bluuebunny/crossref_metadata_2025 huggingface dataset:
A vertical‐intensity magnetometer
Authors: la Cour D.
Published: February 2008

Magnetic observations, and in particular those necessary for the control of magnetograph records, at stations in high magnetic latitudes have been greatly handicapped, because of unfavorable magnetic conditions as well as temperature conditions at such stations, for lack of a suitable instrument to determine rapidly and with precision the vertical intensity of the Earth's magnetic field. The establishment of the Godhavn Magnetic Observatory in Greenland, where the magnetic inclination is about 82°, led the author to consider electrical methods of determining the magnetic vertical‐intensity of the Earth's field. An experimental apparatus was used during a trip to Greenland in 1925 to select a site for the Observatory, and as a result of these experiments a new type of vertical‐intensity magnetometer was developed and was sent in August 1926, after trial at the Rude Skov and Potsdam observatories, to the Godhavn Observatory for use there regularly.

The essential part of the new instrument is a precise standard for mutual inductance, that is, an inductor with two sets of windings, and very strongly built, By rotaiing the standard 180° on a horizontal axis the vertical intensity of the Earth's magnetic field gives rise to electromotive forces in the windings. One winding is connected with a ballistic galvanometer which, through the arrangement described below, measures the induced effect; the sensitivity of the galvanometer is such that rotating the inductor 180° would cause a deflection quite beyond the scale‐limit of the galvanometer, for example, at Rude Skov for a scale‐distance of 2 meters, a deflection of 10 meters. This arrangement, a sort of zero‐method, by which the deflection of the galvanometer never exceeds a few centimeters even for highest sensitivity of the apparatus, utilizes an accurately determined electric current which, during the turning of the inductor, may be made or broken in the second winding. The making or breaking in this current through the second winding induces an electromotive force in the winding connected with the galvanometer, and the connections are such that the electromotive force induced by the variation of the “compensating current” is opposite to the electromotive force induced by the vertical component of the Earth's magnetic field during a turn of the inductor. Thus, the resulting deflection of the galvanometer corresponds to the difference of the two induced electromotive forces. By again turning the coil and using some other compensating current, a second galvanometer reading is obtained. By means of two such readings the strength of a compensating current, which should give just the zero‐deflection of the galvanometer, is readily computed.
Provisional sunspot numbers for December, 1926 to February, 1927
Authors: Wolfer A.
Published: February 2008

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Principal magnetic storms recorded at the Sitka Magnetic Observatory, April to December, 1926
Authors: Ulrich F. P.
Published: February 2008

(Lat. 57° 03′.0 N.; long. 135° 20.′1 or 9h 01m.3 W. of Gr.)
Principal magnetic storms recorded at the Cheltenham Magnetic Observatory, October to December, 1926
Authors: Hartnell Geo.
Published: February 2008

(Lat. 38° 44′.0 N.; long. 76° 50′.5., or 5h 07m.4 W. of Gr.)
Note on declination base‐line control at the Godhavn Observatory, Greenland
Authors: la Cour D.
Published: February 2008

Dr. Olsen, in charge of the Godhavn Observatory, has sent an example to show how well the special arrangement for time‐marking in use at the Observatory for determination of base‐line value of one of the declination variometers is functioning. The scalings and record are for August 9, 1926. I have now measured the photographic record and reduced its readings; the results are given in the following table, which may be of interest in showing how the Godhavn Observatory is able to make precise determinations of base line despite the nearly continuously changing magnetic field.

It appears from the tabulation that the actual range in the five observations for the first position of the magnet was 30′ 15″, and for the second position of the magnet 3′ 37″; the actual photographic record during the period of observation shows much more pronounced movements of the magnet. Thus it will be seen that, despite the generally magnetically disturbed conditions prevailing at Godhavn, the methods in use there permit determination of declination base‐line values with a precision quite comparable with that obtained at observatories in lower magnetic latitudes. This is in a large measure due to the special time‐marking arrangement by which the instant of absolute observation is definitely marked on the magnetogram. There is reason to hope that the determination of the base‐line values for horizontal intensity and vertical intensity at the Observatory will be likewise satisfactory.
Principal magnetic storms and earthquake disturbances recorded at the Huancayo Magnetic Observatory, January 1–31, 1927
Authors: Goddard Richard H.
Published: February 2008

(Lat. 12° 02′.7 S.; long. 75° 20′.4 W. or 5h 01m W. of Gr.)

January 1, 1927.—A sudden commencement indicating an increase in horizontal intensity of 22γ began at 8h 47m and ended at 8h 50m. A change of 0′.5 in a westerly direction was shown in declination and an increase of 2γ in vertical intensity.
Summary of the year's work, Department of Terrestrial Magnetism, Carnegie Institution of Washington
Authors: Bauer Louis A. , Fleming J. A.
Published: February 2008

Continued progress has been made in the study of the relationships between disturbances in the Earth's magnetism and electricity and the Sun's activity. The opinion is gaining ground that superposed on a fairly regular fluctuation in the Sun's activity, with which the normal diurnal‐variation of the Earth's magnetism can be correlated to a very high degree, there are more or less irregular and spasmodic fluctuations both of the Sun's and of the Earth's magnetic activity during a solar cycle. For the latter case the correlation between the solar and terrestrial phenomena is not always evident or close. Therefore, special effort was made to obtain required concomitant data from all available and interested sources.
Diurnal variation of atmospheric potential gradient at Samoa
Authors: Kidson E.
Published: February 2008

I was much interested in the article by Mr. Andrew Thomson in the number of the Journal for September 1926 on the diurnal variation of atmospheric potential‐gradient at Samoa. The “reef‐house” in the lagoon at Samoa was built in order to reproduce oceanic conditions. It seems that in many respects, however, it must fail to do so and some of these may be of vital significance as regards the diurnal variation of potential gradient. Although the trade‐wind at Apia blows parallel to the coast, it is highly probable that a proportion at least of the air flowing over the station has passed over the land and suffered important modification in the process.
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.
Temperature‐compensation and adjustment of magnetic variometers
Authors: McComb H. E. , Ludy A. K.
Published: February 2008

A horizontal‐intensity magnetic variometer was equipped with a quartz‐filament suspension, the tips of which were bent at right‐angles before attachment to the supports. The instrument was compensated for temperature and the effectiveness of this compensation checked in a short time by determination of base‐lines when instrument was operated at different temperatures.
Sitka Magnetic Observatory January to March, 1930
Authors: Ulrich Franklin P.
Published: February 2008

January 4–8, 1930—Although extending over several clays, this storm is not a particularly large one and could be considered several small active storms with intervening slightly disturbed periods. The most active parts occur on January 4, 8h to 16h; January 5, 10h to 17h; and January 6, 11h to 21h. The curves can be followed at all times and during these periods the ranges are rather large with relatively slow motion except on January 6, 17h to 21h when they appear as small rapid oscillations.
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).
The effect of the sunspot‐cycle on the magnetic diurnal variation at Apia
Authors: Westland C. J.
Published: February 2008

In this article the data used are the hourly values in magnetic declination, D, and horizontal intensity, H, each hourly value having been computed from the mean ordinate to the curve during the period of sixty minutes commencing at the Greenwich hour stated. The difference between the highest and lowest hourly value in the day is called simply the “Range,” brevitatis causa. Results of harmonic analyses are given following the notation H or D=m + r1 sin (A1+t) + r2 sin (A2 + 2t) + …….
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.
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.
Provisional sunspot‐numbers for March and April, 1931
Authors: Brunner W.
Published: February 2008

(Dependent alone on observations at Zürich Observatory and its station at Arosa)
Huancayo Magnetic Observatory April to August, 1931
Authors: Ledig Paul G.
Published: February 2008

(Latitude 12° 02′.7 S.; longitude, 75° 20′.4 or 5h 01m W. of Gr.)

There were no magnetic storms recorded during the period.
Test‐deflections for variometers and magnetographs (concluded)
Authors: Hartnell George
Published: February 2008

39. Mutual effects, D‐ and H‐variometers—The mutual potential energy of two suspended magnets in the same horizontal plane is derived from equation (10) by setting ω = β = 0°. Thus

urn:x-wiley:00968013:media:tma31590:tma31590-math-0001
when C ≡ MDMH/d3, in which MD and MH indicate the magnetic moments of the D‐ and H‐magnets, respectively. In this equation ϕ now indicates the position of the H‐magnet, and θ indicates the position of the D‐magnet. The mutual torque on D is

urn:x-wiley:00968013:media:tma31590:tma31590-math-0002
The mutual torque on H is

urn:x-wiley:00968013:media:tma31590:tma31590-math-0003
It is assumed that the two variometers are in the magnetic prime‐vertical
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.
Das Rätsel der erdmagnetischen Säkularvariation
Authors: Schmidt Von Adolf
Published: February 2008

Unser Wissen von der Säkularvariation des Erdmagnetismus ist von Louis A. Bauer nach zwei Richtungen bedeutsam erweitert worden. In seiner Berliner Inaugural‐Dissertation vom Jahre 1895 hat er für alle Orte, von denen schon damals längere Reihen von Deklinations‐und Inklinationsbeobachtungen vorlagen, das Vektordiagramm der säkularen Aenderung der Kraftrichtung entworfen. Aus seinen Ergebnissen glaubte er schliessen zu dürfen, dass das Diagramm an allen Punkten der Erdoberfläche in demselben Sinne—von aussen gesehen in dem der Uhrzeigerbewegung—durchlaufen werde. In einer späteren Arbeit wies er darauf hin, dass die älteren Berechnungen des erdmagnetischen Potentials für das magnetische Moment der Erde einen wesentlich höheren Wert ergeben haben» als die neueren, die auf den Karten von Neumayer beruhen.
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.
On potential gradient and the air‐Earth current
Authors: Whipple F. J. W.
Published: February 2008

(1) Introduction—The fundamental phenomena in the atmospheric electricity of fine weather are three. The gradient of potential is normally positive, that is, such that the electric force drives positive electricity downwards. The air is a conductor of electricity, the conductivity depending on ionization. Electricity flows continually into the ground, the current being positive as long as the potential gradient is positive.
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.
Sources of errors in the determination of the potential gradient of the Earth's electric field
Authors: McNish A. G.
Published: February 2008

Potential‐gradient data are likely to be misinterpreted if space‐charge distributions are not given appropriate consideration. The magnitude of these effects is investigated for various space‐charge conditions. The errors which enter into reduction‐factor determinations from this source are calculated, and conditions for reducing this error to a minimum are outlined. Equations are developed for the effect of finite space‐charge distributions on the quantity V/h. The equations show that if the horizontal extent of the space‐charge layer is several times its thickness, errors introduced by considering its horizontal extent as very great are negligible.
Summary of the year's work, Department of Terrestrial Magnetism, Carnegie Institution of Washington
Authors: Fleming J. A.
Published: February 2008

The death on April 12, 1932, of Louis Agricola Bauer, Director from 1904 and Director Emeritus from 1930 of the Department, removed from science an internationally recognized authority on geophysics. Largely through his enthusiasm and organizing ability, based on his earlier work in the magnetic survey of the United States Government, the systematic magnetic survey of the whole Earth, sponsored by the Carnegie Institution of Washington upon his initiative, was accomplished. This survey established the empirical basis of required accuracy for theoretical discussions of the origin and behavior of the Earth's magnetic field. Bauer was among those foremost in the discussion of terrestrial magnetism and of related geophysical problems, as is evidenced by his many scientific contributions.
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.
Watheroo Magnetic Observatory July to September 1932
Authors: Parkinson W. C.
Published: February 2008

(Latitude 30° 19′.1 S.; longitude, 115° 52′.6 or 7h 43m.5 E. of Gr.)
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.
Biographical sketch of Professor Doctor Albert Wigand
Authors: Dominik H.
Published: February 2008

Albert Wigand was born at Kassel on October 21, 1882, the son of Dr. Paul Wigand, pastor, and Luise, née Thiersch. He was a descendant of an old family of theologians and natural philosophers. After completing his studies at the humanistic Lessing Gymnasium at Frankfurt‐am‐Main, Wigand studied from 1901 to 1906 in Marburg and München, the natural sciences, mathematics, and philosophy. He received in 1906 the degree of Ph.D. at Marburg, with a physical dissertation, as a pupil of Richarz, and passed in Marburg the same year the state examination for teachers of physics, mathematics, chemistry, mineralogy, and philosophical propaedutics for the higher grades. After two years as assistant to Richarz in Marburg, Wigand was engaged from 1907 to 1910, as assistant in physics to Hallwachs at the Technische Hochschule in Dresden. In 1910 he went as assistant in physics to the Physical Institute of the University of Halle at Dorn, and became in 1911 privatdozent in physics and physical chemistry. The title of professor was conferred on him in 1917, he was commissioned to teach physics of the atmosphere in 1920, and in 1921 he was appointed “nichtbeamteter ausserordentlicher Professor” at Halle. In 1925 Wigand accepted a call as professor of physics and meteorology at the Landwirtschaftliche Hochschule, Hohenheim‐Stuttgart, at the same time giving courses in meteorology at the Technische Hochschule, Stuttgart. On April 1, 1929, he was called to Hamburg University to occupy the newly established chair of meteorology which constituted the continuation of the meteorological post previously held by Alfred Wegener and Georgii as associate professors. As director of the Meteorological Institute of Hamburg University, Wigand was also entrusted with the direction of the Meteorological Experiment Station of the Deutsche Seewarte which had developed out of the Koeppen Grossborstel Pilot‐Balloon Station. The Institute is combined with the Experiment Station and since January 1931 has been housed in a new building erected at government expense and belonging to the Deutsche Seewarte, on the north side of the airport in Fuhlsbüttel. On July 4, 1931, Wigand was chosen rector of the Hamburg University for the period October 1, 1931 to September 30, 1932.
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.1

Dirac2 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.
Sitka Magnetic Observatory, July to September 1934
Authors: Hershberger John
Published: February 2008

July 30—This storm began sharply at 3h 19m, G. M. T., in all three elements, although the initial amplitudes were not large. At first the two intensity‐components increased, while the east declination decreased. This trend was reversed at about 7h. From then on the fluctuations became more violent, reaching their largest amplitudes at about 12h, when the horizontal intensity had dropped to 14527 gammas, more than 900 gammas below normal. The maximum had come at about 6h 51m, when its value was 15826 gammas, giving a range of 1299 gammas. Ranges of the other elements were: Declination, 131′; vertical intensity, 735 gammas. The storm ended at about 16h.
Die Magnetisierung der Erde Unter den Ozeanen
Authors: Nippoldt Von A.
Published: February 2008

As many years must pass before the large amount of ocean data collected by the Carnegie Institution of Washington can be analyzed by the tedious method of Gauss, it seems suitable, in the meantime, to seek some other method capable of answering, to a certain extent, some of the principal geophysical questions. One such question is that pertaining to the distribution of the non‐uniform magnetization of the Earth. In a previous paper the author described a new rapid method based on the computation of Bauer's “local magnetic constant”
, for a number of points distributed over the Earth's surface and investigated the law of distribution. For this investigation the magnetic results obtained at the various observatories were used. In the present paper the study is extended to the ocean areas and is based on the ocean magnetic observations obtained by the vessels operated by the Department of Terrestrial Magnetism. The method of computation is briefly described and the results of the study exhibited in a map for the epoch 1922 showing the lines of equal inhornogeneous magnetization of the Earth at intervals of 1 milligauss or 100γ, From an inspection of the map it is concluded that the distribution of the inhomogeneous magnetization over the oceans is quite systematic and not merely fortuitous and that it is not caused by the three upper kilometers (mean depth of the oceans) of the Earth's crust, having its seat principally at depths which have little to do with the surface‐distribution of land and water. The details of the magnetic situation are discussed especially in comparison with the previous chart (based on observatory data). The effect of polar movement is also considered but little weight is given it for the period in question. In connection with the question of constancy of magnetization of masses at great depths in the Earth's crust, comparisons with several recent studies of anomalies are made.
Determinations of the magnetic declination at sea on a motor‐boat
Authors: Ljungdahl Gustaf S.
Published: February 2008

An account is given of the method used to derermine the magnetic declination at sea on an ordinary motor‐boat. The reliability of the results is ascertained by repeat‐measurements. Dynamic deviations of the liquid‐compass are demonstrated. Results in a rough sea determined by observations on a single heading may be less trustworthy than a mean obtained on various headings.
Agenda for the Warsaw Meeting of the International Commission of Terrestrial Magnetism and Atmospheric Electricity, September 1935
Authors: la Cour D.
Published: February 2008

Following the call of President Maurain the first session of the Commission will take place at Warsaw September 2, 1935, at 10 a. m. in the Staszic Palace, Nowy Swiat 72 (entrance by main door facing Copernik Place).

Professor Kalinowski has kindly invited the members of the Commission to visit the Swider Observatory, near Warsaw. Since a general excursion to the Jablonna Meteorological Observatory is scheduled for September 8, it is recommended that those present at Warsaw September 1, visit Swider on that day. Information as to the time of departure for Swider will be posted at the Bureau of the Conference.
A table of inverse trigonometric functions in radians
Authors: Roman Irwin
Published: February 2008

In the integration of numerous expressions, the results are expressible in the inverse trigonometric functions measured in radians. For three‐ or four‐place evaluations, the customary conversion‐formulas may be applied to tables using the sexagesimal system. For more than four places, the tables become bulky and inconvenient and the conversion tedious, especially when values are wanted to seven or more places. In 1927, the writer needed arctangents for torsion‐balance calculations.
Electricity of rain and thunderstorms
Authors: Simpson G. C.
Published: February 2008

In his article on “Electricity of rain and thunderstorms,” which appeared in the March number of the JOURNAL, Dr. Ross Gunn, referring to the production of electricity when a drop of water breaks up in the air, says: “The effect of a superposed charge in modifying the charge generated by break‐up should be investigated in the laboratory.”

It is unfortunate that Dr. Gunn did not read the paper, to which he gives a reference, in which I described the breaking‐drop theory of thunderstorms dismissed by him so summarily; for if he had he would have read: “Experiments were next undertaken to investigate the extent to which the process is affected by any charge already on the drops, for it is quite conceivable that charged drops might behave quite differently from uncharged drops.” The experiments are then described in which over four thousand charged drops were broken up, with the result that I was able to state quite definitely that the positive charge produced when a drop of water is broken in the air is the same within the accuracy of the experiments whether the drop is charged with positive electricity, with negative electricity, or is completely uncharged.
Huancayo Magnetic Observatory April to June, 1935
Authors: Torreson O. W.
Published: February 2008

(Latitude 12° 02′.7 S., longitude 75° 20′.4 or 5h 01m.4 W. of Gr.)

April 10—The disturbance which began at 12h 37m April 10 was of a minor nature with a short life. It affected the H‐trace principally, interposing large bays with an approximate period of 30 minutes. The most rapid change was in the 10‐minute period beginning at 16h 32m. During this interval the horizontal intensity increased 112 gammas.