bluuebunny/crossref_metadata_2025_split huggingface dataset:
Huancayo Magnetic Observatory May to June, 1937
Authors: Davies Frank T. 
Published: February 2008

(Latitude 12° 02′.7 S., longitude 75° 20′.4 or 5h 01m.4 W. of Gr.)May conditions—The average character‐number for May was low, namely 0.1. Only three days during the month were classed as other than zero‐days. These were May 4, 5, and 28. May 5 was very disturbed. Two sudden commencements occurred during the month.
Watheroo Magnetic Observatory May to June, 1937
Authors: Green J. W. 
Published: February 2008

(Latitude 30° 19′.1 S., longitude 115° 52′.6 or 7h 43m.5 E. of Gr.)May 28—There was a sudden commencement at 01h 51m 50s GMT, May 28, as shown by the record of the Crichton‐Mitchell vertical‐intensity inductometer. D suddenly moved 1′ westerly, then 3′ easterly in about forty seconds, followed by a movement 5′ westerly in two minutes. H suddenly increased 5 gammas, then decreased 17 gammas in about forty seconds; these movements were followed by an increase of 18 gammas in two minutes. The numerical value of Z suddenly increased 4 gammas then decreased 13 gammas in about forty seconds; then followed an increase of 20 gammas in three minutes. The character of the trace was “1” during the next twenty‐four hours.
The heating of the ionosphere by the electric currents associated with geomagnetic variations
Authors: Chapman S. 
Published: February 2008

§1. The transient geomagnetic variations (periodic and irregular) appear to be due mainly to primary electric currents flowing somewhere in the ionosphere, and in smaller degree to secondary currents induced within the Earth by the primary currents. These currents must heat the medium in which they flow, and the purpose of this note is to estimate the magnitude of this heating in the ionosphere.§2. Schuster in his important 1907 memoir on S, the solar daily magnetic variation, remarked as follows on the heating of the atmosphere associated with S:
Cheltenham Magnetic Observatory July to September, 1937
Authors: Ludy Albert K. 
Published: February 2008

(Latitude 38° 44′.0 N., longitude 76° 50′.5 or 5h 07m.4 W. of Gr.)July 9–10—A mild disturbance began abruptly, but with small displacements, at 11h 43m GMT, July 9. It ended at 10h, July 10. Ranges: D, 27′; H, 128 gammas; Z, 45 gammas.
Huancayo Magnetic Observatory July to September, 1937
Authors: Davies Frank T. 
Published: February 2008

(Latitude 12° 02′.7 S., longitude 75° 20′.4 or 5h 01m.4 W. of Gr.)July 9—At 11h 44m GMT, July 9, there was a sudden commencement with small increases in D, H, and Z.
Apia Observatory, October to December 1937
Authors: Wadsworth J. 
Published: February 2008

(Latitude 13° 48′.4 S., longitude 171° 46′.5 or 11h 27m.1 W. of Gr.)October 1–13—A magnetic storm commenced at 13h 44m GMT, September 30, with a sudden increase of 20 gammas in H, 6 gammas in Z, and a slight decrease in the easterly declination. This marked the beginning of a disturbed period during which there appeared to be four phases of activity. From the maximum at 15h 34m, September 30, H decreased through a range of 152 gammas to a maximum at 06h 43m, October 1. Another sudden increase of 22 gammas in H at 11h 21m, October 3, was the beginning of more intense activity and the rapid decrease in H on October 4 resulted in a minimum which was too low to be recorded, but the measurable range was 225 gammas. Unfortunately the Z clock stopped on October 3 and the record October 3–4 was missed. There was a period on October 6 during which H, D, and Z showed rapid oscillations of small amplitude which were well defined between 17h and 19h. Conditions appeared to be approaching normal when another disturbance commenced abruptly at 05h 21m, October 7. There was a range of 162 gammas in H associated with this storm. After a short lull, conditions again became disturbed on October 9 between 06h and 07h. The traces showed that the magnetic elements were relatively quiet by October 13 and there were no further disturbances of importance during the remainder of the quarter.
On the diurnal variation of the magnetic pole
Authors: Wasserfall K. F. 
Published: February 2008

Introduction—When Roald Amundsen planned his Expedition with the Gjöa he studied the practical side of the earthmagnetic science at the Observatory at Potsdam, where Ad. Schmidt acted as his chief tutor. Professor Schmidt was personally very interested in this Expedition, especially because it offered the rare opportunity to obtain magnetic observations suitable for fixing the geographical coordinates of the magnetic pole.For use during the Expedition Schmidt provided Amundsen with written instructions, which have been published in part in the magnetic results of the Expedition [see 1 under “References” at end of paper]. Here Schmidt writes: “For an approximate calculation we may accept the following values for the magnetic elements at the surface of the globe in the neighborhood of the magnetic north‐pole: Vertical intensity, V = 62000γ; inclination, I = 90° − 0′.5a, at a distance of a miles from the pole; horizontal intensity, H = 9 × aγ at a distance of a miles from the pole (one mile = 1.852 km). Thus we may, with sufficient accuracy, calculate horizontal intensity by aid of inclination or vice versa, since to each minute by which the inclination is less that 90°, corresponds 18γ, in the horizontal intensity, and we have accordingly Table 1.
American URSI broadcasts of cosmic data, April to June 1938, with American magnetic character‐figure CA, May to July 1938
Authors: Johnston H. F. 
Published: February 2008

The data for terrestrial magnetism, sunspots, and solar constant are the same as given in previous tables.The first three columns of the Table give (1) the magnetic character according to the scale 0–2 of the International Commission of Terrestrial Magnetism and Atmospheric Electricity, (2) the type featuring the day other than normal by the letters b, p, o, and i for days marked by bay, rapid pulsations, long‐period oscillations, and irregular oscillations, respectively, and (3) the hour and minute of Greenwich mean time marking the beginning of a storm, the end of the storm being indicated in the foot‐note to the Table.
Tucson Magnetic Observatory, April to June 1938
Authors: Hershberger John 
Published: February 2008

(Latitude 32° 14′.8 N., longitude 110° 50′.1 or 7h 23m.3 W. of Gr.)April 13–15—A moderate storm began sharply at 11h41m GMT, April 13, with a sudden increase in H of 81 gammas, followed immediately by a decrease of 56 gammas. Numerous similar quick thrusts in H were the chief characteristic of the storm, which lasted until about 01h, April 15. H was somewhat depressed during part of the period, but not greatly at any time.
Apia Observatory, April to June 1938
Authors: Wadsworth J. 
Published: February 2008

(Latitude 13° 48′.4 S., longitude 171° 46′.5 or 11h 27m.1 W. of Gr.)April 13–15—At 11h 42m GMT, April 13, a sudden increase of 34 gammas in H marked the beginning of a disturbed period which lasted until early on April 15. The range in H was 161 gammas.
Correlation of magnetic activity with disturbance of radio transmission
Authors: McNish A. G. , Johnston H. F. 
Published: February 2008

Owing to their mutual dependence on conditions in the ionosphere a close connection between magnetic activity and radio transmission is expected. This connection is revealed by impairment of transmission on high frequencies during magnetic storms, ranging from complete failure of certain channels of communication during severe magnetic storms to minor vitiation during periods of lesser activity.The first experimental evidence on the nature of the changes taking place in the reflecting properties of the ionosphere during a magnetic storm were supplied by Hafstad and Tuve (see 1 under “References” at end of this article) in 1929. Limitations in technique at that time prevented comprehensive observation of the changes taking place. Subsequent developments in methods of ionospheric research at the Department of Terrestrial Magnetism of the Carnegie Institution of Washington and elsewhere, particularly the introduction of automatic multifrequency methods [2, 3] have afforded a clearer understanding of the phenomena.
An ionospheric investigation concerning the Lorentz polarization‐correction
Authors: Booker H. G. , Berkner L. V. 
Published: February 2008

Some years ago considerable discussion took place concerning the relation between the constitution of the ionosphere and its refractive index for radio waves. The question at issue was whether the force per unit‐charge exerted by the electric field of a radio wave upon an elementary charged particle In the ionosphere should be taken simply as the Maxwellian electric intensity E (the Sellmeyer theory), or whether there should be added a contribution (4π/3)P (the Lorentz theory). The discussion culminated in a theoretical treatment of the subject by Darwin which seemed to point to the conclusion that the Sellmeyer theory should hold good in the ionosphere at radio frequencies.For reflection from the ionosphere of radio waves of frequency less than the gyromagnetic frequency there is in middle latitudes a clear‐cut distinction in the behavior of the extraordinary wave according to the two theories. Over the past year a large number of records showing magneto‐ionic splitting of ionospheric echoes at these wave‐frequencies have been obtained. We are led to believe that it is impossible to interpret these observations in terms of the Sellmeyer theory but that no objection exists to their interpretation in terms of the Lorentz theory.On the basis of the Lorentz theory the observations indicate that there is in the E‐region of the ionosphere a level of maximum atomic and molecular ion‐density somewhat below the level of maximum electron‐density.
Radio fade‐outs at Huancayo and Watheroo Magnetic Observatories, Febraury 1937 through June 1938
Authors: Seaton S. L. 
Published: February 2008

Automatic vertical‐incidence recording of ionospheric heights has been continued at the Watheroo Magnetic Observatory, Western Australia, and at the Huancayo Magnetic Observatory, Peru, of the Department of Terrestrial Magnetism, Carnegie Institution of Washington, from the date of the last report [see 1 of “References” at end of paper] through October 1937 for Huancayo and through April 1938 for Watheroo using a fixed frequency of 4.8 mc/sec. These records have been examined and all radio fade‐outs are listed in Tables 1 and 2.From November 1937 and from May 1938 at Huancayo and Watheroo, respectively, fade‐outs were recorded by means of automatic multifrequency equipments recently installed [2] which replace the 4.8 mc/sec fixed‐frequency recording. Records are incomplete during November and December 1937 from Huancayo and during April and May 1938 from Watheroo because of installation and adjustment of the new equipments.
The construction of an azimuthal equidistant map centered about the geomagnetic North Pole
Authors: Pollak M. J. 
Published: February 2008

Before describing the construction of the accompanying map it would be appropriate to make some explanatory remarks regarding its purpose, and the particular advantages of the azimuthal equidistant projection.The map was constructed as an aid to the study of certain magnetic phenomena which take on additional significance when plotted on geomagnetic coordinates. A clear definition of this coordinate system is given by A. G. McNish:1 “Many magnetic phenomena are frequently found to have a relatively simple distribution when consideration is given to the location of the observing stations relative to the pole of the first‐degree harmonics of the Earth's general magnetic field. A coordinate system having this pole as its origin is called a system of geomagnetic coordinates.” The northern geomagnetic pole, the one used as the center of projection of the map, is in latitude 78°.5 north and longitude 69°.0 west.
Cheltenham Magnetic Observatory July to September, 1938
Authors: Ludy Albert K. 
Published: February 2008

(Latitude 38° 44′.0 N., longitude 76° 50′.5 or 5h 07m.4 W. of Gr.)July 4–5—A storm began abruptly July 4 at 12h 04m GMT, with an increase of 9 gammas in H and small changes in D and Z. The perturbations were irregular and ended at 07h, July 5. Between 20h and 24h, July 4, was the time of greatest activity. Ranges: D, 26′; H, 232 gammas; Z, 122 gammas.
The reliability of dust‐counters
Authors: Běhounek F. 
Published: February 2008

There are three types of dust‐counters commonly used: The automatic dust‐recorder and the jet dust‐counter, both devised by Dr. J.S. Owens, and the Zeiss Konimeter, based upon the same principle as the jet dust‐counter of Owens, but differing in construction. Recently an automatic device, using a photronic cell for the records, has been described by Russell A. Nielsen. Unfortunately, however, no quantitative results obtained with this apparatus are available at present.In the automatic dust‐recorder a known volume of air is filtered through white paper producing a dark spot. The degree of impurity suspended in the atmosphere is estimated by comparing the density of the dark spot with a calibrated scale of shades expressed in milligrams of suspended matter per cubic meter of air.
Apia Observatory July to December, 1938
Authors: Sapsford H. Bruce 
Published: February 2008

July 30—A short disturbance occurred on July 30. After a sudden increase of 14 gammas at 04h 35m GMT, the horizontal intensity decreased to a minimum at 08h 05m. The range of the disturbance was 157 gammas and the trace had returned to normal by the end of the day.August 3–6—Shortly after 16h GMT, August 3, the H‐trace became slightly disturbed and a sharp increase of 37 gammas occurred at 21h 35m. A period of rapid fluctuation followed. From the maximum at 21h 39m, H decreased slowly at first and then more rapidly through a range of 195 gammas to a minimum on the 4th at 09h 40m. Conditions remained slightly disturbed until the 6th. Z showed corresponding fluctuations.
Watheroo Magnetic Observatory October to December, 1938
Authors: Green J. W. 
Published: February 2008

December 9–1l—This moderate disturbance began gradually at about 12h GMT, December 9, with moderate fluctuations from 12h to 24h, December 10, and slight disturbance on December 11. Ranges, December 10: D, 17′.2; H, 54 gammas; Z, 88 gammas. Ranges, December 11: D, 18′.9; H, 60 gammas; Z, 80 gammas. Storm‐ranges: D, 19′.2; H, 100 gammas; Z, 117 gammas.December 16–23—This very moderate disturbance began at 07h 40m GMT, December 16. Its most disturbed period was from 12h to 20h, December 18, slightly disturbed conditions followed returning to normal by the close of December 23. The daily range in D was quite normal throughout the entire period, the maximum range being 19′.2, the minimum falling on December 17 and the maximum on December 18. H‐values remained low through December 22, with ranges of 82 gammas on December 17, 101 gammas on December 18, and 112 gammas on December 17–18. The ranges in Z for December 16, 17, 18, 19, 20, and 21 were 111 gammas, 103 gammas, 109 gammas, 87 gammas, 112 gammas, and 96 gammas, respectively. The range in Z for the period of the storm was 142 gammas, the maximum falling on December 18 and the minimum on December 20.
A representation of the sunspot‐cycle
Authors: Anderson C. N. 
Published: February 2008

Although sunspots had been observed occasionally back to ancient times, their study may be said to date from their rediscovery by Galileo in the spring of 1610 with the then newly invented telescope. Since then much has been written about their nature, their periodicities and possible influence on human affairs.The purpose of the study reported on in this paper was to analyze the components of the sunspot‐data and thereby to reconstruct a curve which would not only represent the variation in sunspot‐numbers from 1749 to date but would also be consistent with times of maxima and minima from 1610 to 1749. A number of attempts along this line have been made in the past [see references 3, 4, 5, 6, 7, 9, 11 at end of paper], all of which have neglected the data previous to 1749 and all have used a slightly different method of analysis. It is believed that the agreement in the present study is somewhat better than in those of the past, but nevertheless, no claim is made for any great accuracy in predicting future sunspot‐activity. Harmonic analysis based on a fraction of a period is always a source of danger and furthermore, we have no assurance that all the components of the sunspot‐curve are periodic functions [8]. In fact, some papers have appeared in which each cycle was treated as a more or less independent outburst [2, 10, 12, 13]. Nevertheless, because of the long base‐line over which agreement is obtained in this present study, it is hoped that the results may not be too much in error for at least a few cycles.
The association of radio fade‐outs with solar eruptions
Authors: Giovanelli R. G. , Higgs A. J. 
Published: February 2008

Since the announcement in 1936 that radio fade‐outs were coincident in time with solar eruptions, a large number of observations have confirmed this beyond all doubt, but whether a particular eruption will be accompanied by a fade‐out has not, hitherto, received much consideration. This question is examined in detail in the following discussion.Observations of fade‐outs at the Commonwealth Solar Observatory, Canberra, Australia, have been made since June 1937 with automatic P′ ‐ f (multifrequency) equipment. Briefly, this consists of a pulse‐transmitter, the frequency of which is automatically varied over a range from 2.3 to 12 mc/sec, and a special receiver, automatically tuned to the frequency of the transmitter. The complete cycle of operations is repeated, in the present instrument, every six minutes, while in the first instrument, which was in use until April 1938, the period was made five or fifteen minutes according to the solar activity. The signals picked up by the receiver are delineated, finally, on the screen of a cathode‐ray oscillograph where the “ground‐wave” and reflections, or “echoes,” from the E‐ and F‐regions of the ionosphere are separated. The resulting quasi‐stationary picture is photographed on a moving film. For the purposes of this paper a fade‐out is defined as a period during which no reflections from the E‐region can be seen; a “severe” fade‐out is one in which, in addition, no echoes from the F‐region are visible, while a “minor” fade‐out is one in which some F‐region echoes, though weakened, are present. It should be emphasized that this criterion for a fade‐out is not absolute and refers particularly to the special transmitter and receiver used in the investigation, though it is worth pointing out that such fade‐outs observed here invariably coincide with periods of severe disturbance to commercial radio services.
Huancayo Magnetic Observatory January to March, 1939
Authors: Davies Frank T. 
Published: February 2008

January 5—A sudden commencement occurred at 04h 09m GMT, January 5. During a period of seven minutes D moved westerly 0′.6, H decreased 50 gammas, and Z decreased 7 gammas. Moderate disturbance continued until 21h.January 21—From 13h to 21h GMT, January 21, several fluctuations of large amplitude occurred in horizontal intensity. There was an unusually low value of 29491 gammas in horizontal intensity at 18h 36m.
On prediction and mutual correlations of the maps of distribution of magnetic elements and their annual changes
Authors: Weinberg B. P. 
Published: February 2008

For theoretical investigations, as well as for practical purposes, it is important to find a possible way to predict the distribution of the isolines of the magnetic elements and of their isopors and also of controlling one such distribution by means of another one.These two possibilities are given by equations (1), (2), and (3).
Sitka Magnetic Observatory April to June, 1939
Authors: Gebhardt Robert E. 
Published: February 2008

April 16–17—A severe magnetic storm began with abrupt movements of all elements at 21h 28m GMT, April 16, and at 0lh 57m, April 17. Thereafter the storm increased rapidly with large bays and short‐period vibrations. The storm ended about 23h GMT, April 17; but the trace remained moderately disturbed for several days. Ranges: D, 238″; H, 1569 gammas; Z, 910 gammas.April 23—A moderate disturbance of large bays, began gradually and was followed by an abrupt motion of the elements at 05h 52m GMT, April 23. After the 15th hour the disturbance gradually subsided and ended about 02h, April 24. The H‐maximum was too great to be recorded. Ranges: D, 158″; H, 1304 gammas (estimated); Z, 590 gammas.
TUCSON MAGNETIC OBSERVATORY APRIL TO JUNE, 1939
Authors: Hershberger John 
Published: February 2008

April 16–17—After an unimportant‐looking beginning at 21h 28m GMT, April 16, a real storm began sharply at Olh 56m, April 17, with a sudden increase in H of 71 gammas, followed within a few hours by an irregular drop of 250 gammas, which was 10 gammas less than the range in H for the storm. The fluctuations continued large but diminishing until 24h, April 17, when the storm appeared to be over except for a low H, However, the traces remained moderately disturbed for a number of days, and had not completely quieted down when the next storm struck.April 23—This storm began very sharply at 05h 44m GMT, April 23, with an upward jump of 110 gammas in H and smaller changes in the other elements. In a little more than an hour afterward, H had dropped 180 gammas, the range for the storm. At 16h the perturbations became less violent, and within a few hours the storm had gradually ended.
Alibag Magnetic Observatory January to June, 1939
Authors: Chaudhuri D. L. , Rangaswami M. R. 
Published: February 2008

February 1–2—;A moderate disturbance began at about 07h GMT, February 1. H reached a minimum value at 20h 08m, February 1, and the storm ended at 10, February 2. Ranges: D, 5″.3; H, 114 gammas; Z, 29 gammas.February 6–7—A storm of great intensity began at about 04h 43m GMT, February 6. H began to fall rapidly from 08h 54m, February 6, and reached a minimum value at 13h 20m, February 6. Two prominent humps were recorded between 13h.5 and 15h and between 16h and 17h. The storm practically ended at 01h.5, February 7. Ranges: D, 7″.1; H, 196 gammas; Z, 53 gammas.
Huancayo Magnetic Observatory April to June, 1939
Authors: Davies Frank T. 
Published: February 2008

April 4—The period from 20h to 22h GMT, April 4, was moderately disturbed. H had a low value.April 16—A sudden commencement occurred at 21h 29m GMT, April 16, in H and Z. During a period of five minutes H increased 40 gammas and Z increased 7 gammas. The trace was quiet afterwards.
Padre Luis Rodés, S.J., 1881–1939
Authors: Macelwane J. B. 
Published: February 2008

In the death of Father Louis Rodés, June 7, 1939, at Biniaraix on the Island of Majorca, the Observatory of the Ebro lost its capable director and geophysicists throughout the world an esteemed colleague and friend.Louis Rodés was born at Santa Coloma de Farnés, Spain, December 31, 1881. At the age of sixteen he entered the Society of Jesus. After two years of novitiate at Gandia and seven years of brilliantly successful classical, scientific, and philosophical studies at Saragossa and Tortosa he matriculated in the Faculty of Science of the University of Barcelona. While at the University during the years 1906–1910 he filled with distinction the post of Professor of Physics in the Jesuit College of Sarriá.