bluuebunny/crossref_metadata_2025_split huggingface dataset:
Sitka Magnetic Observatory January to March, 1935
Authors: Herschenberger John 
Published: February 2008

(Latitude 57° 03′.0 N., longitude, 135° 20′. 1 or 9h 01m.3 W. of Gr.)March 14—This storm began about 6h, with a gradual increase of about 35′ in east declination, accompanied by small increases in the other elements, and followed by similar decreases in all the elements. About 8h.5 the fluctuations became violent, characterized by small, short‐period oscillations superimposed on slow, large movements. The severest part of the storm ended about 18h, but the record continued moderately stormy for about 24 hours longer. A lesser disturbance had occurred about 20 hours before the beginning of the storm, lasting for several hours. The ranges were: Declination, 99′; horizontal intensity, 786 gammas; vertical intensity, 528 gammas.
List of recent publications
Authors: Harradon H. D. 
Published: February 2008

(Latitude 30° 18′.1 S., longitude, 115° 52′.6 or 7h 43m.5 E. of Gr.)October 24, 1934—This small disturbance began with a sudden commencement at 1h 02m, G. M. T., the horizontal intensity showing a decrease of 5 gammas in two minutes. The declination changed 0′.7 westerly, while the commencement was not well marked in vertical intensity.
On the origin of the space‐charge in the atmosphere
Authors: Hansen W. W. 
Published: February 2008

The purposes of the present note are to point out some of the errors in a paper by F. J. W. Whipple1 and to discuss qualitatively the space‐charge near the Earth's surface. This latter problem has been solved more exactly by W. F. G. Swann,2 E. R. von Schweidler,3 and others and the discussion to follow adds nothing essentially new to their results but is perhaps of interest because the main results are obtained by extremely simple considerations.As Whipple says, the current at the surface of the Earth is carried entirely by positive ions. This is because the negative ions are removed by the field and none comes from the Earth to replace them. Thus a positive space‐charge exists at the surface of the Earth; and this conclusion holds irrespective of whether there is any diffusion or not. In fact if i is the air‐earth current, F is the field strength (normally positive), and w is the mobility of the positive ions, the space‐charge will be +(i/Fw); also dF/dx = +(4πi/Fw). These conclusions depend on the assumptions that all the current at the ground is carried by positive ions, that at x = 0 there is no space‐charge except that of the positive ions, that Poisson's equation holds, and that a steady state has been reached. Now Whipple's equations [either (9) or (11)] indicate that the space‐charge at the surface depends on his diffusion constant k, in fact, if k = 0 they lead to an infinite value for the space‐charge. The cause of this trouble is that Whipple's equation (2) is incorrect as is seen if we make k approach zero when it leads toi = (λ1+λ2) F which, as Wrhipple states, is incorrect at the Earth's surface. Thus Whipple's statement, “The accumulation of positive electricity near the ground on account of the interplay of conduction and diffusion is known as the electrode‐effect,” is entirely misleading. There is a positive space‐charge at the ground because the field carries the negative ions away and the conclusion is independent of whether there is or is not diffusion.
Summary of the year's work, Department of Terrestrial Magnetism, Carnegie Institution of Washington
Authors: Fleming J. A. 
Published: February 2008

The activities of the Department of Terrestrial Magnetism during the report‐year July 1, 1934, to June 30, 1935, may be grouped under the following general divisions: (1) Reduction and study of accumulated observational data; (2) further development of technique and apparatus to record photographically the electrical conditions and variations in the ionosphere, and their investigation and correlation with other geophysical phenomena; (3) continued theoretical formulation and experimental investigation, in the laboratory, of basic aspects of nuclear physics and magnetism; (4) maintenance of observational program in the field to make for continuity of secular‐variation data and of recording at observatories of the Department the seasonal, diurnal, and irregular changes in the Earth's magnetic and electric fields.As in past years, every opportunity has been taken to encourage and to cooperate with organizations everywhere engaged in geophysical research similar to that of the Department. This is in accord with the growing efforts toward world‐wide coordination sponsored by various international scientific bodies and congresses. Such coordination with studied and planned unification of methods and aims in attack is peculiarly necessary for advance in terrestrial magnetism and electricity.
Der zustand des netzes der magnetischen observatorien der U. d. S. S. R. und weitere perspektive seiner entwickelung
Authors: Rose N. 
Published: February 2008

Bis 1917 zählte man auf dem Territorium der U. d. S. S. R. nur sechs magnetische Observatorien: Pavlovsk, Ekaterinburg, Sui (Irkutsk), Karsani (Tiflis), Kazan, und Odessa, wovon die letzteren zwei nur einige Jahre und zwar mit Unterbrechung arbeiteten; mit dem Beginn des Krieges 1914 hörte ihre Existenz auf.Nach der Revolution, besonders in den letzten fünf Jahren, beginnt eine rasche Entwickelung des Observatoriumnetzes und zur jetzigen Zeit zählen wir dreizehn funktionierende Observatorien und ausserdem fünf im Zustande der Uebertragung oder der Reorganisation. Beifolgende Tabelle gibt erschöpfende Auskunft über die Lage der Observatorien und die Dauer ihrer Arbeit.
The problem of Dirichlet for an ellipsoid
Authors: Sokolnikoff I. S. , Sokolnikoff E. S. 
Published: February 2008

(1) Introduction—In a group of important problems in potential theory it is required to determine a harmonic function which takes on preassigned continuous values on the boundaries of some region R. Under the proper limitations on the geometrical characteristics of the region R, it is known that the solution of the problem of Dirichlet exists and is unique, but the actual task of determining such a function often presents enormous analytical difficulties even for relatively simple geometrical configurations.An important type of Dirichlet's problem appears in a number of investigations in electrodynamics and geophysics, where the boundaries of the region are conductors and the boundary‐values assumed by the harmonic functions are constants. Recently C. M. Rigby1 determined the electrical field produced by a distribution of charge in equilibrium on a conducting sphere lying midway between two parallel conducting planes at zero‐potential. The present paper treats of a more general problem in which the sphere is replaced by either an oblate or prolate ellipsoid of revolution, and thus enables one to calculate the field due to a charged circular disc and thin rod lying between the infinite parallel earthed planes.
Coulomb wave‐functions
Authors: Yost F. L. , Wheeler John A. , Breit G. 
Published: February 2008

It is well known that magnetism is closely related to the fundamental problems of physics and that even ferromagnetism cannot be understood without a rather thorough study of atomic phenomena. Nuclear studies are throwing a new and deeper light into the constitution of matter and one may hope that through a study of nuclear phenomena a proper understanding of magnetism and electricty will be reached.One of the ways of learning the nature of nuclear binding‐forces consists in studying the rate of reactions caused by the bombardment of nuclei with charged projectiles such as protons, deuterons, and alpha particles. In order to interpret the experimental results in terms of nuclear binding‐forces it is necessary to take into account rather accurately the effect of the Coulombian repulsion between the nucleus and the incident projectile. It is usual to treat this part of the problem by approximate methods which may at times lead to misleading results because the effect of the Coulombian repulsion is large and a small error in its estimate may lead to a considerable error in conclusions about the nuclear structure. The object of the computations presented below is to remove these uncertainties and to provide accurate values for the wave‐functions which enter the calculations.
Apia Observatory July to September, 1935
Authors: Baird H. F. 
Published: February 2008

July 7–10—A magnetic disturbance commenced with a sudden rise in H of 16 gammas at 21h 07m July 7, to reach a value of 35051 gammas. After oscillating about this value the trace began to descend from about 5h 00m July 8 and reached a minimum of 34910 gammas at about 10h 10m July 8. The trace then rose slowly and continued more or less disturbed until July 10.July 19–20—The H‐trace was slightly disturbed from early July 19 until July 20.
On small local rapidly periodic magnetic fluctations
Authors: Menaw Fares 
Published: February 2008

Among the interesting minor phenomena of the Earth's magnetic field are the small periodic fluctuations, having periods ranging from a few seconds to several minutes, that are occasionally observed. The late Bruno Rolf1 showed that these fluctuations are at times fairly local.A detailed examination of these fluctuations in the three field‐components for a number of observatories spread over the affected area would show whether the fluctuations originate above or below the Earth's surface. It seems most likely that their origin is external, though if so there will in addition be a secondary internal field due to currents induced within the Earth.
Intended substitution of the practical absolute system of electrical units for the existing international system
Authors: Kennelly A. E. 
Published: February 2008

(1) In accordance with the authority and responsibility placed upon it by the General Conference of Weights and Measures in 1933, the International Committee of Weights and Measures has decided that the actual substitution of the absolute system of electrical units for the international system shall take place on January 1, 1940.(2) In collaboration with the national physical laboratories, the Committee is actively engaged in establishing the ratios between the international units and the corresponding practical absolute units.
An attempt to simplify magnetic charts
Authors: Ljungdahl Gustaf S. 
Published: February 2008

Everyone who uses magnetic maps of the conventional type, where the magnetic elements are indicated by isomagnetic lines, may often meet difficulties in deciding how far the lines are sufficiently ascertained by observations, or merely obtained by interpolation, especially in incompletely surveyed or magnetically disturbed regions. The appreciation of the reliability of a map may, therefore, at times, be difficult without supplementary aid of tables containing the observational material, or of figures on the map, showing the corresponding values.Figures are not perspicuous in the same degree as curves, and often encumber the form of the map, especially if the scale used is small in relation to the distance between the observed stations.
Der Tägliche Gang der Kosmischen Ultrastrahlung nach Sternzeit
Authors: Illing Wolfram 
Published: February 2008

The existence of a regular diurnal variation of the cosmic‐ray ionization according to sidereal time—as postulated by A. H. Compton's theory of the extragalactic origin of the cosmic radiation—was tested by analyzing the registrations of the Cosmic‐Ray Observatory on the Hafelekar (7,000 feet above sea‐level) near Innsbruck, Austria, covering a period of three years with 21,000 hourly observations.The triennial average‐curve giving the daily variations according to sidereal time as observed with the apparatus screened on all sides with lead (thickness 10 cm) is rather similar to Compton's theoretical curve while the observations with the apparatus unscreened from above give a different curve with two maxima at 8:30 and 19:30 sidereal time. The amplitude of the experimental curves (average of three years) is ≠0.03 per cent, somewhat less than the theoretical one (≠0.05 per cent) and much smaller than the amplitude of the daily solar‐variation (≠0.20 per cent). The observed variations according to sidereal time are of the same order of magnitude as the mean errors calculated for each point of the curve.Although the general resemblance of the experimental and the theoretical curves seems to be an argument for the validity of Compton's theory, it must be kept in mind that an additional reduction of the experimental values on account of a slight relation between outdoor temperature and ionization might alter the appearance of the curve considerably as it was found by tentative corrections.Final conclusions must be postponed until the correlation between outdoor temperature and observed ionization is more thoroughly investigated.
Huancayo Magnetic Observatory January to March, 1936
Authors: Torreson O. W. 
Published: February 2008

(Latitude 12° 02′.7 S., longitude 75° 20′.4 or 5h01m.4 W. of Gr.)January 24–25—This minor disturbance was conspicuous for its sudden commencement and for a very great decline inH directly following the commencement. At 16h 45m there was a sudden commencement in all three elements,H increasing 50 gammas in eight minutes andD andZ in the same interval increasing respectively two minutes and one gamma. At 16h 53m, immediately following the increase associated with the sudden commencement, there began a long steady decline inH which ended at 20h 38m after a decrease of 368 gammas. The value ofH at 16h 53m (approximately 29,800 gammas) was the maximum for the day and that at 20h 38m the minimum. Following the minimum,H gradually increased to normal value by 5h on January 25, there being minor fluctuations superposed on the general trend.D andZ, during the interval in question, showed numerous minor perturbations superposed on the usual diurnal trend. Throughout January 25 and 26 all three elements showed marked fluctuations without departing greatly from the usual diurnal curves.
Cheltenham Magnetic Observatory April to June, 1936
Authors: Ludy Albert K. 
Published: February 2008

(Latitude 38° 44′.0 N., longitude 76° 50′.5 or 5h 07m.4 W. of Gr.)April 17‐24—A period of disturbance, prolonged but not of great amplitude, began at 18h GMT April 17 and extended to the end of April 23. It had two outstanding features, (a) a bay lasting about an hour beginning April 18 about 5h when the declination increased 44′, the horizontal intensity 105 gammas, and the vertical intensity 116 gammas; (b) a time of short‐period fluctuations in declination and horizontal intensity lasting about thirty hours on April 21 and 22.
The magnetic character of the year 1935 and the numerical magnetic character of days 1935
Authors: van Dijk G. 
Published: February 2008

The annual review of the “Caractère magnétique de chaque jour” for 1935 has been drawn up in the same manner as for the preceding year1. Fifty‐one observatories contributed to the quarterly tables; forty‐seven of them sent complete data.Table 1 (reproduced from Table II of the annual review) contains the mean character of each day for each month. The lists of calm days and disturbed clays, and the days recommended for reproduction are also reprinted here as Table 2.
Alfred Nippoldt, 1874–1936
Authors: Bock R. 
Published: February 2008

Am 4. Oktober 1936 verschied plötzlich nach kurzer Krankheit der Direktor des Magnetischen Observatoriums der Universität Berlin, Prof. Dr. Alfred Nippoldt.Noch wohlgemut hatte er die Reise nach Edinbourgh angetreten, um bei der Tagung der Union géodésique et géophysique internationale die deutsche erdmagnetische Forschung zu vertreten. Aber ein plötzlich auftretendes inneres Leiden zwang ihn, in London Heilung zu suchen und die Reise abzubrechen. Nach wenigen Tagen raffte er sich zur Rückreise in die Heimat auf. Die eingetretene Besserung war jedoch trügerisch, und nur zehn Tage liess ihn das unerbittliche Geschick freudvoll in seinem Heim auf Genesung hoffen.
Huancayo Magnetic Observatory November to December, 1936
Authors: Davies Frank T. 
Published: February 2008

(Latitude 12° 02′.7 S., longitude 75° 20′.4 or 5h 01m.4 W. of Gr.)November 2—This was a very brief disturbance with sudden commencement in all three elements. After 14h 20m GMT, H increased seven gammas in one minute, decreased 18 gammas in two minutes, increased 127 gammas in three minutes, and decreased 60 gammas to normal value at 14h 32m. After 14h 22m D decreased 1′ in two minutes, increased 3′ in three minutes, and decreased 2′ in five minutes to normal value at 14h 32m. After 14h 22m Z increased six gammas in four minutes and then decreased eight gammas in four minutes to normal value at 14h 32m. Prior to and following this 12‐minute interval of disturbance the magnetic records were undisturbed.
Watheroo Magnetic Observatory October to December, 1936
Authors: Green J. W. 
Published: February 2008

(Latitude 30° 19′.1 S., longitude 115° 52′.6 or 7h 43m.5 E. of Gr.)October 9–10—A minor disturbance was ushered in by a sudden commencement at 7h 26m 50s GMT, October 9, as shown by the record from the vertical‐intensity inductometer. Westerly D decreased 4′ in seven minutes, H increased 16 gammas in six minutes, and the numerical value of Z decreased 7 gammas in six minutes. The period of slightly disturbed magnetic conditions continued until 16h, October 10.
The electric current‐systems of magnetic storms
Authors: Goldie A. H. R. 
Published: February 2008

In “Terrestrial Magnetism and Atmospheric Electricity,” Volume 40, No. 4 (December 1935), in a paper under the above title, Professor S. Chapman refers to some work on the same subject by the present writer. Besides replying to certain questions raised by Professor Chapman the writer would like to comment on features of interest and special difficulty.(1) On page 365 Chapman notes that though his own results and mine are in general agreement and point to maximum currents of the same order, the values given by me for ten of the greatest storms of the year 1926 are about twice as great as those derivable from the storms dealt with in his paper No. 1. Later he remarks that if these ten storms were on the average twice as great as those dealt with in his paper, the difference in results would be natural.
Our knowledge of the lunar‐diurnal variation of the magnetic declination and new results obtained from observations at Mogadiscio
Authors: Bossolasco M. , Egedal J. 
Published: February 2008

The opinion that the magnetic diurnal variations also depend on the magnetic elements in the place where they have been recorded, has been set forth by Ad. Schmidt; thereafter the question has been treated occasionally, most recently in a paper by A. G. McNishFor this question the magnetic observations made during the Polar Year at Mogadiscio are of special interest because the magnetic observatory there lay in the northern geographic but in the southern magnetic hemisphere, in other words, the Observatory lay between the geographic and the magnetic equators.
American URSI broadcasts of cosmic data, January to March, 1937
Authors: Ennis C. C. 
Published: February 2008

The data for terrestrial magnetism, sunspots, and solar constant 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 Atmospheric 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 the mean value of k for Mount Wilson was 0.53 during 1936.
Auroral display of April 26, 1937, at Burlington, Vermont
Authors: Butterfield Arthur D. 
Published: February 2008

The auroral display of April 26, 1937, was first noticed by a former student of mine, A. A. Hutchins, now living at Essex Junction, Vermont. At 22h 10m (75° meridian mean time) he happened to go outside his house and the peculiar appearance of the sky almost actually frightened him. The following is quoted from his description:“I felt that I was inside a conical tent the top of which was just a little south of the zenith and from all around the horizon in a complete circle there were streamers ascending to the zenith. At first the color was like silvery white, then suddenly changed to a dark red for just a moment, and later to a greenish blue. At times the intensity would diminish a little on one side and then come in with greater intensity.”
Suggested magnetic nomenclature
Authors: Weinberg Boris 
Published: February 2008

The introduction of the concept and the term “isopor” has so greatly increased the interest in studies of the secular variation of the geomagnetic elements that the time seems ripe to expand this concept. Therefore, I venture to propose designating the isopor of D, I, H, Z, etc., by “isallogons,” “isalloclins,” “isallodynams,” or specially “isallo‐H‐dynams,” “isallo‐Z‐dynams,” etc.Perhaps it would be still more expedient to adopt a general name of “E′t‐isoline” for isolines of annual variation E′t of a geomagnetic element E or of gradients E′ϕ;, E′λ, E′h along the latitude ϕ, the longitude λ, and the height h above sea‐level.
Apia Observatory January to March, 1937
Authors: Dyer W. Ralph 
Published: February 2008

(Latitude 13° 48′.4 S., longitude 171° 46′.5 or 11h 27m.1 W. of Gr.)February 2–5—A fairly intense magnetic disturbance commenced suddenly at 23h 02m GMT, February 2. The Z‐trace showed considerable fluctuations during February 3 but unfortunately records of H and D were not obtained until 20h, February 3. The H‐ and D‐traces were moderately disturbed during February 4 and 5 and gradually returned to normal.
Measurement of air‐potentials by the leak‐free and null method
Authors: Sherman K. L. 
Published: February 2008

The purpose of this paper is to report further on a leak‐free and null method of making electrostatic measurements. The method and some results obtained when applied to observations of air‐potentials have previously been given. Whereas the leak‐free feature of the method was stressed in that report, it is desired now to emphasize some of its other advantages and to describe small, convenient units designed to replace the more cumbersome apparatus assembled in the laboratory for the preliminary trials.Reports from persons who have used the method have consistently indicated that it is worth while adopting because of the ease of observation and reduction of the data even though the leak‐free feature is not used. Although the circuit is somewhat more complex than the conventional one and so requires slightly more time to prepare for an observation, the total time of a set of observations is less with this method because it saves the time required to calibrate the electrometer and to convert the electrometer‐readings to volts.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, April, May, and June, 1937
Authors: Nicholson Seth B. , Sternberg Mulders Elizabeth E. 
Published: February 2008

The magnetic storm from April 24 to 28 could be described as a series of three storms separated by quiescent periods lasting a few hours. The second active period began suddenly at 15h 47m.5, April 25, the third at 18h, April 26. During these storms two sunspot‐groups were very active. The smaller one crossed the central meridian on April 23.3 in latitude 24° north, the larger on April 24.7 in latitude 19° north.The storm of June 5 was probably caused by activity in the group which crossed the central meridian on June 4.8 in latitude 13° north.