bluuebunny/crossref_metadata_2025_split huggingface dataset:
Magnetic storm of October 14–16, 1926, as recorded at the Cheltenham Magnetic Observatory
Authors: Hartnell George 
Published: February 2008

(Greenwich Civil Mean Time.)The principal portion of the storm began at 21h, October 14, and ended at 5h, October 16. From 17h to 21h on October 15 the motion of the magnets was so rapid that only at turning and halting points was a legible record made on the magnetogram. This was the period during which there was interference with the operation of telegraph lines. The amplitudes of the variations were as follows: Declination, 57′.1; horizontal intensity, 419γ; vertical intensity, about 730γ; (the Z spot went below the limits of the paper twice between 7h and 9h on October 15.)
Principal magnetic storms recorded at the Huancayo Magnetic Observatory, October to December, 1926
Authors: Goddard R. H. 
Published: February 2008

(Lat. 12° 02′.7 S.; long. 75° 20′.4 W. or 5h 01m W. of Gr.)October 13–16, 1926.—This magnetic storm was of unusual violence. The time of commencement is not easily assigned, but the first movement of note occurred at 11h 36m on October 13, when the horizontal‐intensity trace showed a sudden increase in that component of 3γ, followed immediately by a more leisurely decrease amounting to about 35γ, this occupying a period of 15 minutes of time. The declination trace showed a fairly sudden easterly movement of about one minute of arc at this time, while the vertical component increased slightly but at a slower rate. The next phase occurred at 19h 24m on the same day, when the horizontal component increased within six minutes of time by 56γ (or 0.00187H). The declination trace showed the characteristic sudden westerly movement and the vertical component the corresponding sudden increase within the same interval of time. This movement, in fact, might well be considered the true commencement of the disturbance. The traces during the ensuing 22 hours were composed of moderately irregular fluctuations, but followed, in the main, the usual curves of diurnal variation. At 19h on October 14 the horizontal component began to decrease rapidly, passing off the lower extremity of the paper at 22h. At Greenwich midnight the trace was taken off and developed as usual, and the horizontal‐intensity spot was returned to the paper by decreasing the torsion of the suspending fiber. From this time the fluctuations were very rapid and irregular. The maximum violence occurred between 12h and 20h on October 15. The movements of the horizontal‐intensity magnet were, at times during this period, too rapid for definite registration. The declination and vertical‐intensity traces, particularly at 14h 15m and 15h 30m on October 15, showed remarkable fluctuations, both as regards rapidity and amplitude. One outstanding variation in the horizontal component was recorded at 18h 20m on October 15, when the intensity within the ensuing seven minutes decreased by 340γ, or more than one per cent of the average horizontal‐intensity value at Huancayo (0.297 C.G.S.). At 22h 45m the horizontal‐intensity trace again passed the lower limits of registration and was brought into view one hour later by the same means as before. By 4h on October 16 the traces had resumed their normal character, the value of horizontal intensity, however, being still distinctly sub‐normal.
Die periodische Schwankungen def. Sonnenflecken und der magnetischen Kraft
Authors: Schostakowitsch Von W. B. 
Published: February 2008

Ich habe in meinen zwei Abhandlungen, welche sich jetzt im Druck befinden (Meteor. Zeitung.) gezeigt, dass man in der Sonnenflecken ausser der längs bekannten 11‐jährigen Periode noch folgende drei: von 33.1, 5.8, und 3.2 Jahren, nachweisen kann. Diese vier Perioden legen auf einander auf und die wirklich beobachtete Sonnenfleckenerscheinung, welche durch die Wolfer'schen Relativzahlen ausgedrückt ist, stellt das Resultat der Zusammenwirkung aller Perioden dar.Ich habe weiter in dem sekulären Gang der verschiedenen Klimaelementen: Radiation, Luftdruck, Lufttemperatur, Niederschläge und auch einiger geophysikalischen Erscheinungen, welche von dem Klima abhängig sind, z. B. Niveauschwankungen der Flüsse and Seen, Schwankungen der Eismenge bei Island und bei Grönland, dieselben Perioden nachgewiesen und gezeigt, dass alle diese Erscheinungen durch die Sonnenflecken beeinflusst sind und dieselbe Periodicität besitzen.
Remarques à propos des mesures magnétiques de M. Parkinson et des formules des variations séculaires à Tunis
Authors: Palazzo Luigi 
Published: February 2008

En examinant le Vol. VI des Researches of the Department of Terrestrial Magnetism, “Land Magnetic and Electric Observations, 1918–1926,” j'ai vu, entre autres choses, que des mesures magnétiques ont été faites par l'observateur M. Parkinson dans la “Repeat” station de Tunis en février 1922. Moi aussi, j'ai fait itérativement des déterminations magnétiques à Tunis, et la dernière fois fut en octobre 1923; après cela j'ai entrepris l'étude des variations séculaires à Tunis, en publiant une note intitulée: “Variazioni magnetiche secolari a Tunisi, Cartagine e Malta” (Mem della Pontif. Accademia delle Scienze Nuovi Lincei, Vol. VIII, 1924–1925). J'avais aussi calculé, sur la base de toutes les observations dont je possédais alors les valeurs (Denza 1877.8, Teisserenc de Bort 1883, Moureaux 1887.4, Palazzo 1896.6, Sligh 1911.9, Palazzo 1923.9) et par l'application de la méthode des moindres carrés, les formules suivantes représentant la marche séculaire de D et H: D = 10° 21′.9 − 6′.06t − 0′.055t2H = (25691 + 15.7t − 0.506t2)γoù t est l'an compté à partir de 1900.
Principal magnetic storms recorded at the Cheltenham Magnetic Observatory, January to May, 1928
Authors: Hartnell G. 
Published: February 2008

(Latitude 38° 44′.0 N.; longitude 76° 50′.5 or 5h 07m.4 W. of Gr.)March 11, 1928—There was a moderate disturbance beginning March 11 at 10h which ended at 4h on March 12.
Ozone in the northern and southern hemispheres
Authors: Fowle F. E. 
Published: February 2008

Measuring the output of radiation from the Sun encounters greater difficulties when attempted in the northern hemisphere (Mt. Wilson, Harqua Hala, Table Mountain) than in the southern (Calama and Montezuma, Chile). May not this be due to some asymmetry between atmospheric conditions above these two sets of stations which spoils the apparently excellent skies of such a station as Table Mountain, California?Supposing that something coming from the Sun causes a change in the upper air, either in the form of electric particles or as ionization due to ultra‐violet light, then the resulting particles, electrically polarized, under the influence of the Earth's magnetic field, might very probably drift unsymmetrically toward one of the poles of the Earth.
Relative sunspot‐numbers for the central zone of the sun's disc for the 11‐year period 1917 to 1927
Authors: Brunner W. 
Published: February 2008

For the purpose of studying the relationship between terrestrial and solar phenomena particularly with regard to terrestrial phenomena which appear to depend upon corpuscular emissions projected from the Sun in limited streams, it may be interesting to have the daily relative sunspot‐numbers not only for the whole disc but also for a certain central sector nearer the line joining the center of the Sun and the Earth.The following tables give the relative sunspot‐numbers for a central zone equal to a circular surface of the semi‐diameter of the Sun's disc. A spot passing near the center of the disc takes from the east to the west end of the central zone a little more than four days. The numbers given are dependent alone on observations at Zürich Observatory made during 1917 to 1926 by A. Wolfer and during 1926 to 1927 by W. Brunner.
Sitka Magnetic Observatory July to September, 1928
Authors: Ulrich F. P. 
Published: February 2008

(Latitude 57° 03′.1 N.; longitude 135° 20.1′ or 9h 01.3m W. of Gr.)July 7–10, 1928—This storm was one of the most active ever recorded at the Sitka Observatory. It began at 23h 13m with the magnetic elements more or less active for several hours before that time. From 23h 13m, July 7, to 23h 44m rapid oscillations occurred in D and H while the fluctuations in Z were much smaller. At the latter time all of the elements began changing irregularly and fast and from then on the record was an almost unintelligible mass of faint lines and dots. With only occasional places where some of the elements can be identified this continued until 14h on July 8. At that time the H reserve‐spot came back on the magnetogram after being off a considerable portion of the storm, while for several hours the Z, H, and D reserve‐spots were moving almost entirely across the magnetogram. The main features of the storm were the unusually low values of H during most of the period of greatest activity; the abnormally high values of Z during the first part of the storm, going beyond the edge of the magnetogram a number of times, with unusually large and fast oscillations in the latter part of the storm, and the unusually low values of D.
In tribute to the memory of James Percy Ault
Authors: Fisk H. W. 
Published: February 2008

Throughout the record of achievement of the Carnegie on all oceans runs the reflected personality of the man who has been associated with her from the beginning, and who, for the past fifteen years, has been her commander.His service under his predecessor, first on the Galilee, then on the early cruises of the Carnegie, prepared him for the responsibility, but Nature gave him the qualities of heart and mind essential to successful leadership.
Sitka Magnetic Observatory, April to September, 1929
Authors: Ulrich Franklin P. 
Published: February 2008

During the quarter April to June there were no magnetic storms of sufficient intensity or unusual characteristics to warrant reproduction. While the storm of April 15–17 shows a large range in the horizontal intensity it is not a large or active storm. This large range is caused by an abnormally large but slow increase at one time and about ten hours later by an abnormally large and slow decrease.There were no particularly large magnetic storms during the third quarter.
The relation of space‐charge and potential gradient to the diurnal system of convection in the lower atmosphere
Authors: Brown Joseph G. 
Published: February 2008

The mean electric field of the Earth is characterized by a negative surface‐charge and a positive space‐charge in the atmosphere. The mean distribution of the positive space‐charge can be inferred from the values of the potential gradient at different elevations, since d2V/dh2 = −4πρ. Approximate computation shows that 50 per cent of the charge is in the first kilometer. Variations in distribution will cause variations in potential gradient at any point by changing the relative magnitude of the spacer‐charge (a) in horizontal layers and (b) in vertical columns. Expansions or contractions and convection‐currents will produce such changes in distribution and hence determine the character of changes in potential gradient.Continuous records of space‐charge and potential gradient have been obtained for a year 7.5 meters above the ground and their diurnal variations have been compared with the diurnal system of convection as inferred from the variation in the meteorological elements. It is concluded that for this set of records the diurnal variation of the potential gradient is satisfactorily accounted for on this theory.
Earth‐resistivity survey at Huancayo, Peru
Authors: Rooney W. J. , Gish O. H. 
Published: February 2008

This survey, carried out near the Huancayo (Peru) Magnetic Observatory of the Department of Terrestrial Magnetism of the Carnegie Institution of Washington in the high Andes, is one of a series of earth‐resistivity surveys made in connection with the study of earth‐currents at observatories where potential‐gradient registration is in progress. The general resistivity of the region and its variation with position, depth, direction of current‐flow, and rainfall, were determined. All may affect potential records and are indicative of the geological structure.The resistivity of soil near the surface varied from over 100,000 to less than 2,000 ohm‐cm, depending on the character of the overburden. The mean values tended to converge to a value around 10,000 ohm‐cm as earth to depths of 200 to 300 meters was included in the measurements. These results are typical for an underlying structure of sedimentary rocks. A local area of high resistivity (values three times the mean for the region as a whole) was found near one earth‐current line and explains the high potential‐gradient records obtained from that line. The results were found to be independent of the orientation of the survey‐lines, indicating that the region is laterally isotropic. The seasonal variation was small and relatively unimportant.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, February and March, 1930
Authors: Nicholson Seth B. 
Published: February 2008

The greatest activity in the Earth's magnetic field during February was between the twelfth and eighteenth. No extreme solar activity was observed at that time although there were bright hydrogen flocculi connected with three groups which on February 12 were 60° west, 25° west, and 20° east of the central meridian, respectively.In March moderate activity was recorded between the twelfth and fifteenth when the large spot‐tream consisting of two groups was crossing the Sun's central meridian. No exceptional activity was observed in the hydrogen flocculi during this storm.
Earth‐movements and terrestrial magnetic‐variations
Authors: Gunn Ross 
Published: February 2008

It is shown that a general contraction of the Earth or a movement of a small part of it may give rise to appreciable disturbing magnetic fields. The movement of a conducting region inside the Earth across the Earth's magnetic field sets up electromotive forces which may produce large current‐systems. These current‐systems can give rise to the observed magnetic variations if the conductivity of the earth's core is sufficiently large.Earlier determinations of the resistivity of the Earth's core are found to be to several orders of magnitude too high, due to the neglect of skin‐effects. It seems probable that the electrical time‐constant of the Earth's core is not less than 1,000 years, and therefore magnetic diurnal‐variation data cannot be used to calculate its conductivity.
Huancayo Magnetic Observatory June to September, 1930
Authors: Forbush Scott E. , Ledig Paul G. 
Published: February 2008

(Latitude 12° 02′.7 S.; longitude 75° 20′.4 or 5h 01m W. of Gr.)Although the mean of the characters for the month was quite low (0.2) there were few traces without small disturbances. Attention is directed to disturbances at about 5h 20m 75° M. T. on the magnetogram for June 25 and again at about 16h 22m on the same date which must be attributed to earthquakes since simultaneous disturbances of the same character were noticed on the potential‐gradient traces and the latter disturbance was also very marked on the conductivity trace, having apparently caused the “B” conductivity light to go out.
Apia Observatory
Authors: Westland C. J. 
Published: February 2008

(Latitude, 13° 48′ S.; longitude, 171° 46′ or 11h 27m.1 W. of Gr.)The H‐trace showed a sharp deflection upward July 9, 14h 54m. This amounted to 17γ and subsequent rises brought it to maximum 68γ higher than at time of deflection at 19h 50m. The minimum at 10d 9h 49m was about. 140γ below the maximum. Z had a sharp deflection upward, 7γ, at same time as H. The maximum was between 18h and 19h, and the minimum between 3h and 4h on July 10—range about 30γ. There was no disturbance in D.
Additional notes on observations of magnetic anomalies with a variometer
Authors: Koenigsberger J. G. 
Published: February 2008

Referring to my article in the preceding number of this JOURNAL (pp. 243–249), I have pleasure in sending herewith a graph with another abscissæ‐axis to take the place of Figure 5; this now is a projection on a north‐south line and shows further and improved analysis as regards part of the line of the magnetic profile through the Black Forest, the Swiss Jura, and the Swiss Alps, including the additional observations obtained (and summarized in Table 1 of the previous communication) to extend it to Lago di Lugano and Chiasso in Italy.The curvatures of the profiles for the differences of H and Z against the normal values as shown in the Figure herewith indicate the depth of the center of the disturbing rock on the first 25 km of the line to be about 7 to 12 km between kilometers 15 and 20 for the principal anomaly, and that of a second anomaly to be about 5 km in the same region between kilometers 15 and 20—more probably caused by intrusive basic rocks than tectonics. The same or similar anomaly was detected on the other side of the Rhine (Alsatia, France) by J. Jung and C. Alexanian [Ann. Office Nation. Combustibles Liquides, 6, 43–58 (1931)]. Anomalies having depths of centers about 5 km are indicated at kilometer 100 and at kilometer 150, and another center of depth more than 10 km at kilometer 200, as well as indications of some weak and shallow maxima at kilometers 163 and 190, Shallow minima (values under zero) for vertical intensity appear to extend from kilometers 120 to 180 and from kilometer 215 farther south. It is possible, however, that the normal gradient of the whole region Freiburg to Chiasso was taken a little too high for Z, namely, 600 gammas per 100 km, and that instead of two minima there are really two less shallow maxima extending from kilometers 140 to 160 and from kilometers 170 to 240. Smaller anomalies are not easily detected in case their effects are not far‐reaching.
The Agincourt Schuster‐Smith coil‐magnetometer
Authors: Jackson W. E. W. 
Published: February 2008

In August 1931 a Schuster‐Smith coil‐magnetometer was installed in the Magnetic Observatory at Agincourt, and is now being used as the standard for horizontal‐force determinations.It may be of interest to other observatories to know how it has functioned during the several months it has now been in operation, and also the results obtained in a series of intercomparisons with our Elliott Magnetometer No. 98, which was in use formerly as the standard, and whose correction on the Department of Terrestrial Magnetism provisional International Magnetic Standard, had been obtained through intercomparison with DTM CIW Instrument No. 15, which was standardized at Washington, D.C., U.S.A.
Thunder‐storm problems in atmospheric electricity
Authors: Deppermann C. E. 
Published: February 2008

Cumulus caps—Because of conflicting claims with reference to their connection with thunder‐storms, special attention was given to the so‐called cumulus “caps.” “Cap” is used to mean one of those limited sheets of cloud which often appears right above a cumulus top, but which soon after is either pierced by the cumulus as it rises or gently falls upon the cumulus, or clings to it. While in the first stage, that is, while a small sheet, usually curved, directly above the cumulus, it is most properly called a cap.During the spring and summer of 1931, there was a most unusual opportunity of studying these caps at Manila because of the protracted thunder‐storm period. The types observed were very varied, but may be grouped under five types, (a) The first type is a sharply outlined layer, usually but not always curved, often reminding one forcibly of a white‐penciled eyebrow; the layer may be very sharp, or wide like a ribbon, single or multiple, faint or densely white; cumuli have been seen with as many as four or five superimposed caps, (b) The second or misty type results when, during an active thunder‐storm, the first type settles on top of the cumulus and thickens, as is often the case, to form a mist, generally brilliantly white; there may be included in this type also the bright white mist into which the existing thick stratus is changed by a rising cumulus, (c) The flocculus type, in which a continuous sheet is not formed, consists of little clouds like some forms of alto‐cumulus, (d) The pennant type is really only a cap of the first or second type, wind‐blown to one side, (e) The wispy or smoky type is formed at times if a cumulus top very slowly falls after just getting a cap; the top seems to be connected with the place of the former cap by smoke‐like wisps or tendrils. There can be absolutely no question that caps can occur at other than cirrus heights, as this phenomenon has been observed at Manila times almost without number, especially when the air is much stratified.
Final relative sunspot‐numbers for 1931
Authors: Brunner W. 
Published: February 2008

The following Tables contain the final relative sunspot‐numbers for 1931, for the whole disc of the Sun, based on observations made at the Zurich Observatory, supplemented by series furnished by other cooperating observatories for days (indicated by asterisks) where no observations were possible at Zurich.Table 1 gives the yearly mean of the relative numbers, R, since the last minimum 1923 and of the number of days without spots.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, January, February, and March 1932
Authors: Nicholson Seth B. , Sternberg Elizabeth E. 
Published: February 2008

In addition to the following magnetic storms, in which the total range in H exceeded 100γ, two storms of slightly less intensity were recorded on February 19 and 20, and March 18, respectively.No solar observations were made at Mount Wilson from January 30 to February 3, inclusive. On February 4 the only spot observed was a small one, 40° west of the central meridian. The hydrogen spectroheliograms on that date showed no unusual activity.
Cooperative work of the Department of Terrestrial Magnetism under the directorship of Louis A. Bauer—An acknowledgment
Authors: Sverdrup H. U. 
Published: February 2008

In Volume I of the “Researches of the Department of Terrestrial Magnetism” Bauer summarizes the first part of the program of the Department of Terrestrial Magnetism of the Carnegie Institution of Washington by saying: “The chief endeavor is to secure magnetic results in the regions where most needed and where there are no organizations prepared to undertake the work.”Under Bauer's directorship the Department of Terrestrial Magnetism has, through its expeditions and observatories, contributed infinitely more than any other institution to the completion of the magnetic survey of the globe. When studying the volumes in which the results are published, the reader is impressed not only by the vast amount of information but also by the painstaking care which has been exercised to develop adequate instruments and to facilitate the work of the observers.
Magnetic characterization of days
Authors: van Dijk G. 
Published: February 2008

At its meeting in Paris in September 1900, the International Meteorological Committee, on the recommendation of the Magnetic Commission, adopted a resolution that the directors of the magnetic observatories be requested to furnish periodically a list of the days which they considered as calm. Dr. Maurits Snellen, member of the Commission and director of the De Bilt Observatory was, from the end of 1903, entrusted with collecting and distributing these lists.At the meeting of the Commission in Innsbruck in September 1905, it was resolved that the magnetic observatories should be requested to prepare, beginning January 1, 1906, statements showing the magnetic character of each day on the scale 0 to 2, proposed by Professor Ad. Schmidt: 0, to indicate calm days; 1, disturbed days; and 2, very disturbed days. It was left to the discretion of the individual directors to fix limits for defining these divisions. The collection and distribution of the statements were again confided to Dr. Snellen.