bluuebunny/crossref_metadata_2025 huggingface dataset:
On the correlation of radio reception with the Moon's position in the observer's sky
Authors: Stetson Harlan T.
Published: February 2008

Papers previously presented by the writer,1 and by G. W. Pickard2 and others, have shown significant correlation of the intensity of radio reception with solar activity. The 15‐month cycle in secondary maxima, to which particular attention has been called in the present sunspotcycle by both Stetson and Pickard, have led to numerous speculations as to the possible cosmic causes.

The possibility of planetary influences being the basis for periodic solar disturbances have been exhaustively studied from time to time, notably by Schuster3, Maunder4, and Brown5. The relatively small tidal forces of the planets give little encouragement for disturbances arising on the gravitational basis. The fact, however, that the 15‐month period corresponds fairly closely with two sidereal periods of Venus and five of Mercury, with the arrival of Mercury at perihelion at approximately the same interval, suggested to the writer that charges on these inner planets might be a disturbing factor in the electrostatic equilibrium of the solar atmosphere.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, October to December, 1930
Authors: Nicholson Seth B. , Sternberg Elizabeth E.
Published: February 2008

During the last quarter of 1930 several magnetic storms of intensity 1.0 and two of intensity 1.5 were recorded at Mount Wilson.

On October 3, at 4h 36m, G. M. T., a disturbance of intensity 1.0 began with an increase in the horizontal intensity. At 10h 18m of the same day the horizontal intensity again increased suddenly, but neither of these changes had the appearance of a typical “sudden commencement.” An active spot‐group which crossed the central meridian on October 2 was 11° west at the beginning of this storm.
Cheltenham Magnetic Observatory October to December, 1930
Authors: Hartnell Geo.
Published: February 2008

(Latitude 38° 44′.0 N.; longitude, 76° 50′.5, or 5h 07m.4 W. of Gr.)
The lunar‐diurnal magnetic variation in relation to the geographic and magnetic equators
Authors: Egedal J.
Published: February 2008

In an article in the Ad. Schmidt‐Festschrift1 it has been stated that a representation of the field of the solar‐diurnal magnetic variation ought to contain magnetic as well as geographic coordinates, since the solar‐diurnal variation depends on magnetic latitude of the place of observation. Now it will be shown also that the lunar‐diurnal magnetic variation depends on the magnetic latitude of the place of observation.

Reckoning the declination positive towards east, the lunar‐diurnal variation for the northern hemisphere is given approximately by

urn:x-wiley:00968013:media:tma31521:tma31521-math-0001
where l is the amplitude and t the lunar hour‐angle. For the southern hemisphere the lunar‐diurnal variation is given by

urn:x-wiley:00968013:media:tma31521:tma31521-math-0002
Up to the present it has not been possible to say whether the change of 180° in the phase‐angle takes place at the geographic equator or at the magnetic equator (where the magnetic vertical intensity Z is zero). This problem is solved when the lunar‐diurnal variation is determined for a place lying between the two equators.
Sitka Magnetic Observatory January to March, 1931
Authors: Ulrich Franklin P.
Published: February 2008

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

The magnetic activity for this quarter was exceptionally low, the sum of the magnetic characters for the quarter being 23. The present observer has been at Sitka since 1918, and since that time there have been only two quarters when the magnetic activity was less. In the first quarter of 1921 the magnetic activity or the sum of the magnetic characters was 21 and in the third quarter of 1923 the sum was 23. The quarters of greatest activity were the second quarter of 1930 with a sum of 79, the first quarter of 1926 with a total of 70, and the third quarter of 1930 with a total of 68. The years of highest activities were 1930 with a total of 252, and 1918 with a total of 216. The years of lowest activity were 1923 with a total of 115, and 1921 with a total of 131.
The influence of hydrostatic pressure on the critical temperature of magnetization for iron and other materials
Authors: Adams L. H. , Green J. W.
Published: February 2008

This cooperative investigation by L. H. Adams and J. W. Green, of the Geophysical Laboratory and Department of Terrestrial Magnetism, respectively, both of the Carnegie Institution of Washington, was undertaken principally because of its bearing on the Earth's magnetic field and its relation to the problem of the central iron‐core. The object was to determine whether or not the temperature at which iron and other ferromagnetic substances pass from the magnetic to the non‐magnetic state is affected by an increase of pressure.

The specimens of the materials investigated were made up as the core of a miniature transformer or induction‐unit, and placed in an electrically heated pressure‐bomb. A six‐volt alternating‐current was supplied to the primary of the transformer and the output from the secondary was amplified, rectified, and carried to a direct‐reading galvanometer. The temperature of the inversion‐point, indicated by the galvanometer‐reading dropping to zero, was measured by means of platinum‐platinrhodium thermocouples.

Five ferromagnetic metals were used. Determinations were made at pressures up to 2,000 atmospheres for iron and magnetite, 2,200 atmospheres for nickel, 2,600 atmospheres for nickel‐steel, and, in the case of meteoric iron, 3,600 atmospheres. The results indicate that pressure has practically no effect on the inversion‐point, although the possibility of a slight decrease is not excluded, as there was a slight tendency toward depression, especially in the case of nickel‐steel and meteoric iron.

On the whole, it seems a fair inference that the pressure‐coefficient of the magnetic inversion‐point remains zero or negative even at the high pressures in the Earth's interior, and that consequently the permeability of the nickel‐iron core of the Earth is not significantly higher than that of ordinary rocks.
Observations of the aurora australis, Byrd Antarctic Expedition, 1929
Authors: Davies F. T.
Published: February 2008

Observations of both the aurora borealis and australis indicate the existence of an auroral zone in each hemisphere and a belt of maximum activity within these zones. In the northern hemisphere this belt is situated some 23° from the point in which the axis of the uniform magnetic field of the Earth meets the surface. This point is not the magnetic pole, however, but is situated some hundreds of miles from it. Analysis of the auroral records of antarctic expeditions shows that a similar distribution of auroral frequency occurs in the southern hemisphere, though the data are insufficient to establish the position of the maximum activity‐belt as accurately as is the case in the northern hemisphere.
On observations of magnetic anomalies with a variometer
Authors: Koenigsberger J. G.
Published: February 2008

The accuracy of determinations for magnetic anomalies in horizontal intensity, H, and vertical intensity, Z, using the author's variometer, is now as good as that obtained by absolute measurements. The variometer can be used accurately without resetting for determinations on lines as long as 300 kilometers in the north‐south direction. The question as to whether local anomalies may be affected by secular variations is discussed theoretically. An attempt to check the theory developed using previous observations of intensity gives no definite conclusions; absolute measurements of inclination with the dip‐needle are not of sufficient accuracy to give a reliable test. In the study of a deep‐seated regional anomaly and in the preparation of land magnetic charts, it is found best to discard all values at stations where the adjacent rocks have differences of susceptibility of more than 2×10−4.
Test‐deflections for variometers and magnetographs
Authors: Hartnell George
Published: February 2008

1. Introduction—This paper develops equations describing the deflections of a suspended magnet produced by a deflecting‐magnet fixed in any desired position. The distances are assumed large enough to render distribution‐effects negligible. The equations are applied individually to a declination (D), horizontal‐intensity (H), and vertical‐intensity (Z) variometer, and to an assembly of these three variometers, which constitute a magnetograph. Under the conditons assumed, the equations furnish a convenient means of testing magnetic instruments.
Provisional sunspot‐numbers for August, September, and October, 1931
Authors: Brunner W.
Published: February 2008

(Dependent alone on observations at Zürich Observatory and its station at Arosa)
Provisional solar and magnetic chracter‐figures, Mount Wilson Observatory, July, August, and Septenber 1931
Authors: Nicholson Seth B. , Sternberg Elizabeth E.
Published: February 2008

During the third quarter of 1931 only one storm was recorded during which the range in II exceeded 100γ. The hydrogen spectroheliograms of September 15 show a marked increase in the activity associated with the spot‐group which was about 33° west of the central meridian at the commencement of this storm.

On July 23 a moderate storm began suddenly at 3h 21m G. M. T.
American URSI broadcasts of cosmic data
Authors: Clarke Katharine B.
Published: February 2008

Beginning the middle of August 1931, Science Service, cooperating with the American Section of the International Scientific Radio Union (URSI), is adding to the cosmic data, collected and broadcast, information concerning aurora. These data are supplied daily by the Alaska Agricultural College and School of Mines at College, Alaska.

The aurora data as given out by Science Service have been decoded and added to the table of cosmic data which is published regularly in the JOURNAL. Under the general heading of aurora in the table, the first column gives the character of the day: 0 indicates no aurora; 1, faint; 3, moderate; 5, strong; 7, brilliant; and 9, no observation or no observations possible on account of cloudiness. The second column gives the number of hours during which aurora was present. The third column indicates the amount of sky covered by cloud on a scale of 0–10, where 0 means cloudiness, and 10 completely overcast.
A typical case of variability of the quiet‐day diurnal variation in terrestrial magnetism and Earth‐currents at Watheroo
Authors: Bartels J. , Rooney W. J.
Published: February 2008

The small magnetic diurnal‐variation recorded at the Watheroo Observatory, Watheroo, Western Australia, on two successive magnetically very quiet days, February 3 and 4, 1929, was noteworthy. This case is discussed as typical for the variability of the quiet‐day diurnal‐variation. A significant parallelism is found with the diurnal‐variation of earth‐currents.
Sitka Magnetic Observatory October to December 1931
Authors: Ulrich Franklin P.
Published: February 2008

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

There were no large magnetic storms during this quarter, all of the storms being only mildly active for some time or moderately active for short periods.
Huancayo Magnetic Observatory September to December 1931
Authors: Ledig Paul G.
Published: February 2008

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

October 29–30, 1931—A mild magnetic storm was recorded beginning October 29 at 8h 39m (Greenwich mean time). At that time the H‐trace showed a slow upward trend of 13γ occupying 6 minutes; thereafter the element was mildly oscillatory and decreased steadily. At about 11h 50m large slow movements began to take place and continued until approximately 22h. The storm showed no definite termination, the elements remaining considerably disturbed until 22h on October 31. The month was generally disturbed, but an ending to the storm might be placed tentatively at 21h 20m on October 30. During the progress of the disturbance the D and Z elements showed some irregularities. The normal maximum in H was entirely obliterated on the 29th, but it showed itself on the 30th, though somewhat depressed. The range of the storm was 227γ in H, though over the most disturbed period, from the commencement to 22h on the 29th, the range was only 186γ.
Watheroo Magnetic Observatory September to December 1931
Authors: Parkinson W. C.
Published: February 2008

(Latitude 30° 19′.1 S.; longitude, 115° 52′.6 or 7h 43m.5 E. of Gr.)

October 29, 1931— A mild storm commenced at 7h 43m (Greenwich mean time) on October 29 and ended at 21h 40m the same day. It was followed by a slight disturbance the next day. The total ranges were as follows: Declination, 19′; horizontal intensity, 120γ; vertical intensity, 160γ.
Chapters in the history of terrestrial magnetism
Authors: Mitchell A. Crichton
Published: February 2008

I—On the directive property of a magnet in the Earth's field and the origin of the nautical compass

1—The science of Terrestrial Magnetism is based on the fact that a magnet, free to move about its center of gravity, tends to assume a position of relative rest in an approximately definite direction with respect to the geographical meridian and the vertical at the place of observation. That it should do so must be due to the existence of a field of force which is known as the terrestrial magnetic field [1], and the systematized knowledge of that field, of its variations in time and space, and of its relations with the subject‐matter of other branches of terrestrial and cosmical physics, constitutes the science of Terrestrial Magnetism.
Auroral observations and magnetic conditions at the Sitka Magnetic Observatory, July 1931 to June 1932
Authors: Ulrich Franklin P.
Published: February 2008

This paper is a continuation of the reports, begun in 1923, of the investigation concerning the relation between aurora and the Earth's magnetic field. The investigation of the Earth's magnetic field and its relation to radio reception was discontinued with the report for 1928–29 because of the lack of proper sensitive instruments and because this investigation is being taken up elsewhere in a more detailed manner than was possible at this Observatory.

Instruments and methods—The instruments and methods as outlined in the report for 1923–24 were used during these observations.
Principal published papers of Louis A. Bauer
Authors: Harradon H. D.
Published: February 2008

The total number of contributions to knowledge by Louis A. Bauer alone, or by him in collaboration with others, exceeds 300. These include research papers, scientific reports, lectures, magazine articles, notes, etc. Aside from his favorite field of investigation—terrestrial magnetism—he has to his credit important papers dealing with magnetism, atmospheric electricity, various aspects of terrestrial and cosmical physics, and thermodynamics. To enumerate all these papers would transcend the limits of the space here available, and accordingly only a summary of the chief publications will be attempted.
Magnetic activity—Numerical magnetic character of days
Authors: Duvall C. R.
Published: February 2008

A table of monthly, equinoctial, solstitial, and annual means of the new measure is given for 1930 and 1931 at 17 observatories. Curves of the monthly means are given which show (1) good agreement in the time of maxima and minima at the different observatories; (2) the difference in value and range in value at the different observatories, the far northern observatories having large values, those near the equator small; (3) the decrease in amplitude for 1931 as compared with 1930; this decrease is very nearly in the same proportion as the corresponding decrease in sunspot‐numbers. The question of reducing the amplitudes of the new measure to a common basis is discussed. A table of statistics of the 17 observatories and of the new measure is given to aid in this discussion. No satisfactory result is arrived at, and it appears questionable whether such a result is possible. The monthly means of the new measure are analyzed for both years at the 17 observatories and the results given in a table. A discussion of this table and a comparison with some results given by Chree leads to the conclusion that a seasonal variation in the new measure is well established.
Magnetische Vermessungen in Deutschland
Authors: Haussmann Von K.
Published: February 2008

Vor einem Jahrhundert waren es hauptsächlich A. von Humboldt, W. Weber und C. F. Gauss, und G. Erman, die in Deutschland das Interesse für erdmagnetische Forschung in weiten Kreisen wachgerufen haben. Gauss und Weber haben im Jahre 1833 in Göttingen ein vollständiges magnetisches Observatorium errichtet. Gauss hat für den Erdmagnetismus eine feste mathematische Grundlage geschaffen. Für die magnetische Feldmessung hat J. Lamont Instrumente und Methoden geschaffen und in Deutschland und im westlichen Europa grosse Messungen ausgeführt.2
Études sur l'électricité atmosphérique au Val‐Joyeux et à Paris
Authors: Maurain Par Ch.
Published: February 2008

Des observations relatives à l'électricité atmosphérique ont été instituées au début de 1923 au Val‐Joyeux, à 30 kilomètres S. W. de Paris, Observatoire dépendant de l'Institut de Physique du Globe de l'Université de Paris. Depuis le 1er mars 1923, le champ électrique est enregistré, et des mesures de la conductibilité électrique sont faites trois fois par jour, à 9h, 13h, et 17h. De plus, des mesures du nombre des gros ions et des petits ions ont été faites au même endroit au cours de plusieurs années. D'autre part, des mesures de la conductibilité et du nombre des ions ont été faites à diverses époques au Service central de l'Institut de Physique du Globe, qui est situé dans Paris, à l'angle des rues Saint Jacques et Pierre Curie, entre la Sorbonne et le Val‐de‐Grâce; ces mesures, faites avec des appareils semblables à ceux employés au Val‐Joyeux, ont permis de comparer les résultats obtenus à la campagne et dans une grande ville.
Reverend Ricardo Cirera, S. J.
Authors: Rodés Luis
Published: February 2008

Rev. Ricardo Cirera, S. J., founder and first director of the Observatorio del Ebro, died at Barcelona, August 3, 1932, at the age of 66 years. He was born in Os de Balaguer (Lérida) July 16, 1864, and entered, while still very young, the Company of Jesus, of which he was a member for 52 years. The studies required by the Order were completed by him with signal success owing to his powers of clear thinking and his intense application.

Before terminating his ecclesiastical studies he was sent to the Philippines to collaborate with Father Federico Faura in directing the Manila Observatory, with the hope on the part of his superiors, that one day he would be able to replace Father Faura and take upon himself the responsibilities of the directorship. He embarked at Barcelona July 27, 1888 and reached Manila August 28, but he was able to remain only a few weeks with Father Faura who on account of his health, was obliged to leave for Spain the middle of the following month. On his arrival at the Observatory, the young student, at the time 24 years of age, assumed charge of the Magnetic Section initiated by his confrère, Father Martín Juan, and added to the absolute observations already being made by the latter, the continuous registration of the magnetic variations in a separate building constructed for the purpose where all the instruments were in normal operation on January 1, 1890.
Provisional sunspot‐numbers for September, October, and November 1932
Authors: Brunner W.
Published: February 2008

(Dependent alone on observations at Zürich Observatory and its station at Arosa)
Sitka Magnetic Observatory July to September 1932
Authors: Ulrich Franklin P.
Published: February 2008

(Latitude 57° 03′.0 N.; longitude, 135° 20′.1 or 9h 01m.3 W. of Gr.)
The diurnal inequalities of horizontal force at Abisko and at Sodankylä
Authors: Rolf Bruno
Published: February 2008

A Toepfer magnetograph, purchased by the Royal Academy of Sciences in 1913, was installed at the Abisko Geophysical Observatory by the writer in June, 1921, for the Meteorological and Hydrographical Service of Sweden. This was for the purpose of cooperating with the Fram drift under Amundsen to further knowledge of arctic magnetic perturbations. Absolute observations to determine base‐line values could be made only at the beginning of the series by Dr. G. S. Ljungdahl and at its end by the writer. These were sufficient for accurate calculation of scale‐values for the variometers from deflection experiments, which were made fortnightly throughout the series, and to deduce the differences for magnetically quiet days in horizontal force (H) and in declination (D) between Abisko and Sodankylä.
Provisional sunspot‐numbers for December, 1932, and January and February, 1933
Authors: Brunner W.
Published: February 2008

(Dependent alone on observations at Zürich Observatory and its station at Arosa)
Watheroo Magnetic Observatory October to December, 1932
Authors: Parkinson W. C.
Published: February 2008

(Latitude 30° 19′.1 S.; longitude 115° 52′.6 or 7h 43m.5 E. of Gr.)

There were no major magnetic disturbances recorded at the Watheroo Magnetic Observatory during the fourth quarter of 1932. A relatively small storm was recorded October 14–15.
Problems in the geologic interpretations of the Earth's major magnetic anomalies
Authors: Jenny W. P.
Published: February 2008

The writer assumes that the magnetic field along the Earth's surface would correspond mainly to the field of a magnetized sphere and that the magnetic axis of this sphere would coincide with the rotational axis, if it were not for the varying chemism and the tectonic dislocation within the magma‐zone and rock‐zone of the Earth. From the total Earth's magnetic field is deducted an inner portion. The remaining field contains major, continental, regional, and local anomalies, which are classified first theoretically and second empirically. The empirical major anomalies are represented in the form of magnetic vectors. The main high and low magnetic trends as indicated by these vectors show a striking parallelism with the main trends of the alpine orogeny. The small secular variations of the declination of the circum‐Pacific stations as compared with circum‐Atlantic stations are explained by the general conception that the basement of the Pacific is more stable than the basement of the Atlantic.
The calculation of electrical resistivity for a region underlying two uniform layers—Concluded
Authors: Roman Irwin
Published: February 2008

While the problem has been solved theoretically and while a complete solution may be obtained as accurately as may be needed, at least in theory, practical importance suggests that the simple geophysical case be studied in more detail. The special conditions of this case make possible numerous simplifications of the results. Since the medium G1 is air, we may take σ1=0. Since the current‐pole is essentially at the surface of the Earth, we may take b=0. Since the potential is measured essentially at the surface of the Earth, we may take z=0. Thus, for this case, three important quantities vanish.
Huancayo Magnetic Observatory April to June, 1933
Authors: Cairns J. E. I.
Published: February 2008

April 30‐May 2, 1933—This storm of moderate intensity began with a sudden commencement in all three elements on April 30, 1933, at 16h 27m 49s Greenwich mean time as determined from the magnetogram from the rapid la Cour magnetograph. By 16h 28m 16s the horizontal intensity had decreased 14γ. From that time until 16h 32m 42s, when the maximum value of the storm was recorded, there was a continual increase in horizontal intensity amounting to 99γ. Slow irregular short‐period oscillations marked the horizontal‐intensity trace up to 21h 18m. The values of horizontal intensity decreased 294γ during this period—approximately three times as rapidly as normal. From 21h to 23h there was a recovery of 54γ in horizontal intensity which was lost by 0h May 1.
The Magnetic Observatory in Maisach
Authors: Burmeister Fr.
Published: February 2008

Nearly a hundred years ago the first regular magnetic observations in Bavaria were made, at the instigation of C. F. Gauss, by Johann von Lamont, who in 1836 began making such observations at fixed intervals. These were published in the “Resultate des magnetischen Vereins.” Some few years later Lamont succeeded in founding at the astronomical observatory a special magnetic observatory, which he equipped with instruments of his own construction. It is known that Lamont greatly advanced the science of terrestrial magnetism, chiefly by developing methods of observation, which in part are used to‐day, and also as author of the first fundamental conception of terrestrial magnetism.
American URSI broadcasts of cosmic data
Authors: Clarke Katharine B.
Published: February 2008

The data for terrestrial magnetism, sunspots, solar constant, and aurorae 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.
Watheroo Magnetic Observatory July to September, 1933
Authors: Parkinson W. C.
Published: February 2008

(Latitude 30° 19′.1 S.; longitude 115° 52′.6 or 7h 43m.5 E. of Gr.)

There were no major magnetic disturbances recorded at the Watheroo Magnetic Observatory during the third quarter of 1933.
Terrestrial‐magnetic activity in the years 1931 and 1932
Authors: Bartels J.
Published: February 2008

For a continuation of the series of the u‐measure of terrestrial‐magnetic activity1 daily means of the horizontal intensity in the years 1931 and 1932 were used for four observatories—De Bilt, Honolulu, San Juan, and Tucson (the last mentioned only for January 1931 to August 1932). The data for De Bilt, 1932, were published in November 1933, while the other data were kindly supplied, in advance of publication, by the Director of the United States Coast and Geodetic Survey. The conversion‐factors k, for Honolulu and Tucson, are 1.14 and 1.44, as formerly; for San Juan, k was chosen as 1.24; for De Bilt k = 1.75 was determined by direct comparison with Seddin for the seven years, 1921 to 1927.

A short definition of u may be repeated as the average change, taken without regard to sign, measured in the unit 0.0001 c.g.s. = 10γ, of the daily means of horizontal intensity on the magnetic equator of the Earth. The monthly means of u1 are derived from those of u: For values of u from 0.0 to 0.6, u1 = (100 u − 30) for higher values, u1 increases less rapidly, approaching asymptotically the limiting value 140. The quantity u1 has been introduced in order to obtain a measure of activity which has a frequency‐distribution similar to that of the relative sunspot‐numbers, and therefore is more suitable for research on correlations between terrestrial‐magnetic activity and solar activity.
The atmospheric potential‐gradient at Boulder, Colorado
Authors: Broxon James W. , Strait Louis
Published: February 2008

Potential‐gradient records were made at Boulder for a period of several months. The diurnal variation on clear and undisturbed days was of the double‐maximum type with the usually principal maximum at about 9h, and a second maximum at about 18h, local time. Not only the daily mean gradient, but also all the Fourier harmonic amplitudes (with the exception of the third, which remained constant) were greatest during late winter and least during late summer. The fundamental phase‐constant showed the presence of Mauchly's universal‐time “wave” of 24‐hour period. The seasonal variations of this phase‐constant also resembled those at most stations. The local‐time phase‐constant of the second harmonic, ϕ2 = 190°, was about that found by Mauchly for many land stations. The 6‐hour harmonic of the general mean curve also resembled that at sea and some land stations, amounting to 6 per cent of the daily mean, with zero phase‐angle at local midnight.
Atmospheric‐electric observations of the potential gradient at Chesterfield, Canada
Authors: Currie B. W.
Published: February 2008

Summary—Continuous records of the atmospheric potential‐gradient were taken at the Canadian International Polar Year station at Chesterfield, N. W. T., from April to August 1933 inclusive. After excluding all days with snow‐drift, fog, or negative values af the potential gradient, 57 days are classed as undisturbed meteorologically. The mean hourly value of the potential gradient for these days is 68 volts per meter. The mean hourly value for each month is practically constant with the exception of April, which has an unusually low value. Analysis of the diurnal variations shows a predominating 24‐hour wave with its maximum varying from 17.7 hours G. M. T., for April and May to 18.7 hours G. M. T., for June, July and August. The potential gradient is definitely higher for days with wind off Hudson Bay than for days with the wind in other directions.
Messungen der Exhalation von Radiumemanation aus dem Erdboden
Authors: Zupancic Von P. Reginald
Published: February 2008

The amount of radon given off from the soil was measured by a new method. An area of 2800 cm2 of lawn was covered by a zinc cylinder filled with air completely free of radon at the beginning of each experiment. Twelve or 24 hours later the air from the cylinder after thorough mixing was introduced in an ionisation‐vessel calibrated in curies and measured in the usual way. From this measurement the amount of radon exhaled from the soil per square centimeter and second can be calculated. The average amount of this exhalation of radon as observed in the period December 1932 to July 1933, was 23×10−18 curie per cm2 per sec. Within the period mentioned the minimum of exhalation was found in January and the maximum in June. The exhaltation during the day is about 1.5 times as much as in the night hours. The maximum value of exhaltation during the observation‐period of about six months exceeds the minimum by about 100 times. Exhalation of radon is mainly governed by the temperature of the soil, increase of this temperature causing an increase of exhalation of radon. Freezing of the soil decreases the amount of exhalation almost to zero. Atmospheric pressure and its variations seem to be of secondary importance.

Zusammenfassung—Die Exhalation von Radiumemanation aus dem Erdboden wurde nach einem neuen Verfahren quantitativ untersucht: Auf die zu untersuchende Stelle des Bodens wurde ein grosses Metallgefäss mit der Öffnung nach unten eingesetzt und die darin enthaltene Freiluft bei Beginn des Versuches durch Einleiten emanationsfreier Luft aus einem Pressluftzylinder verdrängt. Nach 12 bis 24 Stunden wurde die in dieser Zeit ins Gefäss eingetretene radonhältige Luft nach gründlicher Durchmischung des Gefässinhaltes in eine in curie geeichte Ionisationskammer übergeführt und im radioaktiven Gleichgewicht gemessen. Daraus wurde die mittlere Exhalation berechnet. Für die erste Jahreshälfte ergab sich ein Mittel von 23×10−18 curie/qcm sec. Es zeigte sich ein ausgeprägter Jahresgang mit dem Minimum im Jänner und dem Maximum im Sommer. Es konnte festgestellt werden, dass die Exhalation bei Tage ungefähr 1½ mal so gross ist wie bei Nacht. Das Verhältnis zwischen grösstem und kleinstem Wert im Laufe der Untersuchung war 1:100. Die Exhalation erwies sich als sehr stark abhängig von der Bodentemperatur: Eine Erwärmung des Bodens bringt eine Erhöhung der Exhalation mit sich. Einen geringeren Einfluss üben Luftdruck‐schwankungen aus. Überaus stark wird sie durch das Gefrieren des Bodens behindert.
Provisional sunspot‐numbers for December, 1933, to February, 1934
Authors: Brunner W.
Published: February 2008

(Dependent alone on observation at Zürich Observatory and its station at Arosa)
Watheroo Magnetic Observatory October to December, 1933
Authors: Parkinson W. C.
Published: February 2008

(Latitude 30° 19′.1 S.; longitude 115° 52′.6 or 7h 43m.5 E. of Gr)

There were no major magnetic disturbances recorded at the Watheroo Magnetic Observatory during the last quarter of 1933.
AURORAE AND EARTH‐CURRENTS
Authors: Rooney W. J.
Published: February 2008

A comparison of auroral observations and earth‐current records from the College‐Fairbanks Station during the International Polar Year 1932–33 shows considerable agreement between the aurorae and disturbances in the earth‐current records. Coefficients of linear correlation from 0.71 to 0.76 were obtained from the records for 80 clear nights. Effects associated with brilliant isolated auroral displays at College are readily detected in the earth‐current records at Tucson, Arizona, and in exceptional cases, in records obtained as far south as Huancayo, Peru. Oscillatory disturbances in the earth‐current records and moving types of aurora, respectively, seem to show the highest degree of correlation. These results are at variance with comparisons of magnetic and auroral records which indicate a lack of relationship between the two phenomena.
FINAL RELATIVE SUNSPOT‐NUMBERS FOR 1933
Authors: Brunner W.
Published: February 2008

The following Tables contain the final sunspot‐numbers for 1933, for the whole disc of the Sun, based on observations made at the Zürich Observatory, supplemented by series furnished by other cooperating observatories for days (indicated by asterisks) where no observations were possible at Zürich.

Table 1 gives the yearly means of the relative numbers, R, since the last minimum 1923 and the number of days without spots.
Note regarding aurorae and Earth‐currents
Authors: Rooney W. J.
Published: February 2008

In the final paragraph of my paper “Auroræ and Earth‐Currents” in the June issue of the JOURNAL (39, 103–109, 1934) appears the statement that the results of the British Antarctic Expeditions led Dr. Chree to the conclusion that there is no definite relationship between auroral and magnetic activities. My attention has been called by Dr. C. S. Wright to the fact that this statement is inaccurate unless a very specialized and unusual significance is given to the word definite, since the records of those expeditions do show a certain degree of correlation which is high in some respects. The inadequacy of the reference may best be corrected by quoting from Dr. Wright's report “Observations on the Aurora, British (Terra Nova) Antarctic Expedition, 1910–1913” (Harrison and Sons, Ltd., London, 1921), which was critically reviewed by Dr. Chree prior to publication. On page 34 the report states:

“The whole relation between magnetic and auroral disturbances . . . may be stated as follows:
Report of ionosphere‐investigations conducted at College‐Fairbanks, Alaska, during the winter of 1933–1934
Authors: Fleming J. A.
Published: February 2008

The investigations of the ionosphere begun at Fairbanks, Alaska, during the Second International Polar Year were continued during the winter of 1933–1934. Continuous automatic registrations of ionosphere virtual‐heights on a frequency of 2050 kc were made. The equipment, as modified for this work, is described. The transmitter and receiver were operated at separate locations until February 10, 1934, when they were moved to College, Alaska, and further modified for side‐by‐side operation.

A typical record is illustrated. Tabulated values of virtual height during the morning show that, following the appearance of the critical frequency, the virtual heights fall rapidly to an average value of about 210 km, identifying the layer returning reflections on this frequency as the F‐layer.

The periods during which reflections are returned and the times of critical frequency are shown. The usual morning increase in ionization is shown to be associated with sunrise, and from these data it is deduced that the ionizing rays of the Sun must be absorbed below a certain limit in the atmosphere when they are directed parallel to the surface of the Earth. The decrease in ionization in the afternoon is associated with time of sunset, but is not as regular. Reflections are observed most frequently near sunrise and sunset, indicating increased absorption near noon. E‐layer reflections are seldom observed, and then only at night, indicating that the maximum ionization of the E‐layer is not sufficient to prevent penetration on 2050 kc.

Comparison of the ionosphere‐data and the magnetic records at the College station is made. The magnetic disturbances usually occurred at night. There was a strong tendency for the usual morning reflections to fail to appear during or following a magnetic disturbance. A striking improvement in the character of the records with side‐by‐side operation is noted and records obtained under such conditions are shown.
Report on measurements obtained at the Huancayo Magnetic Observatory (Peru) following the program of the second International Polar Year during May to August 1933
Authors: Wells H. W.
Published: February 2008

The accompanying tables summarize the measurements made at the Huancayo Magnetic Observatory of the Department of Terrestrial Magnetism of the Carnegie Institution of Washington according to the schedule of the International Polar‐Year program for ionosphere‐measurements. This Observatory is located near Huancayo, Peru, in latitude 12° 02′.7 south and longitude 75° 20′.4 west at an elevation above sea‐level of 11,000 feet. The equipment used was placed in operation during the latter part of April 1933, and the observations reported upon are therefore subsequent to that date. The transmitter and receiver are located side by side so that the transmissions are at vertical incidence.
Arthur Schuster, 1851–1934
Authors: Chapman S.
Published: February 2008

On Sunday, October 14, 1934, at the age of 83, Sir Arthur Schuster died at his home, Yeldall, near Twyford, Berkshire, England, after a long and distressing illness. The science of terrestrial magnetism and electricity thus loses one who made outstanding contributions to its progress.

Arthur Schuster was born at Frankfort‐on‐Main on September 12, 1851, of a Jewish family which, as early as the middle of the eighteenth century, had established a business in cotton goods in England. Till the age of sixteen he lived in Frankfort, where his father was a banker; he then studied French for two years at Geneva. In 1870 he joined his family in Manchester, whither they had emigrated in 1869, and entered his father's business. In the evenings he attended classes at the Owens College (afterwards the University) in that town, and within a year persuaded his father to let him leave the business to follow a scientific career. For a year he studied physics under Balfour Stewart (professor of physics at Manchester, 1870–87), and then studied spectrum analysis for two years under Kirchhoff at Heidelberg, where he obtained the Ph.D. in 1873. Returning to Manchester, he became an unpaid assistant to Balfour Stewart for a year, then studied at Göttingen under W. Weber and at Berlin under Helmholtz; led a British eclipse expedition to Siam (at the age of twenty‐four); spent another year as honorary assistant at Manchester; worked for nearly two years in the Cavendish Laboratory, Cambridge, first under Clerk Maxwell and later under Rayleigh; and in 1878 accompanied another eclipse expedition, to Colorado. This unusually long and varied training, made possible by the support of a wealthy and enlightened parent, enhanced the fruitfulness of his great natural gifts—not only in his capacity as an individual scientific worker, but also, especially in his later years, as a leader in international scientific organisations, work for which he was peculiarly well fitted by his administrative ability and his knowledge of languages.
Magnetic secular‐variation at Apia, Samoa, 1905–1929
Authors: Glover P. W.
Published: February 2008

Equations are derived to represent the series of annual means of the terrestrial‐magnetic elements at Apia, Samoa, from 1905 to 1929. A definite improvement is effected in the representations by the addition to each equation of a term involving the sunspot‐number, with the exception of the case of the vertical intensity. An attempt is made to eliminate the effect of the eleven‐year solar periodicity by forming series of means of overlapping groups of eleven years. Equations are deduced to represent these series. The declination (O‐C) residuals show a remarkably well‐defined periodicity of seven years for which no explanation has yet been established.

The secular variation is also examined by considering the annual chances as due to a variable disturbing force. It is found that the inclination of the direction of this force is rotating slowly from zenithward to nadirward, and that its azimuth is slowly rotating in the direction south to north through east.
Experimental interpretation of magnetic and gravimetric anomalies
Authors: Jenny W. P.
Published: February 2008

A method and apparatus are described, which allow experimental interpretations of magnetic and gravimetric anomalies. The basic difference between this method and other experimental methods so far applied lies in the use of the direction in space of the magnetic lines of force as due to local structures, instead of the magnetic intensity, for interpretative purposes. This method gives due consideration to the inhomogeneous magnetization of structure and to the relation between the magnetization of a geologic structure and its direction of strike and geographical position. Based upon the relationship between magnetic forces and the second derivatives of the gravitational potential as given by Eoetvoes, the direction of the magnetic lines of force as due to local structures may be calculated from the data obtained with torsion‐balances. This procedure makes it possible to also interpret gravimetric anomalies by the experimental method under discussion. As an example for the practical application of this method the large magnetic anomaly at Grand Rapids, Michigan, has been interpreted in terms of structure.
Provisional sunspot‐numbers for December, 1934, to February, 1935
Authors: Brunner W.
Published: February 2008

The statistical aspects of the application of harmonic analysis, introduced by A. Schuster in his famous paper on the investigation of hidden periodicities, are discussed on the basis of recent developments in the theory of probability. Between the two extreme cases of random fluctuations and persistent waves, hitherto discussed exclusively, the intermediate case of quasi‐persistence is introduced and recognized as a common phenomenon in the time‐functions of meteorology, geophysics, and cosmical physics. Statistical methods, based on the conception of the harmonic dial, are given for dealing with quasi‐persistence and its effect on tests for persistent waves, and they are generalized for the case of periodicities of other form than that of the sine‐wave. Typical examples are given illustrating various forms of random fluctuations, quasi‐persistence, and persistence, as well as questions related to harmonic analysis, such as the periodogram, non‐cyclic change, curvature‐effect, equivalent length of sequences, effective expectancy, random walk, interference, and the infective property of quasi‐persistence on adjacent periods (see summary at end of paper).
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, October, November, and December, 1934
Authors: Nicholson Seth B. , Sternberg Elizabeth E.
Published: February 2008

No exceptionally bright hydrogen flocculi were observed during or just prior to any of the storms recorded during the last quarter of 1934. No spots were seen on October 24, but a small group was observed on October 22 and 23 in an area which crossed the central meridian on October 24. On December 3 the only spots on the Sun were included in a group in latitude 28° south which was then 65° west of the central meridian. On December 29 three groups were observed. The positions of the two largest were 14° west and 31° south and 15° east and 24° south.
The green flash
Authors: Davies F. T.
Published: February 2008

The phenomenon of the green flash was looked, for on many occasions during the Polar Year 1932–33 by the Canadian Party at Chesterfield, Northwest Territories, but it was observed only once. This was at sunrise September 1, 1933, at 4:45 a. m. (90° west meridian time). It was seen by J. Rea and the undersigned from the deck of a small schooner in Hudson Bay. A vivid green point changing quickly to a fairly sizable ball of green fire preceded the first glimpse of the Sun. The whole occurrence lasted from two to three seconds. There was hardly any wind and the sea was calm. Long billows of alto‐cumulus clouds running in a northwest to southeast direction covered nine‐tenths of the sky, but for three or four degrees above the eastern horizon the sky was clear.
Sitka Magnetic Observatory October to December, 1934
Authors: Hershberger John
Published: February 2008

October 24—The disturbance, which began gradually at about 4h, G.M.T., was marked by slow fluctuations of the elements until about 8h 40m, when the amplitudes abruptly became much larger and the periods shorter. In about two hours the violent fluctuations ceased, and by 17h the storm had ended. The ranges were: Declination, 69′; horizontal intensity, 338γ; vertical intensity, 697γ.

December 3–4—This storm also began gradually, about 23h, G.M.T., December 3, The first part was characterized by small, short‐period oscillations of the declination. All the elements began to fluctuate violently about lh 45m, December 4, but became relatively quiet again within half an hour, and remained so until about 4h, when another period of rapid fluctuations began, lasting until about 8h. The storm ended about 16h. The ranges were: Declination, 108′: horizontal intensity, 645γ; vertical intensity, 590γ.
Secular change in the magnetic solar‐diurnal variations at the Huancayo Magnetic Observatory
Authors: McNish A. G.
Published: February 2008

A complete change of the character of the solar‐diurnal variations of vertical magnetic intensity observed at the Huancayo Magnetic Observatory during the past sunspot‐cycle is described. Characteristics of the southern type of variation, present during the northern summer solstice during 1922, give place to a form of variation characteristic of the Northern Hemisphere in 1932. This change is associated with the secular change of the Earth's general magnetic field which consists partly of a southern shift of the magnetic equator in the region around Huancayo.

Detailed features of this change are discussed and found to be qualitatively in agreement with expected changes. The large magnitude of the changes indicates that the solar‐diurnal variation is a complex function of the Earth's general field such as is called for by the atmospheric‐dynamo theory of Balfour Stewart. Statistical considerations lead to the conclusion that the reality of the change is established to an extraordinarily high degree of probability.
Cosmic rays from Nova Herculis?
Authors: Hess Victor F. , Steinmaurer Rudolf
Published: February 2008

The appearance of a new star in the constellation of Hercules is of considerable interest not only to the astronomer but also to the physicist. W. Baade and F. Zwicky1 recently estimated the energy of the so‐called super‐novae and advanced tentatively the hypothesis that cosmic rays are produced in the super‐nova process. The few communications2 on the Nova Herculis do not show—as far as they are accessible to us—whether this new star can be classed as of the super‐nova type. At any rate its behavior seems to differ from that of a common nova.