bluuebunny/crossref_metadata_2025_split huggingface dataset:
On the non‐simultaneity of magnetic storms
Authors: Rodés Rev. Luis 
Published: February 2008

Dr. Bauer in a study based chiefly on data collected by Faris, reached the conclusion that “magnetic storms do not begin at precisely the same instant all over the Earth.” The abruptly beginning ones, investigated by him, appeared to progress more often towards the east than towards the west, with a velocity such that it would require, on the average, about four minutes to encircle the Earth at the equator.1I should like to call attention to the fact that in the case of five well‐defined storms which occurred subsequent to those examined by Bauer, namely, those of January, February and May, 1919, March, 1920, and May, 1921, I have found a simultaneous beginning at Tortosa and at Honolulu, which lies 158 degrees to the west, within the limits of measurement. The photographic paper at Tortosa runs at the rate of 2.8 minutes to the millimeter and the base line is shown every hour by an electric lamp in connection with the astronomical clock, hence, I do not think we can be in error by a minute. The measures for each storm were accurately made by the writer, and the corresponding times of the beginning as registered at the other stations were kindly communicated to me by Col. E. Lester Jones, director of the U. S. Coast and Geodetic Survey, at Washington, and by Capt. R. L. Faris, acting director.2
Proposed magnetic and allied observations during the total solar eclipse of September 10, 1923
Authors: Bauer Louis A. , Fleming J. A. 
Published: February 2008

Special magnetic and allied observations will be made at stations inside and outside the shadow belt of the total solar eclipse of September 10, 1923, by the Department of Terrestrial Magnetism of the Carnegie Institution of Washington, and by various co‐operating magnetic observatories, institutions, and individuals. The distribution of the magnetic observatories within the limits of the eclipse and on both sides of the belt of totality is shown by the accompanying map taken from the American Ephemeris and Nautical Almanac for 1923 and on which the positions of these observatories have been indicated.The observatories, either within or near the limits of the eclipse, are: North of the belt of totality, Sitka (Alaska), Meanook (Alberta), Tucson (Arizona), Agincourt (Ontario), Cheltenham (Maryland), and Vieques (Porto Rico) ; to the south of the belt of totality, Honolulu (Hawaii), Cuajimalpa (Mexico), and Huancayo (Peru); while just outside the limits of the eclipse, at beginning and ending, are Kakioka (Japan) and La Quiaca (Argentina). Of the observatories, that at Tucson is particularly well situated, being only about two hundred miles from the central path of the eclipse; the maximum obscuration at Tucson will be about ninety‐two per cent. It is planned that the Department of Terrestrial Magnetism will have parties at two (possibly three) stations within the belt of totality to make magnetic and atmospheric‐electric observations. The United States Coast and Geodetic Survey will have one special party for taking magnetic observations within the belt of totality in southern California and will have special observations carried out at its observatories.
The magnetic character of the year 1922
Authors: van Dijk G. 
Published: February 2008

The annual review of the “Caractère magnétique de chaque jour” for 1922 has been drawn up in the same manner as the preceeding years. Forty‐three observatories contributed to the quarterly reviews, 37 of them having sent complete data.The following table contains the mean character of each day and each month, the list of “Calm Days” and the days recommended for reproduction.
The anomalies of terrestrial magnetism and gravity in the Kursk Government, Russia
Authors: Lasareff P. 
Published: February 2008

In a preceding article,2 we have given the results of the operations carried out during 1919–1920 in connection with the work undertaken by the Commission des Forces Productives de la Russie cooperating with the Academy of Sciences, for investigating the anomalies of terrestrial magnetism and gravity in the Government of Kursk. The purpose of our note, presented at the Academy of Sciences, on May 2, 1923, was to summarize briefly the results obtained in 1921, 1922, and 1923.As already indicated in the preceding note, a zone (the northern zone) of strong anomaly, consisting of a narrow strip of 2 to 3 kilometers, extends from the northwest towards the southeast and passes through the districts of Kursk, Stschigry and Tim fer a distance of about 250 kilometers. It has a considerable maximum over an extent of 4 kilometers, the value of Z (vertical intensity) ranging from 1.6 to 1.9 gauss.
On the observations of Earth potential‐gradients at Ebro
Authors: Chapman S. , Whitehead T. T. 
Published: February 2008

1. In a recent paper1 the writers have re‐investigated the mathematical relations between the observed terrestrial magnetic variations and the external and internal (induced) magnetic fields which give rise to them. In the course of this paper we compared the diurnal variation of electric potential‐gradient within the earth, given for Berlin, in arbitrary units, by Weinstein, with that derived from the potential of the field of the diurnal magnetic variations, as previously determined by one of us.2 A moderate similarity in type was found; the question of agreement in absolute magnitude could not be tested, however, Weinstein's unit being unknown.2. The recent appearance of Dr. Bauer's discussion of the measurements of earth potential‐gradients at Ebro3 affords the opportunity for further examination of the question. It may be said at once that the results prove extremely puzzling. The observed potential‐gradients are, as in Weinstein's case, nearly of the type to be expected from the magnetic variations, but are five or six times as large in amplitude. As Dr. Bauer's tables refer to the means for groups of five magnetically quiet days, it seemed just possible that allowance for the factor 5 might have been overlooked, but on enquiry Dr. Bauer kindly confirmed our expectation that this was not the cause of the discrepancy.
Relations between the diurnal and annual variations of Earth currents, terrestrial magnetism and atmospheric electricity
Authors: Bauer Louis A. 
Published: February 2008

An investigation is made as to correlations in the diurnal and annual variations of earth‐currents, with those of terrestrial magnestism and atmospheric potential‐gradient, as based on the observations at the Ebro Observatory, Tortosa, Spain, for the magnetically‐quiet days during the five‐year period, 1914–1918.It is found that the diurnal and annual variations of the horizontal components (X towards north, and Y towards east) of terrestrial magnetism are of such a character, quantitatively and qualitatively, as to indicate that only to a certain extent may they ba the direct electromagnetic effects of the observed corresponding earth currents (W towards west, and N towards north). On the other hand there is a high probability that the observed earth‐currents may be the combined result of a varying magnetic field and a varying electric field as indicated by the rate of variation in terrestrial magnetism and atmospheric electricity, during the day and year. The correlation between the variations of earth‐currents and the rate of variation, or time‐gradients, of the atmospheric potential‐gradient is found to be even higher than that for the time‐gradients of terrestrial magnetism, both as regards the diurnal variation and the annual variation.
On the magnetic anomaly in Poland
Authors: Kalinowski St. 
Published: February 2008

When I began magnetic investigations in Polish territory in 1910, I could not be guided in any way by previous surveys, because they were mostly disconnected and not sufficiently worked out.From separate investigations conducted here and there at different times, we could only estimate with some approximation the annual changes. As a fundamental distance between observation points, I took 40 kilometers, though realizing that later on it would be necessary to diminish this; however, when it was possible (the facility of communication had to be thought of and it is to be remembered that I was doing this at the time of Russian rule), I tried to use also smaller distances, about half as large. The above explains why the distribution of my observation points is not uniform over the whole of Congress (Russian) Poland which has been examined. But, thanks to it, I may draw with still greater assurance conclusions as to the abnormal course of isomagnetic lines, and form other plans as to further investigations. Figs. 1, 2, and 3 show the observation‐points mentioned for the years 1910–1913, together with the respective values of D, H, and I, all reduced to average annual value of 1912, and so they are comparable with each other.
Values of the magnetic declination in 1924 at principal stations in the Union of the Soviet Socialist Republics
Authors: Pödder Arnold 
Published: February 2008

Because of the increasing number of requests by various institutions and persons for a magnetic declination chart for the principal stations of the Union of the Soviet Socialist Republics, the following table was compiled. The work of summarizing the material and reducing it to 1924 was assigned to me, and, thanks to N. N. Trubiatchinskii, in charge of Konstantin Magnetic Observatory at Pavlovsk, who made many valuable suggestions, I have summarized the data as accurately as the scientific material at hand allowed.The latest observations of declination in Russia are given; for a few stations only, at which no new observations have been made, the magnetic map of European Russia by A. Tillo, for the epoch 1880, was used.
Concerning the computation of tabular quantities
Authors: Neumann Frank 
Published: February 2008

In the September, 1924, number of this Journal, pages 121–124, Messrs. Duvall and Ennis, of the Department of Terrestrial Magnetism, describe an interesting graphic method for computing diurnal variations from differential formulae. It is gratifying to know that the problem of simplifying magnetic observatory computations is receiving the attention it deserves for there is no doubt that the great amount of labor involved in the computation of tabular quantities is a serious problem in the preparation of many observatory reports.In considering the relative merits of various methods of computing diurnal variations, it is practically impossible to reach a wholly satisfactory decision because the personal preference and aptitude of the individual computer and the facilities available are decisive factors. This is particularly true of the addition method1 in which efficiency is almost wholly dependent upon the computer's ability to operate the computing machine. The preparation of the special tables necessary in this method is an insignificant factor, as compared with the construction of any graph.
Terrestrial Magnetism and Electricity at the Madrid meeting, October, 1924
Authors: Bauer Louis A. 
Published: February 2008

The second General Assembly of the International Geodetic and Geophysical Union met at Madrid, October 1–8, 1924, twenty‐five of the twenty‐seven countries which already adhere to the Union being represented by delegates and guests.† The total number was about one hundred and fifty.At the opening meeting on the morning of October 1, His Majesty the King of Spain presided. The address of welcome was delivered by the President of the National Committee of Spain, Señor Cubillo y Muro, and the response by the President of the Union, M. Lallemand. In the afternoon of the same day the officers of the Union and of the sections met, in order to complete arrangements for the plenary meetings of the Union and for the meetings of the various sections, of which there are now seven, namely, Geodesy, Seismology, Meteorology, Terrestrial Magnetism and Electricity, Oceanography, Vulcanology, and Scientific Hydrology. All sessions of the Union and of the Sections were held in the Chamber of Deputies.
Perturbation magnétique du 1er novembre 1924 à Lu‐kia‐pang et à Tsiing‐tao
Authors: de Moidrey J. 
Published: February 2008

Le 1er novembre dernier, jour magnétiquement très calme, en relève sur l'enregistreur de Lu‐kia‐pang une perturbation assez violente, de fort courte durée, et telle que je ne me rappelle pas en avoir vu sur nos courbes depuis 1877.Elle a un début brusque à 0h 07m, temps de Greenwich, Au déclinomètre et à la balance la forme générale est celle d'une baie profonde et peu ouverte. La durée est d'environ un quart d'heure, après lequel le tracé redevient presque aussi uni qu' auparavant.
Provisional sun‐spot numbers for January to March, 1925
Authors: Wolfer A. 
Published: February 2008

1. The foregoing article (pp. 69‐77) by Dr. Chree has particular reference to an item of the Madrid meeting of the International Section of Terrestrial Magnetism and Electricity pertaining to the application of non‐cyclic corrections in terrestial magnetism and atmospheric electricity which, owing to limited time, could not fully be discussed and regarding which no agreement was reached. Dr. Chree has concerned himself with the application of non‐cyclic corrections for a period of about two decades, but he has had few followers in the method adopted by him. It should be recalled that he has chiefly dealt with the discussion of the so‐called quiet days (limited to 5 per month in the case of terrestrial magnetism, and to 10, in atmospheric electricity).2. The mean values of results from the selected quiet days are frequently termed “normal” values, though, as a matter of fact investigations have repeatedly shown that the quiet clays are as subject to a special kind of disturbance, though to be sure to less extent, as are the greatly disturbed days. This fact is admirably shown in Father de Moidrey's timely article (pp. 79‐82). Instead of the quiet‐day values representing normal conditions they should be looked upon as representing subnormal conditions; it is as bad at times for a patient to have a sub‐normal temperature as a high temperature. On the average, about 65‐70 per cent of the five magnetically‐quiet days per month selected at the De Bilt Observatory, on the basis of characterization lists received from the operating observatories, are the days of minimum range in horizontal intensity. Sometimes it happens that a magnetic‐activity measure based on the assumption that the quiet days represent normal conditions turns out negative, and, hence, does not admit of physical interpretation. It has even occurred that the monthly mean diurnal range for the selected 5 quiet days was higher than the monthly mean diurnal range obtained from the 10 least disturbed days per month. We, accordingly, deem it safer in general, not to apply non‐cyclic corrections by Chree's method, with all the suppositions it implies, e.g., progressive linear change throughout the day, but we are quite ready to give all the information in our observatory publications which others may require for any procedure they may make themselves responsible for. Fortunately in terrestrial magnetism the “non‐cyclic” correction, as derived from differences of successive midnight values, is, in general, small, however, the case is entirely different in atmospheric electricity where the accidental or disturbing features may play a predominant part. We have repeatedly determined the Fourier coefficients from a series of diurnal‐variation observations extending over several months, or over several years, and have invariably found that the differences in the essential quantities, computed with or without application of a supposed non‐cyclic correction, are inconsequential from a physical standpoint.
A search for possible effects of atmospheric electric discharge upon the potential gradient
Authors: Dwight C. H. 
Published: February 2008

A search was conducted to determine whether there were at all times present in the atmosphere small electrical discharges, of the rapidity of lightning and perhaps continually taking place in the upper atmosphere. An apparatus was set up that would respond to rapid but not to slow fluctuations in the potential‐gradient. By photographic means as well as by direct inspection it was possible to count the number of rapid fluctuations in a given time. The possibility of any effect due to the motion of charged clouds nearby was shown to be nil.It was found that, as far as the sensitivity of the apparatus permitted, there were no variations in the gradient that could not be attributed to lightning or other known causes. If there were any rapid changes in the atmospheric potential‐gradient, they were less than about 18 volts per meter, except in the case of thunder‐storms, when some interesting phenomena were observed.
Studies concerning the relation between the activity of the Sun and of the Earth's magnetism
Authors: Bauer Louis A. , Duvall C. R. 
Published: February 2008

Partial Abstract.—The variability with sunspot activity of the quantities a and b in the formula Q = a + b S, of the Wolf type, is investigated; Q is the quantity measuring the activity of the Earth's magnetism and S, the measure of solar activity. Using annual values of Q and S, it is found that a varies directly and b inversely with sunspot activity.At first the Wolf‐Wolfer sunspot numbers, Sn, are used as measures of solar activity, but later other solar measures, sunspot areas, faculae, umbrae, flocculi, prominences, and solar‐constant values, are utilized. While the correlation coefficient, r, for a year‐to‐year comparison between various kinds of solar and of magnetic measures reaches values as high as 0.94, the comparison from month to month, or from day to day, may yield a correlation coefficient, considerably below 0.5, even after every care is taken to eliminate annual periodicities in the solar and magnetic measures.The mean measures of solar activity for magnetically quiet and magnetically disturbed days during a solar cycle may be almost identical whereas the mean values of the magnetic measures for the two sets of days are very appreciably different.None of the present measures of solar activity explain satisfactorily the various penomena of the Earth's magnetic activity on the assumption that there is a direct causal connection between sunspots and the Earth's magnetic disturbances.For further conclusions, the interested reader may be referred to page 213.
The principles of the systematic application of geophysical methods of prospecting to mining and subterranean engineering
Authors: Ambronn Richard 
Published: February 2008

Until a few years ago the research work accomplished by the geologist and the mining engineer for investigating the formations of mineral deposits in the Earth's crust—whether the object be purely or practically scientific—was confined almost exclusively to ascertaining and systematically arranging such empirical facts as could be derived by direct observation at easily accessible places on the surface of the globe, e. g., at exploring works, borings, or existing mines. The miner has been accustomed to say: “Behind the shoulder it is dark,” meaning thereby that the only facts to be taken into serious consideration as a certain basis for his technical and economic ventures and plans were those which he could observe with his own eyes. To such observations may be added all those which may be obtained by petrographic, chemical, or microscopic examinations of specimens taken from the localities in question.The greater the progress of mining technique, the greater the depth at which ore, etc., can be profitably exploited. And on the other hand, the valuable deposits which can be discovered, and evaluated, by prospecting on the surface of the Earth only, are becoming more and more exhausted, so that one is obliged more and more to exploit formations lying in lower strata. The deeper these strata, the more difficult it becomes to draw, from the geological facts ascertainable on the surface, any reliable conclusions as to the conditions prevailing at these greater depths; at the same time the costs increase proportionately for the prospecting work requiring boring, sinking of shafts, and so forth. Thus the increased depth of the deposits involves a disproportionate increase of risk, when the old methods only are employed.
Principal magnetic storms recorded at the Apia Observatory, January to March, 1926
Authors: Thomson Andrew , Westland C. J. 
Published: February 2008

(Latitude, 13° 48′.4S.; longitude, 171° 46′, or 11h 27m.1W. of Greenwich.)January 26–27, 1926.—This storm is remarkable for the large number of rapid motions up and down shown on the horizontal‐intensity magnetogram. Maxima and minima sometimes follow one another at extraordinarily short intervals. A conspicuous example of this occurs at 23h 53m, when the value changes from 35166γ to 35293γ, a rise of 127γ in 7 minutes. Then the curve immediately turns back again and returns to 35178γ, a fall of 115γ again in 7 minutes. The curve is even steeper than this at 17h 57m, where a fall of 92γ is registered in two minutes (35253γ to 35161γ), and several other instances of movements not much less rapid could be mentioned. There are two maxima and minima which are conspicuous among the extreme values recorded, namely: January 25, 16h 28m, H = 35317γ and Z = 20488γ; January 25, 18h 40m, H = 35104γ and Z = 20420γ; January 26, 0h 04m, H = 35293γ and Z = 20490γ; January 26, 1h 12m, Z = 20435γ; January 26, 2h 23m, H = 35062γ. The end of the violent disturbance is at 4h, but there is still some milder disturbance after this time.
Provisional sunspot numbers for April and May, 1926
Authors: Wolfer A. 
Published: February 2008

(Latitude 14° 35′ 48′′N.; longitude 121° 10′ or 8h 04.m 7. of Greenwich.)Besides the above, miner disturbances occurred as follows: January 18 at 9h to January 19 at 4h; January 22 at 15h 37m to January 23 at midnight; February 17 at 15h 36m to February 18 at 5h; March 5 at 10h 10m to March 6 at noon; March 9 at 5h 26m to March 10 at 8h 30m; and March 11 at 0h to March 12 at 4h 40m.
On micromagnetic oscillations of type II
Authors: Pödder Arnold 
Published: February 2008

In my article “Micromagnetic Oscillations as Observed at the Magnetic Section of the Observatory of Irkutsk (Zouy), 1925,” I considered the micromagnetic oscillations of type I, observed with the aid of the sensitive Eschenhagen magnetograph (the sensitiveness of the Lloyd's balance is 1 mm. = 1.3γ; that of the apparatus for horizontal intensity is 1 mm. = 0.34γ, and a velocity of rotation of the drum with the photographic paper is l min. = 15 mm.), and having periods from 4 to 15 seconds. As for the micromagnetic oscillations of type II, with periods averaging about 34 seconds, I calculated only the mean monthly values of the periods and the amplitudes for 1925.Examination of this data revealed some regularity of a change of periods and amplitudes, consequently I decided to treat the above‐mentioned observations in another manner, namely as Dr. W. van Bemmelen treated micromagnetic oscillations or pulsations, as he denominates them, for Batavia and Buitenzorg.
Principal magnetic storms recorded at the Huancayo Magnetic Observatory for April to June, 1926
Authors: Goddard Richard H. 
Published: February 2008

(Latitude, 13° 48′.4S.; longitude, 171° 46′, or 11h 27m.1W. of Greenwich.)April 14, 1926.—A disturbance of considerable intensity began on April 14 at 14h 02m, with a sudden commencement. The horizontal intensity increased within six minutes of time by about 110γ. High values of H occurred at intervals until 20h with large fluctuations; within the next hour the force decreased greatly, the spot going beyond the limits of registration, remaining lost, except for brief periods, until 13h on April 15. A series of large fluctuations then brought the spot back to the paper, but the value remained low until the following day, when normal conditions were gradually resumed. The sudden commencement of this storm was also shown in the D and Z traces.