons are found as low asL= 1.4, however, indicating that several modifications are required in Lenchek's model for the Nerv results. These modifications are discussed qualitatively. The Injun 1 fluxes of 1‐ to 15‐Mev protons agree with the Relay 1 fluxes of 1.1‐ to 14‐Mev protons in the region 1.6

ISSN:0148-0227    

DOI:10.1029/JZ070i009p02035

年代:1965

数据来源: WILEY

摘要:

With Injun 1 data for the inner Van Allen zone in the South Atlantic anomaly, it is shown that trapped protons 1 Mev

ISSN:0148-0227    

DOI:10.1029/JZ070i009p02045

年代:1965

数据来源: WILEY

摘要:

A neutron density measuring system was orbited on a polar satellite in September 1962 and recorded neutron counting rates for two days. The shape of the latitude variation of the measured neutron density was consistent with the shape predicted by Lingenfelter, but the absolute values were about a factor of 3 higher than the predicted densities. The latitude variation amounted to a factor of 10:1 between the poles and the equator. The results were sorted both intoLintervals and into Quenby and Wenk rigidity intervals. It is seen that the L distribution is a much smoother variation than the rigidity distribution. The results of the experiment give an upper limit to the neutron density equal to (1.1±0.2)×10−7neut/cm3at the poles. It is not clear how much of this measured density is contributed by local product

ISSN:0148-0227    

DOI:10.1029/JZ070i009p02057

年代:1965

数据来源: WILEY

摘要:

The reality of a ‘statistical’ solar cosmic‐ray increase has been claimed by some workers and questioned by others. In the present study, a definite statistical increase is found to be associated with solar events producing meter type IV bursts. On the other hand, decimeter and microwave type IV's, unaccompanied by meter IV's, are not associated with any increase. Cosmic‐ray data from 21 stations distributed over the world and covering the period July 1957 through December 1960 are used. The statistical increase, in contrast to the large, unusual increase, is too small to show up definitely in the data for a single event from a single station; superposition of observations is required to bring out any effect. The characteristics of the statistical increase examined here are: (a) The magnetic cutoff rigidity dependence is similar for the statistical increase and the large, unusual increase, if the latter is measured several hours after the flare. (b) The statistical increase has an isotropic particle flux distribution, (c) The time delay from the flare to the intensity maximum of the statistical increase is about 8 to 1

ISSN:0148-0227    

DOI:10.1029/JZ070i009p02065

年代:1965

数据来源: WILEY

摘要:

An intensive study has been made of data from three 213 GM tubes and one 302 GM tube that were carried on the State University of Iowa‐Office of Naval Research satellite Injun 3. Median‐latitude profiles of the electron population of the low‐altitude region of the outer zone for energiesEe≳ 40 kev,Ee≳ 230 kev, andEe≳ 1.6 Mev have been derived. Notable features of the median profiles are: (1) the large diurnal variation forL≳ 7.5 for trapped and precipitated 40‐kev electrons; (2) the lack of a sharply pronounced ‘slot’ for 40‐kev electrons and the consequent softening of the integral electron spectrum aroundL= 3.0; (3) an apparent small diurnal variation of 230‐kev trapped electrons for 6 ≤L≲ 8; (4) a temporal change of about one order of magnitude in the intensity profile of 1.6‐Mev electrons, which preceded and was followed by periods of relatively stable intensity for 2 ≤L≲ 4.5. This change occurred during aKp= 7 magnetic storm that began on June 6, 1963. The dependence of intensity on |B| was investigated with the following results: (1) For specified L values in the range 2 ≤L≲ 7.5 there is an apparent decrease in intensity of 40‐ and 230‐kev electrons of about two to three orders of magnitude for |B| going from ∼0.2 to ∼0.5 gauss. (2) The intensity of 1.6‐Mev electrons also decreases about two orders of magnitude with |B| going from ∼0.2 to ∼0.5 gauss, and for 2 ≤L≲ 4.5 the decrease in intensity

ISSN:0148-0227    

DOI:10.1029/JZ070i009p02077

年代:1965

数据来源: WILEY

摘要:

The intensity and energy spectrum of primary cosmic‐ray protons having energies between 80 and 200 Mev have been studied in nuclear emulsions flown on August 26, 1960, over Fort Churchill. The upper limit to the intensity between 80 and 150 Mev of 53±6 protons m−2sec−1ster−1obtained in this experiment is compared with the value of 121±6 protons m−2sec−1ster−1quoted byVogt[1962] from observations made just before and just after this experiment. The reasons for this differenc

ISSN:0148-0227    

DOI:10.1029/JZ070i009p02111

年代:1965

数据来源: WILEY

摘要:

The flux of precipitating electrons in the northern auroral zone has been measured with scintillation‐type detectors aboard a polar orbiting satellite. The total preciptated energy and spectrums of electrons with energies greater than 180 ev were observed on each of 6 traversals of the auroral zone over distances of hundreds of kilometers. In most instances the dominant contribution to the preciptated flux was from electrons with energies of less than 10 kev. Spectral measurements were made 128 times per second (every 63 meters), and rapid fluctuations in both total precipitated energy and spectral shape were observe

ISSN:0148-0227    

DOI:10.1029/JZ070i009p02119

年代:1965

数据来源: WILEY

摘要:

Electron energy spectrum measurements were made in October–November 1963 from a polar orbiting satellite with an apogee of 355 km and a perigee of 288 km. Data were taken with a plastic scintillation spectrometer equipped with a 16‐channel pulse height analyzer operating in two energy ranges, 0.3 to 2.6 Mev and 0.3 to 10.0 Mev. The data presented were all taken atB,Lpoints whose traces have minimum altitudes of 200 to 355 km. In the Starfish region (L∼ 1.3) the spectrum was fissionlike at energies above ∼2 Mev and rather flat below this energy, whereas on higherLshells the spectrum was considerably softer. The spectral shapes were fitted to the exponential formdϕ/dE= Ae−μE, with a different value of μ for each of three different energy intervals (0.28 to 0.88 Mev, 0.88 to 2.08 Mev, and 2.08 to 4.88 Mev). The energy spectrum, during the period after the sudden commencement of October 29, 1963, underwent significant temporal changes forL≳ 3, but always displayed a general softening with increasingLvalue, except for hardening at L ≈ 3–5 corresponding

ISSN:0148-0227    

DOI:10.1029/JZ070i009p02129

年代:1965

数据来源: WILEY