摘要:

The characteristics of solar flare type (s.f.) variations of the geomagnetic field at Huancayo, Kakioka, and Watheroo are statistically examined. The main indicators of these characteristics are the time from beginning of a s.f. variation to its maximum deviation (T1), and the ratio of its maximum deviation to the range of daily variation at the corresponding time (ΔH/RH). With respect to both quantities, the data of the three stations show nearly the same values. The magnitude of the s.f. variations at Huancayo is abnormally large, butT1and ΔH/RHshow normal values.Assuming that the s.f. variation has an abrupt increase, the integrated electrical conductivity of the ionosphere is estimated with the aid of a theoretical calculation of transient dynamo‐action. The result shows that the integrated conductivity of the ionosphere amounts to 6×10−8∼7×10−8emu. over those t

ISSN:0148-0227    

DOI:10.1029/JZ057i001p00001

年代:1952

数据来源: WILEY

摘要:

The motion of a semi‐infinite neutral ionized stream in a unidirectional magnetic field of increasing intensity parallel to the stream surface is considered. The ions and electrons in the stream are assumed to be devoid of random motion so that the stream surface remains plane throughout the motion. It is shown that the particles in the stream overtake those immediately in front so that the stream surface is constantly reformed by new particles arriving from the main body of the stream. The stream is thus able to penetrate further into the field than would be the case if they were alone in the field.The retardation of the stream surface is calculated and it is shown that the rate at which the velocity of this surface decreases compares well with the calculations made by S. Chapman and the writer in 1931. It is shown that the front surface of the stream is eventually brought to rest.The difficulties envisaged by S. Chapman and the writer [see 2 of “References” at end of paper] regarding the electrical conductivity of the stream are shown to be illusory, as had already been concluded by the authors in [1].The sudden increase in the horizontal force,H, above the mean over a period of about two minutes is here identified with a sudden commencement (SC) of a geomagnetic storm. The curve illustrating the rise inHshows considerable similarity to the curves of SCs derived on “quick‐run” magne

ISSN:0148-0227    

DOI:10.1029/JZ057i001p00015

年代:1952

数据来源: WILEY

摘要:

Twenty‐eight ultraviolet spectra of the aurora have been secured at Saskatoon with a single prism quartz spectrograph. Fifteen of these plates have been analyzed with a microphotometer and intensitometer, and integrated relative intensities obtained of the main spectral features. The intensities have been corrected for the effects of Rayleigh scattering and ozone absorption. The corrected intensities are carefully discussed, and it is shown that they yield vibrational temperatures less than 500°K. This is very different from earlier results, and additional measurements are desirab

ISSN:0148-0227    

DOI:10.1029/JZ057i001p00051

年代:1952

数据来源: WILEY

摘要:

A program of pressure measurements with rockets over White Sands, New Mexico, and over the equator has given values for atmospheric pressure, density, and temperature from the ground up to 160 km above sea level. The data have been obtained from about a dozen rocket flights at White Sands, New Mexico, latitude 32° north, longitude 106° west; and from one flight at the equator, longitude 160° west. Measurements were made in every month except April, June, and July. One rocket was flown at midnight, while the others were between 09h00mand 19h00mlocal time. Except for one daytime flight at White Sands, all the pressure data agree within the experimental errors. The fundamental data are pressures measured on the nose tips, nose cones, and tail sections of V‐2, Viking, and Aerobee rockets. From these measurements, atmospheric pressures, densities, and temperatures have been deduced. The pressure at 160 km is 2×10−6mm of Hg, and the density is 1.5×10−6gm/m3. The temperature reaches a maximum of 270°K at 50 km, a minimum of 190°K at 80 km, and increases to about 500

ISSN:0148-0227    

DOI:10.1029/JZ057i001p00059

年代:1952

数据来源: WILEY

摘要:

The expression for complex polarization given by the magnetoionic theory has been plotted on the complex plane using normalized parameters related to ionisation density and collisional frequency. Booker's definition of ordinary and extraordinary rays is used. This results in the entire realm of ordinary polarizations lying inside the unit circle. The symmetry of the chart is such that all desired information can be extracted from the first quadrant which is plotted in detail. Since experimental data are obtained in the form of ellipticity and tilt angle, another chart has been included relating these quantities to the same normalized parameters as appear on the complex polarization chart.To complete the graphical presentation, a nomogram has been included that aids in converting the normalized parameters on the two polarization plots to the corresponding ionization density and collisional frequency.

ISSN:0148-0227    

DOI:10.1029/JZ057i001p00073

年代:1952

数据来源: WILEY

摘要:

The intensity of the zenith skylight was measured for solar zenith angle of 90° to 106° for wave‐lengths of 0.75μ, 0.59μ, 0.52μ, and 0.44μ. The polarization was measured for the 0.44μ region. The difference between the measured polarization and the computed polarization of the primary scattered light was used to determine the fraction of the total zenith skylight that was due to primary scattering. The equation relating the atmospheric molecular density to the intensity of the primary scattered zenith skylight contains an extinction term. It was shown that the extinction term can be evaluated most accurately for the blue light. The computed atmospheric molecular densities agree with those given by the N.A.C.A. tentative standard at

ISSN:0148-0227    

DOI:10.1029/JZ057i001p00085

年代:1952

数据来源: WILEY

摘要:

The difficulties with the geometric optics (“classical”) definition of virtual height are discussed. The more general definition of virtual height in terms of the derivative of the phase of the reflection coefficient with respect to frequency is derived. It is then shown that the former definition can be derived from the latter, if phase integral method is used. The two definitions are compared in the specific examples of linear, rectangular, Epstein, and parabolic charge distributions.it is demonstrated, by means of examples, that the relation between virtual height and frequency derivative of phase is not valid when the reflected wave contains more than one pulse. In this case the frequency derivative of phase cannot be interpreted as the time delay of any one of the pul

ISSN:0148-0227    

DOI:10.1029/JZ057i001p00095

年代:1952

数据来源: WILEY

摘要:

The arguments in favor of the existence of solar corpuscles are reviewed and the geomagnetic action analyzed. The emission of the storm‐producing corpuscles is discussed in terms of the Milne‐mechanism acting onCaII ions, based on modern data on flares and on the chemical composition of the solar atmosphere. The long‐lived streams of solar corpuscles producing moderate disturbances of the earth's magnetic fields are identified with invisible extensions of the coronal streamers. They can be quantitatively understood as an evaporation of coronal protons into space. The unobservableM‐regions are probably associated with the coronal st

ISSN:0148-0227    

DOI:10.1029/JZ057i001p00113

年代:1952

数据来源: WILEY

摘要:

NocturnalEsionization and “no echo” occurrences, as recorded onh′frecords, have been classified according to the absence or presence of aurora and to its form when present in the zenith areas. The analysis supports the following generalizations. (1)Esionization increases at successively greater heights as aurora approaches the College zenith from the north. (2) In the presence of different nonpulsating auroral forms theEsionization varies with changes in auroral form in a manner similar to the change in luminosity. Likewise, variations in the height of maximum ionization parallel variations in auroral heights. (3) Complete absorption is only slightly more frequent during non‐pulsating aurora than during absence of aurora but prevails in the presence of pulsating aurora. Geomagnetic relationships are di

ISSN:0148-0227    

DOI:10.1029/JZ057i001p00121

年代:1952

数据来源: WILEY

ISSN:0148-0227    

DOI:10.1029/JZ057i001p00135

年代:1952

数据来源: WILEY