bluuebunny/crossref_metadata_2025_split huggingface dataset:
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.
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.
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 compass1—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.
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.
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.
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.
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.
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.
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.
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.
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.