bluuebunny/crossref_metadata_2025 huggingface dataset:
Supplementary note on a graphical method of computing diurnal variations by differential formula
Authors: Duvall C. R. , Ennis C. C.
Published: February 2008

Equation (2) of our former note1 may also be written:

The interpretation of this equation as a “collinear‐points” graph shows how the graph may be very simply constructed in all cases. The scales for the given quantities, ΔH, ΔD, and ΔZ, are laid off on parallel straight lines, graduated uniformly in the same unit. The usual convention of signs, positive to the right and negative to the left, may always be adopted for these scales, thus making the “setting” more mechanical and therefore less liable to error of sign. Accurate squared paper, such as K. and E. “Standard Cross Section 1.0×10” will supply these scales already made, inking in to catch the eye being all that is further required. The array of superfluous lines in this case will detract from the usual simple appearance of the “collinear‐points” graph, but it has been found in actual practice that these lines do not materially hamper work with the graph. The ΔD and ΔZ scales are often most advantageously made identical. The distance of the zero of the ΔH scale from those of ΔD and ΔZ is arbitrary, as is also the angle the line of zeros makes with the parallel scales. By a suitable choice of this distance and angle and of the unit, 1′ or 1γ, the graph may be made to take the most favorable form for determing the required quantities.
Summary of atmospheric‐electric investigations during airplane flights
Authors: Halle A. S. , Wigand Albert
Published: February 2008

The special advantages offered by the airplane for the solution of atmospheric‐electric problems have been utilized by the author in collaboration with Messrs. Keppe, Schlomka and Wenk, for carrying out three investigations, during which a general study was first made of the physical conditions under which work in airplanes must be done, and then corresponding methods of measurements developed.

1. For determining the mean value of the ionic content of the atmosphere,2 E, for a given time, an Ebert ion‐counter was adapted to the experimental conditions of an airplane and tried out on two flights. Between altitudes of 3.3 and 5.2 km, E increases with altitude, and at 5.2 km the number of positive ions is greater than that of negative ions. A method of determining the instantaneous values of the ionic content and of the conductivity in an airplane by current‐measurement, was given.
Results of magnetic observations made by the United States Coast and Geodetic Survey at the time of the solar eclipse of January 24, 1925
Authors: Hazard Daniel L.
Published: February 2008

In order to secure additional information regarding the effect of a solar eclipse on the Earth's magnetism, the United States Coast and Geodetic Survey arranged to have special observations made at Ithaca, New York, at the time of the eclipse of January 24, 1925, in accordance with a program recommended by the Department of Terrestrial Magnetism of the Carnegie Institution of Washington, the station selected being near the central line of the belt of totality. The program included eye‐readings of declination and horizontal intensity once a minute for a period of six hours on January 23, 24, and 25, and dip observations once in two minutes during the same periods.

Through the courtesy of Professor E.G. Merritt of Cornell University, a building on the University farm at Ithaca was made available for the mounting of the instruments and three of his students volunteered to assist in the observations. These men, Messrs. Larson, Taylor, and Childs, deserve much credit for the faithful performance of the duties assigned to them under the very trying conditions which prevailed. R.R. Bodle, magnetic observer, had charge of the mounting of the instruments and made the preliminary observations. Commander N.H. Heck, chief of the Division of Terrestrial Magnetism, took charge of the magnetic observations of the regular program, while Mr. Bodle devoted his attention to observations of the atmospheric potential‐gradient with instruments supplied by the Department of Terrestrial Magnetism of the Carnegie Institution of Washington.
An intensity variometer corrected for temperature
Authors: Hartnell George
Published: February 2008

1. Theory.— The symbols used are as follows:

M0 = magnetic moment of suspended magnet at standard temperature;

MC0 = magnetic moment of compensating magnet at standard temperature;

q1 = temperature coefficient of suspended magnet;

q2 = temperature coefficient of compensating magnet;

M = M0 (1 ‐ q1t) = moment suspended magnet at temperature t;

Mc = Mc0 (1 ‐ q2t) = moment of compensating magnet at temperature t;

τ = angular torsion in fiber when suspended magnet lies in prime vertical;

ψ = angle between axis of suspended magnet and prime vertical;

h = torsion factor;

r = distance between centers of suspended magnet and compensating magnet;

H = horizontal intensity.
Biographical sketch of Marc Deschevrens, S.J.
Authors: de Moidrey J.
Published: February 2008

Father Marc Deschevrens, S.J., lately deceased, should not be forgotten among magneticians of the last century. He was born in Switzerland, July 26, 1845, became a Jesuit, and was scientific master in the college of Vaugirard, Paris. He was chosen to found a magnetic observatory in China, according to the advice of Fathers Secchi of Rome, and Perry of Stonyhurst, England. On November 29, 1873, he arrived in Zi‐ka‐wei, where a private meteorological station had been inaugurated a few years previously, and entered at once on his magnetic measures, beginning a series which is still carried on by his successors.
Principal magnetic storms and earthquakes recorded at the Watheroo Magnetic Observatory, April to June, 1926
Authors: Johnston H. F.
Published: February 2008

(Lat., 30° 19′.1 S.; long., 115° 52′.6 or 7h 44mE. of Gr.)

April 14–16, 1926.—Though disturbed generally, the month of April 1926 presents only one storm of any severity, that occurring on April 14–16. This storm began with a relatively mild commencement at 13h 53m, when all the elements increased slightly. At 14h 02m they changed more abruptly, still increasing, however. A general decline in the value of horizontal intensity followed, and the greatest departure from the mean monthly value occurred at 6h 50m on April 16; the downward trend was interrupted several times, notably at 20h 41m on April 14.
Principal magnetic storms and earthquakes recorded at the Watheroo Magnetic Observatory, July to December, 1926
Authors: Johnston H. F.
Published: February 2008

(Lat. 30° 19′.1 S.; long. 115° 52′.6 or 7h 44m E. of Gr.)

July and August, 1926.—There were no marked magnetic disturbances during these months.
Some new remarks on the cause and propagation of magnetic storms
Authors: Rodés Rev. Luis
Published: February 2008

As the hypothesis advanced by the author in “Terrestrial Magnetism and Atmospheric Electricity” (December, 1922) has aroused considerable interest, a few remarks by me on the same subject might be opportune.

The new and essential point of my hypothesis was stated on page 162 of the article cited, in the following words: “If a magnetic storm is due to the Earth's entering a cloud of electric particles projected from the Sun ... the storm will first be registered at those observatories which are nearer the front meridian, as I have designated the one, which, because of the Earth's rotation, happens to be foremost in direction of movement at the moment the storm begins. Accordingly, an observatory which registers the storm at six o'clock local time, should be the first of all to record it; next would follow those nearer to it on either side, and last of all the one at which the storm began at 18 h. local time.” I added that this hypothesis rests to some extent on facts which were given in the same article.
Weighting by mean differences
Authors: Fisk H. W.
Published: February 2008

It is often desirable to express, according to some suitable criterion, the order of agreement of separate results obtained in repeated measures of a constant quantity, or the amount of dispersion or scattering of values of some periodically recurrent natural phenomenon. Often the range, or difference between extreme values of the group, furnishes a rough, and for some purposes, sufficient criterion. Where greater mathematical precision is desired, the mean error of a single observation,
is used. A criterion more easily derived than the latter when the number of quantities in the group is small, and more reliable than the simple range, is provided by the mean difference.
Biographical sketch of Colonel Francisco Afonso Chaves
Authors: Agostinho J.
Published: February 2008

(Late Director of the Meteorological Service of the Azores.)

Colonel Chaves was born in 1857. He was a laureate pupil of the Military Academy in Lisbon, but later devoted himself to the study of science and became prominent in meteorology and natural history.
The relation of the magnetic work of the United States Coast and Geodetic Survey to geophysical prospecting methods
Authors: Hazard Daniel L.
Published: February 2008

Although the Coast and Geodetic Survey has never had funds available for an intensive study of the relation between underground geological formations and the distribution of the Earth's magnetism at the surface, nevertheless, in the execution of a magnetic survey of the United States, it has accumulated a large amount of valuable data which is available for those who may desire to make such a study.

The magnetic work of the Survey was begun as one of the essential operations in the making of navigational charts, and was later extended to meet the needs of the surveyor making or retracing compass‐surveys. Both of these needs would have been met by the determination of the magnetic declination alone. It was recognized at the outset, however, that little progress could be made in a study of the nature of the Earth's magnetism based on a knowledge of only a single element, and the practice was adopted of determining the dip and horizontal intensity at the stations, as well as the declination. As a result of this wise policy, there are now available values of these three magnetic elements at about 5,000 places in the United States, most of them determined since 1900. From these the vertical intensity and total intensity can be readily computed.
Note on a vertical‐intensity variometer
Authors: Ryd V. H.
Published: February 2008

It is well known that the vertical‐intensity (Z) variometer is considered the most unsatisfactory variation‐instrument of the magnetic observatory, and although various types have been proposed, there is as yet no really good design. However, the possibility is not precluded that the old Lloyd's balance, in a somewhat altered form, may give good results, as the following data show.

In the magnetic observatory in Rude Skov (literally, Rude Forest) at Copenhagen there has been used for some time a small Z‐variometer, the most conspicuous feature of which is the lightness of its moving parts, the needle, together with suspension, mirror, etc., weighing only about five grams. Because of the small weight, it has been possible to make the point of the pivots very fine. Following a suggestion by D. la Cour, the apparatus was mounted in an air‐tight bell‐glass from which the greater part of the air was removed. The variometer was made by the instrument‐maker M. Laessöe‐Müller of Copenhagen.
Remarkable auroral display of July 7 to 8, 1928
Authors: Harradon H. D.
Published: February 2008

A number of communications giving details of the remarkable auroral display on the night of July 7–8, 1928, have been received. Among these is a summary with 20 reports from Dr. Willard J. Fisher of Harvard College Observatory, covering an area extending from Maine to Texas and from Michigan to 100 miles east of Boston, Massachusetts. The east‐west extension is thus seen to be very great, although the aurora is not limited by the reports in that direction. At sea north of Cape Charles Light there was seen a broad arch of light from northwest to northeast, about three degrees wide, with its center about five degrees under the North Star.
Preliminary results of ocean magnetic observations on the Carnegie from Japan to California to Hawaii, June to September, 1929
Authors: Ault J. P.
Published: February 2008

After leaving Yokohama June 24, the first ten days were featured by light variable winds and calms. The engine was operated frequently and the average day's run was about 90 miles. Advantage was taken of a smooth, calm sea on June 27 and 28 to swing the vessel for deviations. One helm for declination‐observations was made on June 27 before the clouds covered the Sun; all the next day was spent in making a swing with both helms for inclination and horizontal intensity.
Note on a theory of the permanent magnetic fields of the Sun and Earth
Authors: Gunn Ross
Published: February 2008

Dr. J. Bartels has recently pointed out in a letter to the Editor of this JOURNAL that in the writer's paper on “A theory of the permanent magnetic fields of the Sun and Earth”1 the step from equation (4) to equation (5) in neglecting the first term of the bracket in (4) is not clearly indicated. In the derivation it was foreseen that the terms which would contribute to the drift‐currents would be terms containing higher powers of sin θ than the first, since the effects must be averaged over all values of θ from 0 to 2π. The term which Dr. Bartels points out should be retained was multiplied into sin θ which when averaged with respect to θ, reduced to zero. Thus the final form of the expression is as given in (5).
Latest annual values of the magnetic elements at observatories
Authors: Fleming J. A.
Published: February 2008

In compiling the above table the data have been entered for every five years from 1900 or from year of beginning of the observatory if later than 1900. Yearly values subsequent to 1920 or 1925 are given so that the accelerations in the secular variations may be noted.

The uneven distribution of magnetic observatories is strikingly evident and in particular the lack in the southern hemisphere, especially in Africa and the oceanic areas. This is further emphasized by reference to the above tabulation of the magnetic elements as published by observatories, of which there are about sixty active ones observing and reporting upon all three elements, and about one dozen observing declination only. In this connection, it is to be noted that at many of the observatories absolute observations only are made. For the study of magnetic storms and other world‐wide effects and of secular variations, observatories should be added to effect a more uniform distribution. Thus locations for other fully equipped observatories which would contribute greatly to the needs of research in terrestrial magnetism could be established in Cape Colony, Belgian Congo, French West Africa, Easter Island, St. Helena, Eritrea, Solomon Islands or New Caledonia, and Guam.
Variation of horizontal‐intensity variometer scale‐value with temperature
Authors: Hartnell George
Published: February 2008

In a paper on horizontal‐intensity variometers the author developed the mathematical relations underlying the operation of horizontal‐intensity variometers and showed how, in the case of quartz‐filament suspension, the scale‐value may be controlled and compensation for temperature secured by use of suitably placed auxiliary magnets. Further development of the formulas shows that if too large a filament is used, change of temperature may have an appreciable effect on the scale‐value.
Some notes regarding auroral displays during the months of August and September, 1930
Authors: Harradon H. D.
Published: February 2008

A number of communications have been received from various sources giving detailed descriptions of auroral displays observed at points in the United States and Canada during the months of August and September, 1930. As these notes may contain material of interest to readers of the JOURNAL, they are presented below in somewhat condensed form.

Aurora of August 6, 1930—The following report by L. E. Cunningham and E. M. Lindsay, describes the aurora as observed at the Harvard College Observatory:
Sitka Magnetic Observatory October to December, 1930
Authors: Ulrich Franklin P.
Published: February 2008

(Latitude 57° 03′.0 N.; longitude, 135° 20′.1, or 9h 01m.3 W. of Gr.)

October 17–18, 1930—Although this storm was relatively short, it was active for most of its duration. There was a little sudden jog in the curves at the point of beginning and for several hours there was practically no activity. At 18d 6h the curves began the large slow oscillations which lasted until 10h, when the oscillations became rapid. From 18d 13h to 18h the motion of the curves was so rapid that they show up mostly as spots. However, the curves can be followed quite definitely except at times during the latter part of this period. For a storm of this intensity, the H‐maximum usually goes very high at the beginning of the storm. In this storm, however, the H‐maximum, although occurring at the beginning of the storm, did not go much above the normal value. Hence, the range in H was relatively small.
American URSI broadcasts of cosmic data
Authors: Clarke Katharine B.
Published: February 2008

The first three columns of the Table give (1) the magnetic character according to the scale 0–2 of the International Commission of Terrestrial Magnetism and Electricity, (2) the type featuring the day other than normal by the letters b, p, o, and i for days marked by bay, rapid pulsations, long‐period oscillations, and irregular oscillations, respectively, and (3) the hour and minute of Greenwich mean time marking the beginning of a storm, the end of the storm being indicated in the footnote to the Table. The next two columns give the data relating to sunspots: (1) the number of groups of spots and (2) the total number of spots. It is to be noted that sunspot‐numbers such as those from Zürich can be obtained from the number of groups and spots given in the Table by the formula N = k (10g + s), where k for Mount Wilson is about 0.77. The sixth and seventh columns show (1) the value in calories of the solar constant, and (2) by letters s, f, and u whether the determination was satisfactory, fair, or unsatisfactory, respectively.
Cheltenham Magnetic Observatory January to March, 1931
Authors: Hartnell Geo.
Published: February 2008

(Latitude 38° 44′.0 N.; longitude, 76° 50′.5 or 5h 07m.4 W. of Gr.)

There were no magnetic storms recorded during the first quarter of 1931.
Air‐potential registration at the Manila Observatory, October 1927 to December 1930
Authors: Deppermann C. E.
Published: February 2008

Features of site and equipment—Registration of air‐potential at the Manila Observatory began October 1927, a Wulf bifilar electrometer adapted for registration being used until April 1928. Thereafter a remodeled Mascart quadrant‐electrometer was used. The results up to the end of 1928 were reported in a preliminary paper1 by the author in which details of site, installation, and discussion of data are given.
Abstract of the Innsbruck meeting of the Commission of Terrestrial Magnetism and Atmospheric Electricity of the International Meteorological Organization and of the resolutions adopted September 21–23, 1931
Authors: Harradon H. D.
Published: February 2008

The meeting of the Commission of Terrestrial Magnetism and Atmospheric Electricity of the International Meteorological Organization was opened September 21, 1931, at Innsbruck, Austria, under the presidency of Professor Ch. Maurain. The following countries were represented: Austria, Denmark, Finland, France, Germany, Great Britain, Holland, Poland, and Sweden.

The President's report at the opening session briefly summarized the status of the principal items of the agenda2 as follows: (1) Concerning publication of the magnetic character‐numbers. (2) Relations between the Commission and the Association of Terrestrial Magnetism and Electricity of the International Union of Geodesy and Geophysics. In this connection, the President stated that the members common to both organizations naturally served as a liaison, that there was no other interest in either case except that of science, and that the harmonious functioning of the two bodies was well illustrated by the development of the question of the Polar Year, the most important item on the agenda. (3) The various questions pertaining to the work during the Polar Year in continuation of the actions taken by the International Association at Stockholm, by the Commission at Leningrad, and by the Commission's subcommittees at London. By a detailed examination of the magnetic and electric work which is desirable and through the preparation of resolutions, the Commission could furnish a basis which would assist the Polar Year Commission in organizing the work. (4) The study of the relations of the moon and the magnetic elements on which topic Dr. la Cour was to present a memorandum by himself and Professor Chapman. (5) The question of the location of new observatories for terrestrial magnetism and electricity, with special reference to the work of the special committee to study this matter appointed at the Stockholm meeting of the International Union of Geodesy and Geophysics. The questions of the agenda were then discussed in order by the Commission during five sessions, the concluding session being held September 23, 1931.
Abstract of the Innsbruck meeting of the International Commission for the Polar Year 1932–33 of the International Meteorological Organization and of the resolutions adopted September 23–26, 1931
Authors: Harradon H. D.
Published: February 2008

The International Commission for the Polar Year 1932–33 held a called meeting at Innsbruck, Austria, September 23–26, 1931, immediately following that of the Commission of Terrestrial Magnetism and Atmospheric Electricity. The following members of the International Commission or their duly accredited representatives were present: Messrs. C. F. Brooks (representing J. A. Fleming), D. la Cour, G. van Dijk, H. Dominik, A. H. R. Goldie (representing G. C. Simpson), H. Hergesell, Th. Hesselberg (representing H. U. Sverdrup), J. Keränen, Ch. Maurain, A. W. Sololoff (representing A. F. Wangenheim), and A. Wallen. Austria, Bulgaria, France, Germany, Great Britain, Holland, Poland, and Sweden were represented by members of their national polar‐year commissions. The principal matters brought before the four sessions of the Commission were indicated in the report of President D. la Cour, an abstract of which is given below.
Wallace Morrell Hill
Authors: Hazard D. L.
Published: February 2008

Wallace Morrell Hill, magnetic observer in the U.S. Coast and Geodetic Survey for many years, died on October 18, 1931.

Mr. Hill was born at Elizabeth, N.J., on June 28, 1868. He received the degree of M.E. from Stevens Institute in 1889, and after several years devoted to teaching and writing on topics related to electrical and mechanical engineering, he entered the Coast and Geodetic Survey as a magnetic observer on March 10, 1904.
On remanent magnetism in rocks
Authors: Koenigsberger J. G.
Published: February 2008

After heating rocks in the magnetic field of the Earth to about 600°C the relative remanent magnetism Q is about 5 to 7. Q is J/KH or the quotient of remanent volume‐magnetization J at 20° in field zero by the susceptibility K times magnetic field H which produced the remanence. The remanence is impressed on the rocks during the cooling from 585°C (magnetic critical temperature of magnetite) to about 500°C. By inverting the field in this temperature‐interval the magnetization is more or less reversed. At about 480° to 500° the same field, but of opposite sign to that field which has primarily magnetized the rock, gives to the rocks a magnetization equal to zero, when measured at 20° in field zero. Not all zero‐magnetizations are equal.
Provisional sunspot‐numbers for November 1931 to February 1932
Authors: Brunner W.
Published: February 2008

(Dependent alone on observations at Zürich Observatory and its station at Arosa)
The magnetic character of the year 1931 and numerical magnetic characterization of days
Authors: Van Dijk G.
Published: February 2008

The annual review of the “Caractère magnétique de chaque jour” for 1931 has been drawn up in the same manner as for the preceding years. Forty‐nine observatories contributed to the quarterly tables; forty‐four of them sent complete data.

Table II of the annual review, containing the mean character of each day and each month, the lists of calm days and disturbed days, and the days recommended for reproduction are reprinted here.
Note on the magnetic potential at the geographic pole
Authors: Steiner L.
Published: February 2008

In the following the general formulae are developed to calculate the magnetic potential of the permanent field at the geographic pole from the horizontal components of the magnetic force on the surface—a subject in which our lamented colleague Bauer was greatly interested.

If V is the potential of the permanent field of terrestrial magnetism and X, Y, and Z are the components of magnetic force towards geographic north, east, and vertically upwards, we have

urn:x-wiley:00968013:media:tma31649:tma31649-math-0001
where u is the co‐latitude, λ the longitude, R the Earth's radius. From equations (1) the well known theorems follow: (a) If X is known at all points of the surface, Y can be determined; and (b) if Y is known at all points of the surface and X at all points of one meridian line, or more generally at all points of a line on the surface from the north to the south geographic pole, then X can also be determined at every point.
Improvements in magnetic instruments and methods adopted by the Coast and Geodetic Survey
Authors: McComb H. E.
Published: February 2008

The present systematic survey of the United States by the United States Coast and Geodetic Survey was planned and organized by the late Dr. Louis A. Bauer as Chief of the Magnetic Division of the Survey, when, under his direction, five magnetic observatories were established and a comprehensive magnetic survey of the United States and outlying possessions was initiated. When he left the Survey in 1907 the observatories were operating on a routine basis, the field‐work was well organized but there were necessarily many unsolved problems associated with different phases of the work. The solution of these problems has been going on steadily since that time and during recent years that part of the work which involves improvements in instruments and methods has been given definite consideration in the general program and progress has been accelerated. The present status of the solution of some of the more important problems and brief descriptions of a few of the improved methods are outlined below.
How the horseshoe‐formed auroral curtains can be explained by the corpuscular theory
Authors: Störmer Carl
Published: February 2008

1. The horseshoe‐formed auroral curtains—An important test of every theory of the polar aurora is that it gives a reasonable explanation of the characteristic arcs, bands, and curtains. This is possible by the corpuscular theory, developed by the late Professor Birkeland and myself many years ago, while no explanation is given by other theories. In particular, the ultraviolet theory of aurora set forth by Hulburt and Maris seems to me incapable of explaining those characteristic phenomena, where auroral rays are arranged along an arc or a band stretching across the sky many hundred kilometers long and everywhere very thin.
The cosmic‐ray observatory on the Hafelekar (2300 meters) near Innsbruck (Austria) and its first results
Authors: Hess Victor F.
Published: February 2008

In spite of the efforts of many prominent physicists from all parts of the world the main problems of the cosmic radiation which was discovered twenty years ago are still unsolved.

While some investigators analyzing the penetrating power of the cosmic rays in various absorbing materials by the use of the ionization method (Kolhoerster, Hoffmann, Steinke, Millikan, and others) and by use of the Geiger‐Mueller tube‐counter (Bothe and Kolhoerster, Rossi, L. M. Mott‐Smith, etc.) have come to very interesting conclusions as to the origin of the cosmic rays, it can be said that these conclusions are as yet by no means definitely proved and partly, at least, contradict each other.
Lettre de la part de MM. les présidents de la Commission Internationale de Magnétisme Terrestre et d'Électricité Atmosphérique, de l'Association Internationale de Magnétisme et d'Électricité Terrestres, et de la Commission Internationale de l'Année Polaire 1932–1933, qui a été envoyée à tous les observatoires magnétiques et à d'autres institutions susceptibles de pouvoir participer aux recherches magnétiques, électriques et d'aurores polaires pendant l'Année Polaire 1932–1933
Authors: Maurain Ch. , Fleming Jno. A. , La Cour D.
Published: February 2008

Monsieur le Directeur,

Etant donnée l'importance des recherches magnétiques, électriques et d'aurores polaires de l'Année Polaire 1932–1933, basées sur une collaboration étendue sur tout le Globe, nous avons l'honneur de nous adresser à vous pour solliciter la collaboration de votre Observatoire en vous demandant de bien vouloir faire de votre mieux pour contribuer au succès de cette entreprise internationale.
Sitka Magnetic Observatory October to December, 1932
Authors: Ulrich Franklin P.
Published: February 2008

There were no large magnetic storms during this quarter.

October 15–16, 1932—This was the most active storm of the quarter. The main features of this storm were the long‐period oscillations in the horizontal intensity beginning at the beginning of the storm and lasting about seven hours. The first four oscillations lasted just a little over an hour for each oscillation and the latter two lasted over one and one‐half hours, each. The first four were quite regular for H. There were long‐period irregular oscillations in the declination and vertical intensity and the entire storm was almost entirely free of the small‐range rapid oscillations. The active period lasted only about eight hours starting at the beginning of the storm and the rest of the storm after this period was only of moderate intensity.
Final relative sunspot‐numbers 1932
Authors: Brunner W.
Published: February 2008

The following Tables contain the final relative sunspot‐numbers for 1932, for the whole disc of the Sun, based on observations made at the Zurich Observatory, supplemented by series furnished by other cooperating observatories for days (indicated by asterisks) where no observations were possible at Zurich.

Table 1 gives the yearly means of the relative numbers, R, since the last minimum 1923 and of the number of days without spots.
Japanese Ursigram, January to May, 1933
Authors: Nagaoka H.
Published: February 2008

The following tables summarize the cosmic data as broadcast weekly (see this Journal, 37, 487–488, 1932) from the Tokyo Radio Station, JAN. The following designations are used to indicate magnetic conditions as determined from records made at the Kakioka Observatory: 0 = calm; 0.5 = rather calm; 1 = slight disturbance; 1.5 = disturbance; 2 = great disturbance. The groups and numbers of sunspots are as observed at the Tokyo Astronomical Observatory.

The table of Kennelly‐Heaviside Layer heights is self‐explanatory.
American URSI broadcast of cosmic data
Authors: Clarke Katharine B.
Published: February 2008

The data for terrestrial magnetism, sunspots, and auroræ are the same as given in previous tables.

The first three columns of the Table give (1) the magnetic character according to the scale 0–2 of the International Commission of Terrestrial Magnetism and Electricity, (2) the type featuring the day other than normal by letters b, p, o, and i for days marked by bay, rapid pulsations, long‐period oscillations, and irregular oscillatioris, respectively, and (3) the hour and minute of Greenwich mean time marking: the beginning of a storm, the end of the storm being indicated in the footnote to the Table. The next two columns give the data relating to sunspots: (1) the number of groups of spots and (2) the total number of spots. It is to be noted that sunspot‐numbers such as those from Zürich can be obtained from the number of groups and spots given in the Table by the formula N = k (10g+s), where k for Mount Wilson is about 0.77.
Huancayo Magnetic Observatory July to September, 1933
Authors: Cairns J. E. I.
Published: February 2008

(Latitude 12° 02.7′ S.; longitude 75° 20′.4 or 5h 01m. W. of Gr.)

There were no marked disturbances during July to September, 1933.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, October, November, and December, 1933
Authors: Nicholson Seth B. , Sternberg Elizabeth E.
Published: February 2008

In the fourth quarter of 1933 there were no magnetic storms in which the total range in H exceeded 100γ. On October 26 a group of moderate size developed rapidly 4° from the center of the solar disc. No magnetic storm occurred while this group was visible.

Two of the sunspot‐groups observed in October were in high latitudes and belonged to the new cycle. Both groups had polarities opposite to those of the waning cycle, indicating that the distribution of magnetic polarities will reverse again at this minimum.1
The relation of the Pacific eclipse of June 8, 1937, to investigations of changes of ionization of the ionosphere
Authors: Berkner L. V.
Published: February 2008

On June 8, 1937, there will be a total eclipse of the Sun of 7.1‐minute duration at noon and visible over a path starting at Santa Cruz Island in latitude 11° south and longitude 166° east at sunrise, over the Pacific Ocean in latitude 10° north and longitude 131° west at noon, and in Peru in latitude 12° south and longitude 70° west at sunset. The total time of travel from the eastern to the western extremities of the path will be roughly 3‐1/2 hours.

Exact details of this eclipse are not yet published, but the Nautical Almanac Office of the United States Naval Observatory has furnished sufficient information to determine the following approximate times, so that some idea of the relation of this eclipse to work on the ionosphere can be obtained.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, July, August, and September 1934
Authors: Nicholson Seth B. , Sternberg Elizabeth E.
Published: February 2008

No sunspots were visible and no exceptional activity was recorded by the spectroheliograph on the days of the July storms, or on the days immediately preceding them. No spectroheliograms were made on September 22, 23, and 24. A disturbed region which may have been active on the preceding days was recorded by the spectroheliograph on September 25. No spots were seen in this disturbed area until September 28, the date on which it crossed the central meridian.
Provisional sunspot‐numbers for March to May, 1935
Authors: Brunner W.
Published: February 2008

(Dependent alone on observation at Zürich Observatory and its station at Arosa)
Cheltenham Magnetic Observatory January to March, 1935
Authors: Hand Eoline R.
Published: February 2008

(Latitude 38° 44′.0 N., longitude, 75° 50′.5 or 5h 07m.4 W. of Gr.)

February 1–2—After the daily rise in D the trace gradually dropped off until 3h 30m on February 2 when there was a rather sharp decrease in westerly declination of 12′, at which level it remained substantially for about an hour when there was a sudden return almost as great as the fall and thence a gradual rise to a normal position. During the same time horizontal intensity underwent a gradual drop and at the time D took its sudden fall went up sharply about 25 gammas, held this level a half‐hour or so, and then at about 4h dropped suddenly around 50 gammas for about a half‐hour and then increased 70 or more gammas almost as suddenly as it had dropped, after which there was a gradual rise to normal.
Earth‐potential measurements made during the international polar year
Authors: Southworth G. C.
Published: February 2008

Data are presented covering the normal diurnal variation of earth‐potentials as measured at about a dozen different points, mostly in eastern United States. These data are arranged in graphical form for the convenience of the casual reader and also in numerical form for the use of the correlator. The data for Wyanet (Illinois), Houlton (Maine), and New York (New York) are based on nearly continuous recordings extending over a period of one or two years. This period includes the International Polar Year. At other points less extensive data were taken. These show the general characteristics peculiar to the location in question.

The data taken at Wyanet, Houlton, and New York have been analyzed for harmonic content. At New York the fundamental and to a large extent the harmonics also, are directed along a northwest‐southeast line. At Wyanet and Houlton these components tend to rotate with time. The pronounced directive effect noted near New York appears to prevail rather generally along the eastern part of the United States from Massachusetts to Florida and possibly into Cuba. The rotary effect noted in the Houlton and Wyanet data is also found in data taken in the southern part of the Mississippi Valley. Most of the data point toward the generally accepted view that there is a close relation between earth‐resistivity and the direction and magnitude of earth‐potentials. However, there are some inconsistencies noted which tend to make this less definite.
A conspicuous solar eruption on April 8, 1936, and simultaneous disturbances on magnetic, ionospheric, and Earth‐current records at Huancayo Magnetic Observatory
Authors: Torreson O. W. , Scott W. E. , Stanton H. E.
Published: February 2008

During observations with the spectrohelioscope at the Huancayo Magnetic Observatory April 8, 1936, there occurred the most spectacular sunspot‐eruption, from the viewpoint of extent and intensity, that had been witnessed over a period of a year of observing there.

The usual second period of observation (in accordance with the program of Commission No. 11 of the International Astronomical Union as arranged at the Paris meeting held in 1935) began at 16h 30m G.M.T., and to within a minute or two of seeing the phenomena about to be described, nothing unusual had been noticed. At 16h 45m, activity was first noticed surrounding the largest sunspot of a group of about six, located at approximately 23° north and 10° west of the central meridian. This increased in brightness until 16h 47m, reaching intensity “2,” and soon after, activity was noticed about three other smaller sunspots in the group, although rather mild in comparison with the first‐mentioned activity. Around 16h 50m the flocculus about the largest sunspot appeared to slowly decrease in size, but retained its great brilliancy. Before disappearing, the flocculus about the largest sunspot assumed the shape of a quite perfect crucifix. By 17h 03m the flocculi about all of the sunspots had returned to their original appearance.
The eccentric dipole approximating the Earth's magnetic field
Authors: Bartels J.
Published: February 2008

The magnetic dipole, situated at the Earth's geometric center O, and whose magnetic field furnishes the best approximation to the observed field of the Earth for the year 1922 has an axis aligned along the direction from a point A (near the geographic South Pole) to the antipodal point B on the Earth's surface, with B situated in latitude 78°.5 north and longitude 291°.2 east. The strength of the dipole is 8.1×1025 Gauss. cm3, yielding a maximal horizontal intensity of 0.315 Gauss at the Earth's surface.

If the observed field is to be approximated by that of a magnetic dipole not necessarily situated at the Earth's center, the best approximation (in a sense to be defined) is furnished by a dipole of the same strength as before, and with an axis parallel to AB, the dipole being situated at a point C (magnetic center) 342 km distant from the Earth's center O and in a direction towards a point C′ in latitude 6°.5 north and longitude 161°.8 east. The field of this eccentric dipole is computed by formulae similar to those given by Adolf Schmidt, expressed in tables and charts, and discussed.

The approximation of the observed Earth's magnetic field furnished by the eccentric dipole is compared with that furnished by the geometrically centered dipole (uniform magnetization) by discussing the differences, or regional anomalies. The improvement in the approximation due to the shift of the dipole from the geometric center O to the magnetic center C is hardly noticeable for the field in the Northern Hemisphere, but quite distinct in the Southern Hemisphere.
The effect of wind upon the Earth's electric field at the surface
Authors: Brown Joseph G.
Published: February 2008

The effect of wind upon the potential‐gradient has long been a subject of study and speculation. Probably the most significant fact so far observed is that stated by C. W. Allen,1 namely, that on days of continuous wind the diurnal variation of the gradient at Mount Stromlo, Australia, approaches the unitary, or world, variation observed over the oceans, while on days with calm the departure from the variation over the ocean is much greater.

In a recent paper by the author2 a method of obtaining the local diurnal‐variation by eliminating the unitary‐variation from mean curves was adopted and a theory of the local variation based upon the daily cycle of turbulence, convection, and subsidence in the atmosphere was proposed. Allen's observation is of considerable interest in connection with this theory, for if the wind blows continuously throughout the 24 hours the constant turbulence due to the wind should greatly reduce the effect of the turbulence and convection due to the heating of the surface and of the subsidence at night. On the other hand, days with calm nights and no general wind should allow these processes to take place with the greatest effect upon the gradient. To examine this result more fully, the mean local‐variations of the days of continuous wind and the days with calm at Mount Stromlo have been computed using the method referred to above. These are shown in graph A of Figure 1 along with the local variation computed from all electrically‐quiet days. It is evident from these curves that wind is an important factor in determining the amplitude and form of the local variation; it is believed that the differences here found are of the sort to be expected from a consideration of the proposed theory of the local variation.
The effect of visible solar radiation on the calculated distribution of atmospheric ozone
Authors: Wulf Oliver R. , Deming Lola S.
Published: February 2008

In the last issue of this Journal the authors have described and given the results of a theoretical calculation of the distribution of atmospheric ozone1, considering the ozone to be maintained in a photochemical steady state by solar radiation that is absorbed by oxygen and ozone. The resulting distribution resembles rather closely the actual distribution so far as it is now known from observation, and suggests that the photochemical picture is adequate to account for the major aspects of atmospheric ozone. Certain factors not taken into account in the calculation, but which are of importance for the complete picture, were briefly discussed at the end of the above‐mentioned paper. Two of these were the influence of the absorption of ozone in the visible spectrum (the Chappuis bands) and the influence of air‐movements on the amount of ozone over any particular point on the Earth's surface. It is the purpose of this and another short article, which will follow to expand upon these two points.
Auroral band at Grand Forks, North Dakota
Authors: Brooks Charles F.
Published: February 2008

The following description of what was probably an auroral band was supplied by Professor A. Russell Oliver, of the University of North Dakota, Grand Forks, North Dakota, under date of July 21, 1936: “About ten days ago about 22h 30m I noticed a well‐developed band of white light extending completely across the sky from west‐northwest to eastsoutheast and only a short distance south of zenith. It reached from horizon to horizon and was not over one degree wide. There was no flickering nor shifting and it was the only unusual phenomenon visible. There were no other light displays of any description.
Solar disturbance of May 25, 1937, accompanied by simultaneous magnetic, earth‐current, and ionospheric effects
Authors: Davies F. T. , Scott W. E. , Stanton H. E.
Published: February 2008

Solar—On May 25, from 16h 51m to 17h 05m GMT, a bright active flocculus was observed on the Sun at latitude 19° south and longitude 50° west from the central meridian.

Magnetic—The horizontal‐intensity component H increased 118 gammas between 16h 51m and 17h 01m, then decreased less rapidly to normal value by 17h 20m. The declination decreased one minute of arc during this interval and returned to normal value. The vertical‐intensity component Z increased 3 gammas and then decreased 15 gammas between 16h 52m and 17h 05m.
An improved inductor‐compass
Authors: Gunn Ross
Published: February 2008

A rugged type inductor‐compass having a period of less than a second is described. A gravitationally oriented magnet is so arranged adjacent to an inductor turning about a fixed axis that the induced potentials, due to the existence of a vertical component of the Earth's magnetic field, are neutralized. A new type of commutator particularly suitable for very low potentials and currents is described. The compass is particularly valuable for steering aircraft or small boats.