bluuebunny/crossref_metadata_2025_split huggingface dataset:
Report on magnetic storm of July 7 and 8, 1928, as recorded at the Apia Observatory
Authors: Thomson Andrew , Westland C. J. 
Published: February 2008

(Latitude, 13° 48′.4 S.; longitude, 171° 46′, or 11h 27m.1 W. of Gr.)The horizontal‐intensity record showed a change from quiet conditions to a state of oscillation at 23h 15m, July 7, but the deflection which may be regarded as the real commencement of the storm, was at 23h 27m. The first movement of an increase of 35 gammas was followed by another four minutes later, bringing the intensity 50 gammas above the value of the starting point. At 23h 42m there was a rapid fall of 140 gammas in about six minutes, this being also the time of the first conspicuous movement in declination, which moved 2 minutes westward practically instantaneously. The total range in horizontal intensity was 540 gammas, the value being 35315 on July 8 at 1h 17m and 34775 gammas at 9h 20m. The range in declination was 12 minutes, with a minimum at 0h 30m and a maximum at 4h 20m, the absolute values being approximately 10° 23′ east and 10° 35′ east. The reserve intensity‐trace was recording most of the time between 8h and 10h, and moved in steps of 8 or 10 gammas in intervals of two minutes, more or less. While the observer was attending the instrument from 9h 45m to 10h there was an increase of 120 gammas in about 15 minutes. The degree of disturbance became less noticeable after 11h, but July 9 and 10 were both days of character 2.
The upper atmosphere
Authors: Maris H. B. 
Published: February 2008

The density calculations of the following paragraphs are based on the assumptions of diffusion as indicated by Table 3 and temperature‐distribution as shown in Figure 7. The calculations for the atmospheric conditions of summer nights are given in detail since it was considered these figures would be the most useful.The change in atmospheric pressure per centimeter can be calculated for any height Z by the equation or in words PZ+1, the pressure at altitude (Z+1), is equal to the pressure at Z minus the weight of one cubic centimeter of gas at Z. Equation (13) may be written then log PZ = log P0‐Σ0Z log [1 + (WZ/PZ)] but here W0, PC, T0, g0, and M0 represent the weight per cubic centimeter, pressure per square centimeter, temperature, acceleration due to gravity, and molecular weight of any given gas at the initial point, Z = 0, and WZ, PZ, TZ, gZ, and MZ represent the same quantities for the gas at altitude Z. In table 11, calculated values of WZ/PZ are given in column 1 and values of log (1 + WZ/PZ) in column 2 for altitudes from 0 to 100 km. The value of MZ/M0 was considered to be unity below the diffusion‐levels given in Table 4, column 4, for all gases; at these levels an abrupt change is considered to take place and for greater altitudes (MZ/M0) for a given gas is taken as the molecular weight of the given gas divided by 28.95, the molecular weight of air. The change in density is calculated separately for each gas for altitudes greater than 100 km. Table 12 gives values of W/P and log (1 + W/P) for altitudes 100, 500, and 1000 km for the condition of summer night based on the assumption of gravity‐equilibrium for each gas For these calculations (W0/P0), (T0/TZ), and (MZ/M0) are considered constants ; the only variable term in the value of (WZ/PZ).is therefore (gZ/g0), which maybe replaced by (r02/rZ2) where r0 and rZ are distances from the center of the Earth at sea‐level and at the height Z, respectively. The change in (WZ/PZ) is then very nearly linear for these altitudes.
Mesures magnétiques pendant l' eclipse de Soleil du 29 avril 1930 à Lu‐Kia‐Pang
Authors: De Moidrey J. 
Published: February 2008

Nous envoyons copie de nos photogrammes pendant la dernière éclipse de Soleil qui a eu lieu, en temps de la côte de Chine, le 29 avril 1930.On a reproduit d'une part le jour de l'éclipsé et d'autre part la veille et le lendemain à la même heure.
Bericht über die Versuchsfahrt des bidlingmaier'schen Doppelkompasses mit dem Luftschiff Graf Zeppelin
Authors: Grotewahl M. 
Published: February 2008

Durch das grosse Entgegenkommen des Luftschiffbaus Zeppelin wurde die Möglichkeit zur Aufstellung einer Versuchsreihe mit dem Doppelkompass während der Spanienfahrt vom 15.4.1930 14:10 Uhr bis 17.4.1930 19 Uhr M. E. Z. gegeben. Der Weg des Schiffes, der Ort, und die während der Messung zurückgelegte Strecke über Grund ist aus beiliegender Karte zu ersehen.Die Ergebnisse (s. Tabelle) sind folgende: Von 15 Messungen lagen. 11 innerhalb der geforderten Genauigkeit von 100 γ, die übrigen 4 wiesen gegen die tatsächliche Horizontalintensität eine Differenz von 320 γ (1. Messung), 180 γ (3. Messung), 130 γ (4. Messung), und 110 γ (7. Messung) auf. Es ist hierbei jedoch zu berücksichtigen, dass es sich um eine erste Probefahrt mit dem Gerät handelt ohne die Möglichkeit, die Rosenabstände damals einwandfrei zu fixieren, und zum Teil über Gebieten, in denen H noch unbekannt ist und nur durch Schätzen festgelegt wurde (Biskaya, Portugal).
Diurnal variation of concentration of condensation‐nuclei and of certain atmospheric‐electric elements at Washington, D.C.
Authors: Wait G. R. 
Published: February 2008

Diurnal‐variation observations of the concentration of condensation‐nuclei in the atmosphere and of certain meteorological elements have been made simultaneously with those of the potential gradient and of the electric conductivity of the atmosphere. The diurnal‐variation curve for condensation‐nuclei is similar to the general temperature‐curve in that high values occur during the daylight hours and low values during the night. The curve is somewhat similar to that for the potential gradient and in a very general way inverse to that for the atmospheric conductivity. The rate of ionization calculated from the linear recombination‐law, shows a diurnal‐variation curve very similar to that for the negative air‐earth current as computed from the potential gradient and the negative conductivity.The results of this investigation suggest that relative humidity is not a large factor in determining the number of nuclei present in the atmosphere. Calculated values of negative conductivity by means of both the linear recombination‐law and the square‐root law show fair agreement with the observed values of the conductivity—neither shows any decided advantage over the other.Several mechanisms whereby the diurnal variation of potential gradient at Washington may be accounted for through the observed number of condensation‐nuclei, charged or uncharged, are considered, in view of the known universal character of the diurnal variation of the potential gradient, it was considered necessary to explain only a portion of the diurnal variation through some such mechanism. On the basis of experimental results it is shown that this portion may be entirely accounted for through variation in height and in density of a local space‐charge. The necessary variation in height can be satisfactorily explained through the action of local convection‐currents in the atmosphere while the required variation in density can be explained through a variation in the number of condensation‐nuclei.Evidence is presented in support of a theory that the secondary minimum in the potential‐gradient diurnal‐variation curve, occurring at many land stations during the warmest time of the day, is produced through the mechanism of convection‐currents in the atmosphere.
An apparatus for registration of the aurora borealis
Authors: Harang Leiv 
Published: February 2008

In statistical treatments of the aurorae, visual observations usually have been used. During the winter 1930–31 an objective registration of the aurora borealis at the Observatory of Aurora Borealis in Tromsö has been tried, using an apparatus described below.The registering‐apparatus consists of a small spectrograph of very high light power, and a movable plate‐holder which is displaced 3.2 mm automatically every hour.
Distribution of magnetic elements and of their annual changes in the vicinity of the magnetic poles
Authors: Weinberg Boris P. 
Published: February 2008

A certain picture referring to the distribution of magnetic elements and, particularly, to their annual changes in the vicinity of the magnetic poles can greatly reduce the difficulties in tracing the corresponding isolines, the poles being peculiar points and therefore capable to provide useful indications.Owing to the meagerness of the number of observations not only around the south, but also around the north magnetic pole, it is interesting to make an attempt to form an idea on the distribution of magnetic isolines and especially of magnetic isopors on the basis of theoretical considerations.
Distribution of magnetic observatories and secular‐variation stations
Authors: Fleming J. A. 
Published: February 2008

In terrestrial magnetism and electricity, as in most physical sciences, coordination of data and experiment must pave the way for the development and test of theory—a coordination which Bauer so consistently emphasized and which was so materially forwarded through his efforts during the many fruitful years he directed the scientific research of the Department of Terrestrial Magnetism of the Carnegie Institution of Washington. The problems presented are extremely complex and so interrelated with other physical, geophysical, and cosmical ones that they offer great resistance to attack; their solutions, therefore, call in marked and exceptional degree for international cooperative endeavor. Herein appears to lie the most promising hope of ultimate successful interpretation, in whole or in part, of the many complexities and variations shown by these fields of the Earth and of its atmosphere.In the collection of data through the magnetic survey of the Earth, paramount attention must be given to the geographical and space‐distributions and to the time‐variability characterizing the phenomena concerned. Such work must include not only isolated observations on land and sea to determine the geographic distribution and long‐period variations but also continuous work at fixed observatories to follow the time‐variations simultaneously with coordinated observations in the physical laboratory and in astrophysical observatories.
Die Magnetisierung der Erde nach der geomagnetischen Konstanten der Observatorien
Authors: Nippoldt Von A. 
Published: February 2008

Louis Agricola Bauer hat im Jahre 1914 eine neue Grösse in die erdmagnetische Forschung eingeführt, die “Lokale Geomagnetische Konstante.” Er benutzte sie in der Hauptsache, um aus ihren Variationen in der Zeit den Zusammenhang erdmagnetischer Veränderungen mit der Sonnentätigkeit zu prüfen. In folgenden Zeilen soll dargetan werden, dass diese Grösse auch geeignet ist, um etwas über die räumliche Verteilung der Magnetisierung der Erde auszusagen.Die Anzahl der erdmagnetischen Observatorien ist zu einer genügend ausreichenden Erledigung der verschiedenen Fragen, allerdings noch nicht gross genug; es sind daher längst Rechnungen in grösserem Umfang eingeleitet worden, über die dann später noch einmal im Zusammenhang zu berichten ist. Aber die besondere Bedeutung der Observatorien als das feste Gerüst für alle magnetischen Vermessungen macht eine nur für sie durchgeführte Studie doch wertvoll genug, um sie hier bekannt zu geben.
The distribution of mass in marine compasses
Authors: Peters W. J. 
Published: February 2008

This preliminary note was prepared for the memorial number of the JOURNAL to show one phase of the investigation of compass‐deviations caused by the rolling motion of ships, which seems suitable for this number because of its bearing on the making of magnetic observations of the highest precision at sea—a field which the Carnegie Institution of Washington in its Department of Terrestrial Magnetism under the direction of Bauer did so much to advance.The distribution of mass in the designing of marine compasses with object of equalizing the moments of inertia about horizontal axes of the card was considered in the earliest investigations of the deviations of the compass. It was found that “if two needles are placed parallel with their ends 30° on each side of the diameter and therefore 60° from each other, there will be no sextantal deviations... . These deviations will also disappear if two pairs of parallel needles are placed symmetrically on each of the diameter, one pair at 15° and the other at 45° from the diameter... . These results suppose the magnetism of the needles to be collected in one point at each extremity; but as the points in which the magnetism may with least error be considered as collected lie a short distance from the extremities, the consequence is ... that the sextantal and octantal errors are slightly over‐corrected; and the accuracy of the correction might doubtless be increased with little or no injury to the performance of the compass in other respects, by bringing the needles a little within the regulated distances of 30° and 60°.”
Earthquakes recorded by magnetograph
Authors: Hazard Daniel L. 
Published: February 2008

The illustration shown herewith is a copy of a portion of a magnetogram from the magnetic observatory of the Coast and Geodetic Survey at Cheltenham, Md., giving a record of the Mexican earthquake of June 3, 1932. The record of the horizontal intensity variometer in the center, is particularly sharp and shows the preliminary phases, the long waves, and several after shocks. Because of the slow rotation of the drum (20 mm per hour) accurate timing of the phases is impossible, but the measured time of beginning differs by only a fraction of a minute from the time given by the seismograph at Georgetown University.It is interesting to note in this connection that the seismological work of the Coast and Geodetic Survey was started in 1903 by Bauer, at that time in charge of the magnetic work of the bureau, in order to compare the earthquake records of magnetographs and seismographs and determine whether or not the movement of the magnets was entirely mechanical.
Sitka Magnetic Observatory April to June 1932
Authors: Ulrich Franklin P. 
Published: February 2008

(Latitude 57° 03′.0 N.; longitude, 135° 20′.1 or 9h 01m.3 W. of Gr.)April 1–2, 1932—This was a small magnetic storm. There were sharp bays in all curves of the gram with an increase in value of all elements just before the third hour on April 2. This was followed by a calm, normal period until 6h 30m and from then until the end of the storm there were irregular bays of moderate intensity. For an hour centering just before the 13th hour the curves show small rapid oscillations.
Japanese URSIgram
Authors: Nagaoka H. 
Published: February 2008

In cooperation with the Naval Experimental and Research Establishment, the Central Meteorological Observatory of Japan, the Tokyo Astronomical Observatory, and the Department of Communications, the Japanese National Committee of URSI has arranged to collect the data for the use of the Ursigram and broadcast it from the Tokyo Radio Station, JAN.Transmission schedule of the Ursigram—The Ursigram in code described below is transmitted weekly, on Saturdays at 13h G.M.T. on frequency 11980 kc/s beginning September 8, 1932.
North Atlantic radio transmission‐conditions for long‐wave daylight signals for the years 1931 and 1932
Authors: Briggs L. J. 
Published: February 2008

The following tables represent daylight transmission‐conditions between Europe and the northeastern United States for wavelengths between 10,000 and 20,000 m (15–30 kc). These are derived from signal intensity measurements made in Washington on a number of long‐wave European transmitting‐stations averaged according to a method described by L. W. Austin in the Proceedings of the Institute of Radio Engineers (19,1615,1931). The measurements in Washington are made at such times that daylight conditions exist over the whole of each of the signal‐paths.The errors of the averaged values of signal field‐intensity as given in the tables are estimated not to exceed ±10 per cent. These tables were prepared by L. W. Austin and since his death by E. B. Judson, who has taken most of the field‐strength observations; S. E. Reymer performed the necessary calculations.
The energy acquired by a Dirac isolated magnetic pole in a magnetic field
Authors: Tuve M. A. 
Published: February 2008

The large value of the energy which would be acquired by a one‐quantum Dirac isolated magnetic pole in a quite ordinary magnetic field appears to have escaped general attention. This energy is of a sufficiently striking magnitude to stimulate experimentalists to search for evidence of the existence of this new entity, and possibly to encourage calculations as to the interactions of a high‐speed isolated pole with electrons and other particles and with radiation, much needed to guide the experiments.1Dirac2 calculates the “magnetic charge” or pole‐strength of a one‐quantum pole to be 3.28×10−8 electromagnetic unit. Hence the kinetic energy acquired by such a unit pole in falling one centimeter in a field of one gauss is 3.28×10−8 ergs. This is an energy of 20,600 electron‐volts. If isolated Dirac poles exist in Nature, a mechanism for the production of single particles of extremely great energy is at once obvious. Thus, if they could be introduced at one end of a solenoid producing a field of 200 gauss (159 ampere‐turns per cm), the Dirac poles would each acquire 20,600×200×100=4.1×108 electron‐volts energy in traveling only one meter inside this solenoid. Hence the possibility of producing highspeed particles (probably including all types of primary particles and quanta, by recoil and by secondary processes) having energies exceeding even cosmic‐ray energies (1010 electron‐volts) is immediately at hand if the Dirac poles exist and can be isolated in the laboratory. Incidentally, as my colleague Mr. McNish pointed out when I first mentioned these computations, multiple acceleration in a re‐entrant solenoid would be possible (the magnetic field of a current is not derivable from a potential), although rather large electric fields evidently would be required to produce the desired near‐circular paths.
Cheltenham Magnetic Observatory April to September, 1933
Authors: Hartnell Geo. 
Published: February 2008

(Latitude 38° 44′.0 N.; longitude 76° 50′.5 or 5h 07m.4 W. of Gr.)The only marked disturbance recorded during April to September, 1933, was that beginning September 9 at 4h 22m and ending September 10 about 7h Greenwich mean time. The ranges were 43′.6 in D, 151γ in H, and 222γ in Z.
American URSI broadcasts of cosmic data
Authors: Ennis C. C. 
Published: February 2008

The data for terrestrial magnetism, sunspots, solar constant, 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 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.
On the origin and maintenance of the Sun's electric field
Authors: Gunn Ross 
Published: February 2008

The systematic motion of the Sun's conducting atmosphere across its own magnetic field is shown to modify greatly the effective electrical conductivity of the region. The velocity of the superposed mass‐motion of the atmosphere due to the impressed crossed electric and magnetic fields is found to be E/B to a very good approximation. It is shown that the processes of ionization and recombination of ions and electrons subject simultaneously to impressed electric and magnetic fields result in a systematic migration of the ions. The greater probability of electrons recombining when they possess a minimum of energy results in a transport of charge in a direction opposite to the motion imposed by electrical conduction. The magnitude of this systematic motion in the Sun is adequate to replenish the Sun's electric charge and hence maintain a steady electric field.Electrical equilibrium in the reversing layer is determined by “three‐body” recombinations and the electronic conductivity, whereas equilibrium in the chromosphere is determined by “two‐body” recombinations and the ionic conductivity. The latter equilibrium is of such a type that high effective electron‐temperatures must exist in the chromosphere and this is adequate to explain both the presence of certain solar bright‐line spectra such as the ionized helium line λ 4868 and the observed chromospheric pressure‐gradients. The estimated effective temperature of the chromospheric ions approximates 26,000°.The superposed atmospheric velocity and electric fields calculated from the present theoretical considerations agree in magnitude, direction, and distribution with those deduced in earlier papers from observational data regarding the anomalous solar rotation [Phys. Rev., 35, 635–642 (1930), and 36, 1251–1256 (1930)].
Celebration of the completion of one‐third century of continuous operation at the Cheltenham Magnetic Observatory
Authors: Heck N. H. 
Published: February 2008

A milestone in the progress of investigation of terrestrial magnetism in the United States was reached with the completion of a third of a century or three sunspot‐cycles of continuous operation at the Cheltenham Magnetic Observatory at Cheltenham, Maryland, about 14 miles from Washington. The occasion was celebrated October 10, 1934, at the Observatory by addresses, demonstrations of field‐ and observatory‐work and exhibits. The latter covered the entire range of activity and also collection of all types of compasses used on sea, on land, and in the air, and views of the various vessels of the United States Coast and Geodetic Survey which took part in the development of magnetic work at sea of the United States out of which grew the well‐known ocean‐surveys by the Department of Terrestrial Magnetism, Carnegie Institution of Washington.The guests—175 in number—were from the Coast and Geodetic Survey, the Department of Terrestrial Magnetism of the Carnegie Institution of Washington, the National Bureau of Standards, and the Naval Research Laboratory. There were three guests of honor, Dr. John A. Fleming, Acting Director, Department of Terrestrial Magnetism of the Carnegie Institution of Washington and Editor of the Journal, Dr. J. Bartels, Professor of Geophysics at the University of Berlin and Professor of Physics at the Forstliche Hochschule in Eberswalde, Germany, and Research Associate of the Carnegie Institution of Washington, and Mr. Daniel L. Hazard, Senior Mathematician and Chief Magnetician of the Coast and Geodetic Survey.
Ole Krogness and his work
Authors: Vegard L. 
Published: February 2008

The premature death of Professor O. Krogness will be greatly regretted, not only by his family and numerous friends, but also by those who have been engaged in the study of solar and terrestrial relationships during the last twenty years.Born at Trondheim in 1886, he had reached only the age of 48. His early death is the more deplorable, as most of his activity had been devoted to the development of new institutions for research, to new observational stations, and to the collection of observational material.