bluuebunny/crossref_metadata_2025_split huggingface dataset:
Agenda for the Warsaw Meeting of the International Commission of Terrestrial Magnetism and Atmospheric Electricity, September 1935
Authors: la Cour D. 
Published: February 2008

Following the call of President Maurain the first session of the Commission will take place at Warsaw September 2, 1935, at 10 a. m. in the Staszic Palace, Nowy Swiat 72 (entrance by main door facing Copernik Place).Professor Kalinowski has kindly invited the members of the Commission to visit the Swider Observatory, near Warsaw. Since a general excursion to the Jablonna Meteorological Observatory is scheduled for September 8, it is recommended that those present at Warsaw September 1, visit Swider on that day. Information as to the time of departure for Swider will be posted at the Bureau of the Conference.
Electricity of rain and thunderstorms
Authors: Simpson G. C. 
Published: February 2008

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

(Latitude 12° 02′.7 S., longitude 75° 20′.4 or 5h 01m.4 W. of Gr.)April 10—The disturbance which began at 12h 37m April 10 was of a minor nature with a short life. It affected the H‐trace principally, interposing large bays with an approximate period of 30 minutes. The most rapid change was in the 10‐minute period beginning at 16h 32m. During this interval the horizontal intensity increased 112 gammas.
American URSI broadcasts of cosmic data October to December, 1935
Authors: Ennis C. C. 
Published: February 2008

The data for terrestrial magnetism, sunspots, solar constant, and auroræ are the same as given in previous tables.The first three columns of the Table give (1) the magnetic character according to the scale 0–2 of the International Commission of Terrestrial Magnetism and 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 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 0.7.
Harmonic analysis by means of linear combinations of ordinates (Concluded)
Authors: Labrouste H. , Labrouste Mrs. 
Published: February 2008

Multiple combinations and curve definitions§20. We have seen that simple and compound combinations permit suppressing or reducing greatly certain sine‐waves while they amplify others, but they are generally insufficient to isolate the diverse elementary components which are present in a curve.Multiple combinations (or combinations of combinations), that is, a succession of combinations, must be used: The first one, made on the given curveC, gives a transformed curveC′, the second one, made onC′ gives a new transformed curveC′′, etc. We represent them by a symbolical product, so as to bring under notice the fact that the magnification‐factor is equal to the product of the magnification‐factors of the successive combinations and that it is possible to interchange the order of the combinations in the same way as it is possible to interchange the order of the factors in a product.
The New Observatory at San Miguel, Argentina
Authors: Puig Ignacio 
Published: February 2008

On December 12, 1935, a cosmic‐physical Observatory was inaugurated in the San Miguel District, on the Pacific Railway Line about 30 kilometers from the center of Buenos Aires. The President of the Republic together with the Ministers of Public Instruction and of Agriculture were present on that occasion.The new Observatory, although belonging to the Society of Jesus and directed by its members, has been founded through the initiative of the National Council of Observatories and is invested with an official character.
On the auroral spectrograms taken at Chesterfield, Canada, during 1932–33
Authors: Currie B. W. , Edwards H. W. 
Published: February 2008

This is a study of 693 spectrograms of the auroral and the night‐sky light that were taken at Chesterfield during the International Polar Year. The spectrograms had been obtained with successive exposures of about 1.5 hours throughout each night. In addition to presenting spectrographic pictures of the variations in auroral activity throughout each night they showed the effect of twilight and of moonlight on the auroral radiations.The radiations that appeared on the spectrograms are identified with reasonable certainty, and their frequencies of occurrence are computed. Evidence is presented to show that the radiations from the upper atmosphere at Chesterfield are characteristically auroral at all times, and that the green‐line luminescence of the night‐sky at lower latitudes does not occur continuously at Chesterfield. A comparison is made between the frequencies of occurrence and the intensities of the two red‐radiations on moonlight nights and on dark nights to show the effect of moonlight on these radiations. Similar effects are shown to occur during twilight‐periods.The possibility of using spectrographic observations to deduce auroral character‐numbers is indicated. The mean nightly variation in the intensity of the aurora for 30 clear nights is deduced from the apparent changes in the intensity of 5577Å, of 3914Å, and of all the radiations appearing on the spectrograms, and is compared with the mean nightly variation as deduced from the visual observations. The appearance of the radiation 3578Å (as an indicator of bright, active aurora), is used to find the mean nightly variation in auroral activity during the winter. The mean nightly variation in auroral activity is compared with the mean diurnal ranges of the earth‐potential and of the magnetic declination used as indicators of earth‐current and magnetic activity, respectively.
The new San Miguel cosmophysical observatory
Authors: Puig Ignacio 
Published: February 2008

On December 12, 1935, the new cosmophysical observatory at San Miguel, about 30 kilometers from Buenos Aires, Argentina, was formally inagurated in the presence of the President of the Republic and other officials (see Plate 3 in which the lower view was made during the inaugural ceremonies, December 12, 1935). The National Committee on Observatories extended its patronage and has invested the Observatory with an official character although it is the property of a private organization—the Society of Jesus.The complete program of this Observatory is similar to that of the Observatory of the Ebro in Spain. It embraces the study of solar and cosmic phenomena and their relations with terrestrial phenomena, particularly those of magnetism and electricity. The work will be distributed among three sections—Geophysical, Electrometeorological, and Astrophysical. The Geophysical Section will investigate terrestrial magnetism, earth‐currents, and earthquakes; the Electrometeorological Section will investigate Hertzian waves, electrical potential, ionization, and radioactivity of the atmosphere; the Astrophysical Section will concern itself with phenomena connected with solar activity and cosmic rays.
Solar and magnetic character‐figures, Mount Wilson Observatory April, May, and June, 1936
Authors: Nicholson Seth B. , Sternberg Elizabeth E. 
Published: February 2008

The bright hydrogen eruption of April 8 which was simultaneously accompanied by a major radio fade‐out occurred in a group situated in latitude north 20° and longitude west 8°. The horizontal intensity at Mount Wilson decreased suddenly by 12 gammas at 16h 45m, GCT. No magnetic storm followed and it is quite probable that the relation between this solar eruption and the disturbance in the Earth's magnetic field is very different from that which exists between solar activity and ordinary magnetic storms.1An oscillation of about 120 gammas occurred between 5h and 6h April 18. Irregular oscillations from April 19 to 24 were probably caused by an active region in the southern hemisphere which crossed the central meridian from April 21 to 23.
Magnetic station at Cape Chelyuskin
Authors: Harradon H. D. 
Published: February 2008

In view of the importance of continued registrations of the magnetic elements in the arctic regions, it is pleasing to note in a recent number of the Bulletin of the Arctic Institute that the Polar Station established by that Institute on Cape Chelyuskin in 1932 was considerably enlarged in 1934, the staff consisting of 32 men under the direction of I. D. Papanin. In addition to dwelling‐houses and technical buildings, there were erected a pavilion for variation‐instruments with a room for absolute control‐measurements, a pavilion for atmospheric‐electric observations, and a number of other buildings for meteorological, hydrological, and other purposes.The atmospheric‐electric investigations were conducted by V. I. Gerassimivich who had specialized in that work. During the winter of 1934–35, he succeeded in obtaining a continuous record of the potential gradient using a Benndorf recording‐electrometer in which a number of alterations has been made to adapt it to polar conditions. The necessary absolute determinations were made for control of the registrations. A second Benndorf instrument was arranged for continuous registration of the electric conductivity of the atmosphere.
Sitka Magnetic Observatory April to June, 1936
Authors: Burke R. G. 
Published: February 2008

(Latitude 57° 03′.0 N., longitude 135° 20′.1 or 9h 0lm.3 W. of Gr.)April 18–22—This storm was a drawn‐out disturbance but of no great violence at any one time. It began at 2h GMT, April 18, and ended about 17h, April 22, with extremes ranging from the beginning to the end, of 88′.6 in D, 980 gammas in H, and 594 gammas in Z. There were irregular pulsations and bays throughout with more disturbed periods from 4h to 8h on April 18, from 12h to 16h on April 20, and from 7h on April 21 to 17h on April 22.
Tucson Magnetic Observatory April to June, 1936
Authors: Joyce J. Wallace 
Published: February 2008

(Latitude 32° 14′.8 N., longitude 110° 50′.1 or 7h 23m.3 W. of Gr.)April 17–24—A moderate disturbance began gradually at about 21h GMT April 17. At 5h April 18, H and D, and to a lesser degree, Z, went to sudden peaks and then subsided again all within a little over an hour. During this short interval, the following ranges were recorded: Horizontal intensity, 133 gammas; vertical intensity, 19 gammas; declination, 16′. The remainder of the storm was a series of very long, gradual bays, with intervals of superimposed short‐period activity. Total ranges were: Horizontal intensity, 176 gammas; vertical intensity, 59 gammas; declination 24′. The storm ended about 7h April 24.
Note on magnetic conditions June 18–20, 1936
Authors: Johnston H. F. 
Published: February 2008

This short description of magnetic conditions existing during the total solar eclipse of June 19, 1936, is based upon a radio report from Watheroo Magnetic Observatory, upon magnetograms from the Huancayo Magnetic Observatory, both operated by the Department of Terrestrial Magnetism of the Carnegie Institution of Washington, and upon copies of magnetograms from the observatories at Cheltenham, Tucson, San Juan, and Honolulu kindly furnished by the United States Coast and Geodetic Survey.The total eclipse of June 19, 1936 began at 2h.9 GMT, and ended at 7h.9. A magnetic disturbance blanketed the total eclipse‐period. It began at 9h.7, June 18, and lasted until approximately 7h June 20. This magnetic disturbance was a magnified reappearance of a minor disturbance which had affected the magnetic elements at various multiples of 27 days previously, namely, March 24–28, April 21–25, and May 18–22.
Sitka Magnetic Observatory July to September, 1936
Authors: Hershberger John 
Published: February 2008

(Latitude 57° 03′.0 N., longitude 135° 20′.1 or 9h 01m.3 W. of Gr.)July 2—A storm began about 7h 30m GMT, July 2, although the elements had been slightly disturbed for some hours previous to this time. East declination increased 42′ in about half an hour, and the vertical intensity decreased nearly 300 gammas in less than an hour, while the horizontal intensity gradually decreased 824 gammas in five hours. All the elements fluctuated moderately until about 11h, when the oscillations became quite violent, continuing so until 16h, During the next hour they resumed their normal values, and by 17h the storm was over. Ranges: Declination, 115′; horizontal intensity, 824 gammas; vertical intensity, 669 gammas.
Apia Observatory April to September, 1936
Authors: Baird H. F. 
Published: February 2008

(Latitude 13° 48′.4 S., longitude 171° 46′.5 or 11h 27m.1 W. of Gr.)June 18–20—A fairly intense magnetic disturbance seems to have commenced with a sudden rise in H of only 6 gammas at 9h 40m GMT, June 18. The H‐trace was then slightly disturbed rising gradually to a maximum at 18d 20h 15m and then declining slowly until 18d 23h 10m when a sudden fall of 29 gammas in H introduced a very disturbed trace. H then fell rapidly to a minimum at 19d 07h 40m rising again gradually and remaining disturbed throughout June 19 and 20. D and Z also showed very disturbed traces over the period. The total range of the disturbance in H was 218 gammas.
Huancayo Magnetic Observatory July to October, 1936
Authors: Torreson O. W. 
Published: February 2008

(Latitude 12° 02′.7 S., longitude 75° 20′.4 or 5h 01m.4 W. of Gr.)July 2—A brief disturbance occurred July 2 with an abrupt movement in H and Z but not in D. H decreased 41 gammas in seven minutes while Z decreased seven gammas in the same interval. The disturbance is chiefly notable for the depressed values of H between 9h and 17h GMT, the minimum in H for the day occurring about the middle of this period at 13h 34m with the low value of H of approximately 29450 gammas. D and Z were somewhat more variable than usual during this disturbance.
Sitka Magnetic Observatory, October to December 1937
Authors: Gebhardt Robert E. 
Published: February 2008

(Latitude 57° 03′.0 N., longitude 135° 20′.l or 9h 01m.3 W. of Gr.)September 30–October 1—A slight magnetic disturbance began abruptly at 13h 46m GMT, September 30, with a sudden increase of 40 gammas in H and a decrease of 8′ in east declination. The elements were mildy disturbed with short‐period vibrations superimposed on irregular oscillations until about 24h GMT, October 1. Ranges: D, 62′; H, 437 gammas; Z, 437 gammas.
Some atmospheric‐electric observations at Poona
Authors: Sil J. M. 
Published: February 2008

A continuous record of the Earth's electric field has been obtained at Poona since September 1930. Since 1935 arrangements were also made to take systematic measurements of the conductivity as well as of the dust, nuclei, and ionic contents of the air simultaneously at some appointed hour. In this preliminary report, all observations cover a period from 1935 to 1937 except those on potential‐gradient which are from September 1930 to November 1937.Poona is a rocky place, situated on a plateau formed on the eastern side of the chain of mountains, called the Western Ghats. Its position is latitude 18° 30′ north, longtitude 73° 53′ east, and its height above mean sea‐level is 1830 feet. It is not an industrial center. During afternoons in summer, a cool sea‐breeze blows from the Arabian Sea and raises a fairly good amount of dust. During the monsoon season (July to September) the sky is almost overcast on most of the days although it rains only occasionally. During September and October there are frequent thunderstorms. During winter (November to February) a strong inversion of temperature occurs almost every evening, followed sometimes by moderate haze or fog in the early morning. Considering the above it will be clear that the number of undisturbed days in a year is very small and observations extending over a long period, therefore, are necessary for the collection of sufficiently reliable data.
American URSI broadcasts of cosmic data, January to March 1938, with American magnetic character‐figure CA, February to April 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. 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 the mean value of k for Mount Wilson was 0.53 during 1936; during 1937 this value varied from 0.47 to 0.66 with an average value of 0.53.
Asymmetrical characteristics of the Earth's magnetic disturbance‐field
Authors: Vestine E. H. 
Published: February 2008

Asymmetries in the Earth's magnetic disturbance‐field are considered in relation to the asymmetries in the Earth's main field, using data of 32 stations. The auroral‐zone curve of terrestrial magnetism, in north polar regions, is elongated in a direction roughly parallel to the elongation of Hsoclinic curves. It agrees roughly with the curve of maximum auroral frequency, as given by Fritz, except in regions where his auroral data were scanty. The curve appears to undergo regionally a small diurnal oscillation.The amplitude of the disturbance diurnal variation (SD) is approximately symmetrical with respect to the geographical equator in low latitudes, is zonal‐symmetrical with respect to the auroral zone, and has a zero vertical component near the north pole given by the eccentric dipole. No change in amplitude with longitude has been detected, and it is concluded that induced earth‐currents in the oceans contribute little to SD.The local time‐phase of the mainly sinusoidal variation SD shows a range of about four hours with longitude. But if in defining time the geographic north pole be replaced by the north pole given by the eccentric dipole, then at the auroral zone there is no significant variation in time‐phase with longitude. This suggests that the auroral zone has a controlling and initiating influence over the world‐wide electric currents responsible for SD.Average asymmetries in the geographical distribution of magnetic disturbance and aurora are compared. The average force‐vectors for the daily means of disturbance are perpendicular to the average directions of homogeneous auroral arcs, to a high degree of approximation, in polar regions.The SD electric current‐system of magnetic storms proposed by Chapman shows good general agreement with the extensive data here considered. Certain changes are suggested whereby the fit with observation may be improved.
Preliminary results of magnetic measurements at the “North Pole” station
Authors: Fedorov E. 
Published: February 2008

We took magnetic measurements with the aid of a theodolite and also diurnal series of measurements of the magnetic variations using special visual magnetometers. A total of 55 measurements of declination and of horizontal intensity and 36 measurements of inclination were made.Up to the middle of November, 1937, 14 diurnal series of measurements of variation were made, but later the ice‐floe began to turn around hindering the use of the variometers. As a result of measurement of the variations it was observed that the declination had an average diurnal value at about 6h, 13h, and 0h, GMT; between 6h and 13h the deviation was to the east, between 13h and 0h to the west, and between 0h and 6h a little to the east; these characteristics persisted in all cases. The amplitude ranged from 2° on quiet days to 10° on disturbed days. The horizontal intensity had an average diurnal value at about 6h, 10h, and 18h; a small maximum was observed from 6h to 10h, a large minimum from 10h to 18h, and a large maximum from 18h to 6h. In the main this character persisted. The amplitude ranged from 150 to 500 gammas.
Sitka Magnetic Observatory, April to June 1938
Authors: Gebhardt Robert E. 
Published: February 2008

(Latitude 57° 03′.0 N., longitude 135° 20′.1 or 9h 01m.3 W. of Gr.)April 13–15—A moderate magnetic storm began gradually at about 11h 42m GMT, April 13, with an increase in the horizontal intensity and decreases in the vertical intensity and east declination. The storminess gradually increased with short‐period vibrations superimposed on a long‐period motion. At 05h 26m, April 14, there was a sudden decrease in the horizontal intensity of 600 gammas accompanied by similar changes in the vertical intensity and declination. After 09h, April 14, the storm gradually subsided; the traces reaching normal values at 04h, April 15. Ranges: D, 102′; H, 1285 gammas; Z, 371 gammas.
Data for absolute storminess for the polar station Gjöahavn for the year of 1904
Authors: Wasserfall K. F. 
Published: February 2008

Roald Amundsen took a set of Eschenhagen variation‐instruments for use on the Gjöa Expedition during 1903 to 1906 and at his base station Gjöahavn (latitude 68° 37′.6 north and longitude 95° 54′.8 west). That station was occupied from November 1903 to May 1905; hence almost complete hourly data for D, H, and V could be published for that period.When the results from the expedition were published,1 there was no opportunity to undertake special studies of the variation of the magnetic elements, because the data collected were so abundant that publication had to be limited to the hourly values for the three elements D, H, and V. It has seemed, however, worth while to make further use of these valuable data and the present paper represents one of the special variation‐studies based thereon.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory July, August, and September, 1938
Authors: Mulders Elizabeth Sternberg , Nicholson Seth B. 
Published: February 2008

The storm of July 15–17 and that of August 11 were probably associated with the very large and active group which crossed the central meridian on July 15.1 and again on August 10.9.The storms of September 26 and 27–28 were probably associated with two active groups which crossed the central meridian on September 25.6 and 28.0.