bluuebunny/crossref_metadata_2025 huggingface dataset:
The secular variation of terrestrial magnetism in Siberia
Authors: Weinberg Boris
Published: February 2008

Tables VII–XII of a previous paper1 under the above caption gave corrections which had to be added algebraically to the observed values of declination (D), inclination (I), and horizontal intensity (H), at different places in Siberia in order to reduce them to the epoch 1910.0. These tables were based exclusively on the values of the three elements of terrestrial magnetism observed at the same point at various times. Such values constitute a rather small portion of all the magnetic determinations made in Siberia. Therefore when all these values were reduced to the epoch 1910.0 by means of Tables VII–XII, and the results plotted on three charts for D, I, and H, respectively, a thorough study of these charts gave some additional data for determining the secular variation for these three elements owing to the possibility of comparing the reduced values with those observed at various times at points not very far distant from those at which the three elements were coincidently observed.
Periodicity of activity in terrestrial magnetism and the rotation of the Sun
Authors: Angenheister G.
Published: February 2008

The methods by which researches into the physical causes of magnetic storms have been made are essentially as follows:

(I) It has been attempted to determine the geographic distribution of magnetic storms over the Earth. In this way the influence of the Earth's permanent magnetic field, on the geographic arrangement of the disturbance field, has been recognized, and it was made probable that there is an extra‐terrestrial cause of disturbance, solar radiation, acting upon this permanent field. We have learned to distinguish several different properties of these storms, such as that some of them are chiefly local in their character, whereas others range over the whole Earth. The known pulsations also belong to the latter.
Some experiments on the penetrating γ radiation present in the atmosphere
Authors: Marsden E.
Published: February 2008

The present note deals with an experiment on the magnitude of the ionization due to penetrating radiation in a closed can on Mount Ruapehu (latitude 39°.25S.; longitude 175°.6E.; height, 9,200 feet = 2,800 meters).

According to Kolhörster,1 the ionization in a closed ionization vessel, in free air, at an altitude of 2,800 meters is 4 ions per c.c. greater than that at sea level. Kolhörster's experiments were made with air in a zinc (?) ionization‐vessel.
On the methodology of finding and representing the distribution of a natural element over a certain region of the Earth's surface, with special reference to terrestrial magnetism
Authors: Weinberg Boris
Published: February 2008

1. The problem. Let E denote the value of a natural element at a given point and a given time, e. g., the temperature, humidity or pressure of the air, the magnetic force, the geological formation, etc. We shall restrict ourselves here to dealing with elements which can be measured quantitatively and the variations of which are continuous both in space and with time. Furthermore, if we consider only the values of the natural element at the surface of the globe, we may write
where φ and λ are the latitude and longitude of a point at the surface of the globe and t is the time.
Earthquake records, Huancayo magnetograms, October‐November, 1922
Authors: Wallis W. F.
Published: February 2008

The details of the records, as measured on the magnetograms of the Huancayo Magnetic Observatory, Peru, are as follows, the times indicated being Greenwich civil mean time:
Regarding measures of magnetic characterization of days
Authors: Bauer Louis A.
Published: February 2008

1. Experience has shown that the Bidlingmaier “activity” measure for the magnetic characterization of days entails too much labor to be successfully put into general practice. Accordingly, Chree,1 Hazard,2 Adolf Schmidt,3 Bauer,4 and van Dijk,5 have been led to suggest other methods of procedure for obtaining measures of magnetic activity. It is also being recognized more and more that the so‐called international magnetic “character” numbers, issued for quarterly periods by the De Bilt Observatory in behalf of the Commission on Terrestrial Magnetism and Atmospheric Electricity of the International Meteorological Committee, do not serve all the purposes desired. The time therefore has come when it would seem advantageous to omit further discussion of past methods and give serious attention to finding some comparatively simple method for the magnetic characterization of days, the adoption of which will not greatly add to the work of the usual observatory personnel.
Erdmagnetische Störungen und Sonnentätigkeit
Authors: Angenheister Von G.
Published: February 2008

In einer früheren Mitteilung (Terr. Mag., 1922, S. 571 und 1921, S. 116) habe ich zu zeigen versucht, was auch Ad. Schmidt schon früher ausgesprochen hat, dass man zwei verschiedene Perioden in der magnetischen Aktivität wiederfindet: eine 27tägige, die allgemein, sowohl für die ruhigsten wie die gestörten Tage, gilt, aber nur wenige Periodenlängen hindurch anhält; ferner zeigen die Daten der grossen magnetischen Störungen, dass sie sich nach Zwischenzeiten, die ganze Vielfache von 30 Tagen sind, zu wiederholen pflegen. Die kurzlebige 27tägige Periode ist wohl veranlasst durch Vorgänge, die ihren Ursprung im Flecken‐und Fackelniveau der Sonne haben und an der Rotation dieses Niveaus teilnehmen. Für die in Frage kommenden niederen Sonnenbreiten sind solche Umlaufzeiten von ungefähr 27 Tagen beobachtet worden.
Principal magnetic storms recorded at the Huancayo Magnetic Observatory, January to December, 1923
Authors: Wallis W. F. , Parkinson W. C.
Published: February 2008

The storm of September 26 started with a sudden commencement, which is plainly shown in all three elements, the horizontal intensity increasing 11γ within six minutes.

The exact times of beginning and ending of the storm of October 15 are rather difficult to define. Within the whole duration of the disturbance there are periods of comparative quiet, greater activity being shown between October 15, 12h and 20h, and October 16, 11h and 21h G.M.T.
Information on magnetic work in the Union of Socialistic Soviet Republics
Authors: Weinberg Boris
Published: February 2008

1. The Observatory of Zuja (near Irkutsk) has recently renewed its regular functioning.

2. The Observatory at Matochkin Shar (Nova Zembla; Lat., 73° 15′ N; Long., 56° 23.′8 E) was working with short intervals during the whole winter. A new building for it should be finished now and thus a regular magnetic service is assured for the future. Mean magentic values for 1924 are D = 20° 35′ E, I = 80° 03′, II = 0.0952 C. G. S.
Correlations between solar activity and atmospheric electricity*: Concluded
Authors: Bauer Louis A.
Published: February 2008

(For additional results, not given in the Abstract on page 23, the interested reader is referred to the summary of Chief Conclusions on page 186.)

19. The atmospheric‐electric observations at Brussels, as shown by curves 2 and 3 of Fig. 3, were made from 1844 to 1877 with a Peltier electrometer “at noon every day,” and as Quetelet7 states, “with all the precautions which the determination of an element so difficult to measure as electricity requires.” Beginning with the middle of 1844, it would seem that the electrometer was mounted at an invariable height above the ground and protected as far as possible from disturbing influences. In calculating the mean results for any period Quetelet “avoided the use of negative values observed during abnormal periods.” While he at various times made a thorough discussion of his observations and investigated relationships between atmospheric electricity and meteorology, he does not appear to have considered, as I had been led to believe by an erroneous reference, any relationship with sun‐spottedness. If he had done so, he would probably have found difficulty in harmonizing the annual course of his results for the period 1845 to 1856 with that for the period beginning with 1856. Excepting for the irregularity in the Brussels8 annual values of P for the period 1871 to 1875, it will be seen from curves 1, 2, 6, and 7 of Fig. 3 that for the period 1855 to 1877, 22 years, increased potential gradient corresponded in general as well with increased sun‐spottedness as did increased magnetic activity (curves 6 and 7). The same fact is true with regard to the curve (No. 3) of “Average Departures of the Annual Variation of the Potential Gradient at Brussels.”
Circular regarding sudden commencements of magnetic storms
Authors: Tanakadate A.
Published: February 2008

At the Madrid Meeting of the Section of Terrestrial Magnetism and Electricity of the International Geodetic and Geophysical Union, it was decided that a systematic investigation of “Sudden Commencements of Magnetic Storms” be made; and the Executive Committee appointed me to act as the Reporter of different views on the subject. I have, consequently, the honor to submit for your consideration the following questionnaire, and I will ask you kindly to inform me of your views, if possible, before May 31, 1925, using the address given below.

It is understood that after the Report has been submitted to the Bureau of the Section, a decision will be made in the following September to take steps for constructing the instruments.
Provisional sun‐spot numbers for October to December, 1924
Authors: Wolfer A.
Published: February 2008

Attention must be called to the fact that the daily relative numbers for February 28 and 29, 1924, instead of 28 and 25, as previously published, should be 22 and 19, respectively; the monthly mean for February 1924 accordingly becomes 4.9 instead of 5.71. These errors were detected only some time after the numbers had been forwarded for publication.
Summary of magnetic observations for the year 1924 at the Apia Observatory, Western Samoa
Authors: Thomson Andrew , Westland C. J.
Published: February 2008

(Latitude, 13° 48′.4S.; longitude, 171° 46′.5 or 11h 27m.lW. of Greenwich.)

The results given below for 1924 are the means of the hourly values of the magnetic elements for all the days in the calendar month.
On diurnal inequalities and the tabulation of curves
Authors: Chree Charles
Published: February 2008

1. There is a variety of procedure in the hourly measurements of curves and in the derivation of the regular diurnal variation, and it seems desirable to call attention to the consequent effects on the results deduced. At some stations use is made of instantaneous values measured at the hour. At other stations mean values are taken for 60‐minute intervals. These intervals may centre at the hour, or they may begin at the hour.
Report on magnetic and electric observations by the Carnegie Institution of Washington in connection with the total solar eclipse of January 24, 1925
Authors: Ault J. P. , Mauchly S. J. , Goddard R. H.
Published: February 2008

A temporary magnetic and electric observatory was established at Greenport, Long Island, by the Department of Terrestrial Magnetism of the Carnegie Institution of Washington in order to determine any possible variations in the Earth's magnetic and electric fields due to a total eclipse of the Sun. Photographic registrations of changes in magnetic declination, horizontal and vertical intensities, and in the electric potential‐gradient of the atmosphere were obtained during the period January 12 to February 5, 1925. In addition, during the period 12h to 17h G.M.T. on January 22 to 28 eye‐readings of the variations in the electric potential‐gradient, positive and negative conductivity, and positive and negative ionic‐content were made.

In general, the eclipse, magnetic effects, as far as can be determined from a preliminary discussion, agree with those observed during previous eclipses. Unfortunately, January 24 was somewhat disturbed magnetically. The eclipse electric effects were of the same nature as found during previous eclipses, but were smaller and showed some irregularities.
Direct determination of the scale values of declinometers
Authors: Egedal J.
Published: February 2008

When determining the scale value of a declinometer for direct readings (in the following called E D d. r.) at Rude Skov after the method given by Mascart, it was discovered that, when the magnet came near to the copper‐clampers, it suffered a deflection. The declinometer for registrations (in the following called E D r.), being of the same type as E D d. r., it was to be feared that a similar effect should exist also in the registering apparatus. If such were the case, it might further be feared that the previous determination of the scale values, carried out in the current way by measuring distance and torsion, the latter being determined by turning the suspension head, did not give the true scale value. On account of this, it was desired to use a different method for the determination of the scale value, a direct method, namely absolute determinations of two different values of the declination.
Records of principal magnetic storms and of earthquakes at the Watheroo Magnetic Observatory, January to September, 1925
Authors: Johnston H. F.
Published: February 2008

(Latitude, 30° 19.′1S.; Longitude, 115° 52′.6 or 7h 44m.E. of Greenwich.)

There were no notable magnetic disturbances recorded during the first quarter. The following notes give in more detail some of the features of the storms listed in the table.
Determination of the atmospheric potential‐gradient reduction‐factor at the Watheroo Magnetic Observatory, Western Australia
Authors: Johnston H. F.
Published: February 2008

Observations of atmospheric potential‐gradient have been made at divers places over the Earth's surface during the last half century at least. These observations are obtained by measuring the potential at some atmospheric point by means of a collector. Various types of collectors have been used such as jets of water or flame, and radio‐active material. The potentials of the collectors are determined by means of electroscopes or electrometers either by eye readings or by some form of continuously recording apparatus.
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.
Some observations of atmospheric‐electric potential‐gradient on mountain peaks in the Peruvian Andes near Huancayo, Peru
Authors: Parkinson W. C.
Published: February 2008

In order to supplement the scanty data on atmospheric potential‐gradient on mountain peaks, continuous records were obtained at two stations near the Huancayo Magnetic Observatory of the Department of Terrestrial Magnetism. The first station (Matahuata) was 500 feet and the second (Cerro‐de‐Ahuac) was 2,200 feet above the Observatory. Curves showing the diurnal variation during fine weather at the two stations and also at the Observatory base‐station are given and briefly discussed.
On Earth‐current observations at Watheroo Magnetic Observatory, 1924–1927
Authors: Gish O. H. , Rooney W. J.
Published: February 2008

The earth‐current measuring system at Watheroo Magnetic Observatory provides for a number of independent records of both components of potential gradient, a feature which has proven helpful in detecting and locating the source of disturbing effects. The results obtained during the four‐year period, 1924–1927, are discussed. The diurnal‐variation curve of the northward component has a mean range of 1.14 millivolts per kilometer with maxima at 17h.5 and 12h.5 and minima at 8h and 17h.5 (120th east meridian mean time). The records resemble those obtained in the northern hemisphere at Berlin and Ebro except that the curve is inverted and smaller in amplitude. The reversal in the direction of current‐flow points to a symmetrical distribution of earth‐currents with reference to the equator. The small amplitudes can be explained on the basis of the unusually high conductivity of the region about Watheroo. No regular change was observed in the mean diurnal‐variation for individual years. The range of the diurnal‐variation curve varies with season from 0.71 millivolts per kilometer in June (midwinter) to 2.06 millivolts per kilometer in October (late spring), and the morning minimum and midday maximum shift forward with increasing height of Sun. The amplitudes of the three principal harmonics vary with season in a similar manner, indicating a single predominating cause for seasonal variation in the normal activity. The eastward component is extremely small at Watheroo; its diurnal‐variation curve has, in general, a double period and a mean range of less than 0.15 millivolt per kilometer.
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′.055t2

H = (25691 + 15.7t − 0.506t2)γ

où t est l'an compté à partir de 1900.
Principal magnetic storms recorded at the Huancayo Magnetic Observatory, January 1 to April 30, 1928
Authors: Ledig Paul G.
Published: February 2008

March 11, 1928.—A short magnetic storm on March 11, beginning at 6h and ending about 17h, was characterized by severe fluctuations in the horizontal intensity, but the declination and vertical intensity were also affected. It began by a slow fall in the horizontal intensity over about two hours, followed by more rapid and intensive fluctuations which were at their maximum between 8h and 15h. Beginning at 8h 29m a sharp drop of 140 gammas in less than five minutes took place, followed by a moderate peak and another deep bay, all badly broken up and irregular.
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.
The Eötvös torsion‐balance method of mapping geological structure
Authors: Barton Donald C.
Published: February 2008

The Eötvös torsion‐balance measures two quantities: the differential curvature of the level (equipotential) surfaces at the point of observation, and the rate of the horizontal variation of gravity at that point. From the rate of variation of gravity, the variation of gravity throughout the area of a survey can be calculated if the stations are close enough together. In areas of no deformation, normally, the horizontal variation of density is slight, but the vertical variation of density is considerable, and usually in the direction of relatively light unconsolidated Tertiaries at the surface through denser and denser Mesozoic rocks, and yet denser Paleozoic rocks, to the dense crystallines of the basement. Structural deformation therefore causes a deformation of the uniform distribution of density.
The advance of an earthquake disturbance
Authors: Reid Harry Fielding
Published: February 2008

The simplest form of the solution of the general elastic equation of wave‐motion is y = sin (2π/λ) (x − νt), where λ is the wavelength and ν the velocity; x and t are the distance and time, respectively. This equation extends from minus infinity to plus infinity, both in distance and in time. The conditions introduced to determine the movement of a seismograph acted upon by such a disturbance, though mathematically correct, lead to physical impossibilities. Another solution of the general equation was suggested which gives the disturbance a definite front, where the medium is at rest in its position of equilibrium, and does not require the introduction of impulsive velocities, as, for instance, in Love's treatment of wave‐motion.
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.
A new method of marking time on magnetograms
Authors: McComb H. E.
Published: February 2008

A new method of marking time on magnetograms consists essentially in increasing the width of the slit in front of the light source for a few seconds each hour. The resulting marks are short, black lines on all base‐lines and curves. The slits are cut in an extension of the armature of a very sensitive relay which is operated by an independent clock.
Auroral work in southern Norway since 1922
Authors: Störmer Carl
Published: February 2008

In Nature of June 19, 1926, January 8, and September 3, 1927, I gave some results of the photographic work on the aurora borealis from my stations in southern Norway. The complete results for the period 1911 to 1922 have been published in detail in Geofysiske Publikasjoner. Since 1922 observers at six stations have been making photographic determinations of the height and situation of the aurora. The following table summarizes the collected material from photographs, arranged chronologically, corresponding to the dates when aurora were photographed. Column I gives the number of successful photographs from one station only; column II shows the number of pairs of photographs taken simultaneously from two stations in telephonic communication to determine the height and situation of the aurora; column III shows the number of successful simultaneous photographs taken from three stations, and column IV the number from four stations.
On the importance of auroral photographs taken from one station
Authors: Sverdrup H. U.
Published: February 2008

Carl Störmer has, as is well known, developed methods for photographing the aurora from two stations and for computing the altitude and the position in space of the aurora from two simultaneous photographs. The principle is very simple. The same points of the aurora are identified on both photographs and azimuth and altitude of these points are determined by means of corresponding coordinates of stars which also appear on the plates. These data, together with known geographic coordinates of the two stations and the exact time when the pictures were taken give data for computing the position in space of every single auroral point.
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.
Note on the radial magnetic gradient of the Sun
Authors: Gunn Ross
Published: February 2008

Dr. Hale and his collaborators at Mt. Wilson Observatory have studied the general magnetic field of the Sun by spectroscopic measurements of the Zeeman‐effect. These researches established the fact that at any given level the distribution of the magnetic field was very similar to the terrestrial distribution. A study of the radial distribution showed that the field decreased radially several thousand times as fast as would be expected if the Sun were uniformly magnetized. This rapid radial variation has made it very difficult to obtain a consistent view of the general magnetic fields of the Sun and Earth.
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.
The variation of magnetic anomalies
Authors: McFarland W. N.
Published: February 2008

This paper describes briefly a method of isogonic chart construction, and the distribution of station anomalies, or differences of observed values from the average condition shown by the chart. The distribution is shown to be according to the law of occurrence of accidental errors. The available data are given in a table and a figure shows the correspondence of observational data and theoretical curve in an individual case.
Notes on aurora in New Zealand
Authors: Kidson Edward
Published: February 2008

The Reverend Alexander Don, of Ophir, Central Otago, a keen observer, has communicated to the Meteorological Office of New Zealand the following notes on auroral displays, the times indicated being New Zealand standard time, which is 11h 30m ahead of Greenwich: March 26, 1928, faint aurora at 22h 00m; April 16, 1928, faint aurora at 22h 30m; August 29, 1928, faint aurora at 19h 30m to 20h 30m.
Ein transportables elektrisches magnetometer
Authors: Uljanin W.
Published: February 2008

Vor vielen Jahren habe ich1 eine elektrische Methode zur Bestimmung der Horizontalintensität des Erdmagnetismus angegeben, welche an einem provisorischen, mehrmals umgebauten Apparate am Kasaner Magnetischen Observatorium geprüft wurde. Damals habe ich ein projektiertes transportables Magnetometer beschrieben, welches äusserer Umstände wegen lange Zeit nicht ausgeführt werden konnte. Erst im Jahre 1926 wurden von der Tatarischen Regierung in Kasan die nötigen Geldmittel bewilligt, so dass an die Herstellung des Instrumentes geschritten werden konnte. Das Magnetometer wurde nach meinen Zeichnungen und Beschreibungen von der Firma Prof. Dr. Edelmann und Sohn in München gebaut.
Einige wichtige planetare Ursachen für die Schwankungen des Erdmagnetismus im Jahre 1927
Authors: Göschl Franz
Published: February 2008

Der Verlauf der erdmagnetischen Charakterzahlen sei an der Hand von Monatstabellen geschildert. Während im Diagramm für 1926 (Dezembernummer 1928, Seite 219) die hervortretenden Zwei‐Tags‐Summen als Maxima von 1 bis 16 abgezählt wurden, sind in dieser Tabelle die betreffenden Tageszahlen durch Fettdruck hervorgehoben. Die Minima wurden im Diagramm mit lateinischen Buchstaben von a bis n bezeichnet. Hier sind die entsprechenden Abfolgen, welche in den Drei‐Tags‐Summen 0.3 nicht überschreiten, in Klammern gesetzt.
Scale‐values of magnetic variometers
Authors: McComb H. E.
Published: February 2008

F. P. Ulrich has made some further tests of the method of determination of scale‐values by use of a large deflector as mentioned by McComb in the June 1928 number of the Journal and described by Ludy in the March 1929 number. The values obtained with the horizontal‐intensity variometer are in close agreement with those determined by the small deflector, and the use of the small deflector has been abandoned in connection with this instrument. Further tests are being conducted with the vertical‐intensity variometer. The scale‐values reduced to zero‐ordinate as obtained with the small deflector at distances 25.8 and 27.2 cm and with the large deflector at 252.0 cm before and after each day's determinations with the small deflector during June 29 to July 15, 1929, are, respectively, as follows: June 29, 3.88, 3.85, and 3.80, 3.82; July 8, 3.82, 3.83, and 3.90, 3.7.7; July 15, 3.78, 3.79, and 3.73, 3.86.
Watheroo Magnetic Observatory, January to May, 1929
Authors: Johnston H. F.
Published: February 2008

February 26–28, 1929—This mild but protracted magnetic disturbance began at 19h 23m. It was ushered in by a sudden commencement which, though not large, was simultaneous for all three elements. The first period of the storm covered an interval of approximately twelve hours, during which the oscillations were small though particularly rapid in the case of declination. During this time the departures from the normal curves were not large.
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.
Zur Elektrizitätshaushalt der Erde
Authors: Maneff G.
Published: February 2008

In unserer kleinen Abhandlung “Die Energiemasse und der Elektrizitätshaushalt der Erde,”1 die Ladung h′0.79×l0−4 e. s. e. ist mit Hilfe von der ersten Formel (1′)

urn:x-wiley:00968013:media:tma31415:tma31415-math-0001
berechnet. Wenn man die zweite Formel (1′)

urn:x-wiley:00968013:media:tma31415:tma31415-math-0002
anwendet, so würde man für h′

urn:x-wiley:00968013:media:tma31415:tma31415-math-0003
erhalten. Diese h′1 ist 1/17 von h′. Der Grund dafür ist darin zu suchen, dass

urn:x-wiley:00968013:media:tma31415:tma31415-math-0004
nur für freie Bewegungen um ein Zentrum anwendbar ist; hier wird die Schwere durch die Zentrifugalkraft kompensiert. Für die Bewegung eines Körpers von der Erdoberfläche (nicht freie) ist jedoch die obige Gleichung (4) nicht anwendbar. In diesem Fall ist die Zentrifugalkraft (1/17)2 mal kleiner als das Gewicht; dies ist der Grund weshalb das Verhältnis

urn:x-wiley:00968013:media:tma31415:tma31415-math-0005
ist.
San Juan Magnetic Observatory October to December, 1929
Authors: Hand Eoline R.
Published: February 2008

The disturbance of October 7 did not begin abruptly, but there was an abrupt change on all three curves at 10h 15m.

The disturbance of November 8 is listed because of the sudden commencement.
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.
Provisional sunspot‐numbers for March to April
Authors: Brunner W.
Published: February 2008

(Dependent alone on observation at Zürich Observatory and its station at Arosa)
Huancayo Magnetic Observatory January to March, 1930
Authors: Ledig Paul G.
Published: February 2008

January 6, 1930—This magnetic disturbance, not of sufficient importance to be called a storm, took place during the daily maximum period of January 6, and was characterized by rather sharp, long, and ragged peaks and bays in the horizontal‐intensity trace, and by marked though slight variations in declination and vertical intensity.
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.
Cheltenham Magnetic Observatory April to June, 1930
Authors: Hartnell Geo.
Published: February 2008

(Latitude 38° 44'.0 N.; longitude 76° 50′.5 or 5h 07m.4 W. of Gr.)
Preliminary report on terrestrial magnetism and electricity at the Stockholm Assembly, August 14 to 23, 1930
Authors: Fleming J. A.
Published: February 2008

The functions of the International Geodetic and Geophysical Union include consideration of what researches and standards are important in geophysical problems and stimulation of such researches and fixing of standards both nationally and internationally. Naturally it is difficult to preserve boundaries between scientific discussion necessary to such functions and more general scientific communication such as is the field of a scientific society. The delegates to the international assemblies of the Geodetic and Geophysical Union are appointed by the various National Research Councils, and must be citizens of the country from which appointed. Funds for carrying on the work of the Union are contributed by the various governments adhering to the statutes.
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.
On the diurnal variation of the Aurora Polaris
Authors: Hulburt E. O.
Published: February 2008

The auroral observations of the International Arctic Expedition of 1882–83, of the Maud Expedition, of three Antarctic expeditions and of temperate latitudes are assembled in order to bring out the diurnal variation of the aurora forms. Vegard's conclusion that the intense, moving and strongly colored forms are more frequent in the evening than in the morning, the diffuse, weak and quiet forms being more abundant in the morning, appears to be valid. His conclusion that most auroral forms show an evening and a morning maximum is found to be contradicted almost as often as it is upheld. His conclusion that the hour of most frequent auroral occurrence falls near magnetic midnight is not found to be true at the Antarctic stations. On the whole the data give the impression that the diurnal course of an auroral display is different for the different stations, as if it depended upon the meteorology of the upper atmosphere of the station.
Notes on green flash observed August 29, 1928, and October 16, 1929
Authors: Davies F. T.
Published: February 2008

The following notes on the “green flash” seen on two occasions by members of the Byrd Antarctic Expedition may be of interest. The first occasion was at sea off the Florida coast on the evening of August 29, 1928. The green flash was seen at the end of a very smoky dull‐red sunset. The disappearing tip of the Sun's disc showed red changing, through yellow to green, the change taking place during the last two seconds before the Sun disappeared.
Watheroo Magnetic Observatory January to August, 1930
Authors: Wood F. W. , Parkinson W. C.
Published: February 2008

JANUARY TO AUGUST, 1930

(Latitude 30° 19′.1S.; longitude 115° 52′.6 or 7h 43m.5E. of Gr.)
Dependence of the normal earth‐current on latitude
Authors: Stenquist David
Published: February 2008

At the Stockholm meeting last August I submitted to the Section of Terrestrial Magnetism and Electricity of the International Union of Geodesy and Geophysics a paper1 containing also an investigation of the diurnal variation (inequality) of the earth‐current as a function of latitude. This investigation refers to ordinary days; that is, all days excepting those highly disturbed. The inequality for such days does not follow the same laws at high latitudes as at low latitudes. At high latitudes the current is roughly of equal intensity during the day and during the night, and the twenty‐four‐hour wave is predominant.
Auroral observations at the Alaska Agricultural College and School of Mines, 1930–31
Authors: Fuller Veryl
Published: February 2008

Description of stations—The two points of observation used for the auroral work are located a little over fourteen miles apart. One, designated as Station 1, is on the college campus: The other, Station 2, is on the Richardson Highway in a southeasterly direction from Station 1. The choice of an outlying station is limited as transportation must be reasonably easy. There are only two possible directions in which the outlying station can be situated. A northerly one and the one chosen.
Cheltenham Magnetic Observatory April to September, 1931
Authors: Hartnell Geo.
Published: February 2008

(Latitude 38° 44′.0 N.; longitude, 76° 50′.5 or 5h 07m.4 W. of Gr.)

There were no magnetic storms recorded during the second and third quarters of 1931.