bluuebunny/crossref_metadata_2025 huggingface dataset:
Some notes on the occurrence of thunder at Sea
Authors: Peters W. J.
Published: February 2008

It appears that Baron von Humboldt is responsible for the statement that thunder is never heard on the ocean at any great distance from land, though violent thunderstorms are often observed at sea and vessels are frequently struck by lightning.1 Since this statement has provoked discussion from time to time, the following notes made from the Carnegie,observations, received from Captain J. P. Ault, may be of some interest. In accordance with directions issued to the vessel by the Director of the Department of Terrestrial Magnetism, the observations were made on the way from Dutch Harbor, Alaska, to Port Lyttelton, New Zealand, between August 6 and November 2, 1915. As the special object was to obtain some facts on the sound of thunder at sea, it is not likely that thunder audible at the ship occurred without being noted.
Meteorologische und luftelektrische Messungen während der totalen Sonnenfinsternis am 10, Oktober 1912 auf der Facenda Boã Vista bei Christina (Prov. Minas Geraes‐Brasilien). I.—meteorologische Beobachtungen
Authors: Knoche Von W. , Laub J.
Published: February 2008

Vorwort.

Der Unterzeichnete erhielt kurz vor der Sonnenfinsternis vom 10. Oktober 1912 eine Einladung seitens des Direktors des Department of Terrestrial Magnetism der Carnegie Institution of Washington, Herrn Dr. L. A. Bauer, während der Finsternis in Brasilien vorzüglich luftelektrische Messungen auszuführen. Die Kosten der Expedition wurden zum Teil von der genannten Institution gedeckt. Der Expedition schloss sich Herr Dr. J. Laub, Professor an der Universität La Plata, an, durch deren Präsident, Senator Dr. J. V. Gonzalez, ihm dankenswerter Weise die Mittel hierzu zur Verfügung gestellt wurden.
Note concerning the effect of terrestrial relief on the ratio of positive to negative ionic densities in the atmosphere
Authors: Mercanton P. L.
Published: February 2008

The slight inequality which is always found between the positive and negative ionic charge‐densities in one and the same volume of air is considerably enhanced when observations are taken on an elevated point of the Earth's surface. Brunhes and Baldit1 showed, as early as 1905, that at any rate up to 1500 meters altitude, the inequality results from a diminution in the negative ionic density rather than from an increase in the positive. All observers have noticed an enhancement of the ratio E+ / E− of the positive to the negative ionic charge‐densities in the same mass of air. The ratio is identical with a− / a+, the ratio of the dispersion‐coefficients, which is, in fact, the same thing as the ratio of the percentage rate of potential‐diminution of a negatively charged body to that of a positively charged body under the same conditions, i.e.
Magnetic “activity” and hourly ranges
Authors: Chree C.
Published: February 2008

§1. An international scheme has been in operation for some ten years, whose object is to discriminate between days according to the greater or less amount of magnetic disturbance. At all cooperating stations each day has allotted to it the “character” figure 0, 1 or 2, according as it is quiet, moderately disturbed, or highly disturbed. The figures thus arrived at are communicated to the Director of the Netherlands Meteorological Institute at De Bilt, who publishes full details quarterly. Finally at the year's end he assigns to each day a “character” figure, representing the mean estimate of the cooperating stations, omitting those whose returns are insufficiently complete.
The magnetograph records at Theodosia, Crimea, during the total solar eclipse of August 21, 1914
Authors: Palazzo L.
Published: February 2008

On the occasion of the solar eclipse of August 21, 1914, a party of Italian scientists, of which the writer was a member, was organized by the Director‐astronomer Prof. Ricco of Catania, and went to Theodosia, Crimea, in the belt of totality. Astronomical, spectroscopic and photographic observations on the celestial phenomenon were to be made, as well as by the writer various geophysical investigations allied with the occurrence of the eclipse. The scheme of work was planned to embrace pyrheliometric, meteorological and magnetic observations, measures of the penetrating radiation, and records of temperature on the soil surface. But the principal work proposed was properly the magnetic one, viz., that of registering the variations of the three magnetic elements during the eclipse.
Remarks regarding least‐square formulæ
Authors: Doolittle M. H.
Published: February 2008

For intelligent and profitable least‐square computation it is necessary that there shall be at least an antecedent working hypothesis, if not an established theory. The method of least squares assumes that within satisfactory limits the irregularities and observer's errors of opposite algebraic signs balance each other. By a least‐square computation the computer's discrepancies of opposite algebraic signs may be made to balance each other precisely; and if the preliminary assumption is tenable and the least‐square computation is controlled by the adopted standard of regularity, it follows that the computer's discrepancies represent within satisfactory limits the irregularities and observer's errors, and that conclusions may be deduced from those discrepancies with a satisfactory approximation to accuracy. If there is no such standard of regularity at the beginning, nothing better than an inconsequential formula can be expected at the end.
Results of magnetic and electric observations made during the solar eclipse of June 8, 1918
Authors: Bauer L. A. , Fisk H. W. , Mauchly S. J.
Published: February 2008

1. The solar eclipse of June 8, 1918, since somewhat over one‐third of the belt of totality was situated in the United States, offered an exceptional opportunity for astronomical and geophysical observations of various kinds. The Department of Terrestrial Magnetism of the Carnegie Institution of Washington confined its attention to magnetic, electric and allied observations. An appeal for cooperative work by institutions favorably situated, was published by L. A. Bauer in the March 1918 issue of this Journal, and the proposed program of work was communicated to interested persons, universities and observatories. As a result of this appeal, data have been obtained at a sufficient number of stations, both inside and outside the entire belt of totality.
Results of magnetic observations during the solar eclipse of June 8, 1918, at the Kakioka Magnetic Observatory, Japan
Authors: Nakamura K.
Published: February 2008

Fig. 1 is a full‐size reproduction of the portion of the magnetogram obtained during the solar eclipse of June 8, 1918, at the Kakioka magnetic observatory, situated about 75 km. north‐northeast of Tokyo. One mm. of ordinate corresponds to 1′.0 for declination (D), 5.3γ for horizontal intensity (H), and 6.27γ for vertical intensity (Z). The values of the base lines are : D0 = 5°07′ W; H0 = 29790γ; Z0 = 34900γ. The time scale was such that 20 mm. equal one hour.
Results of magnetic and electric observations made during the solar eclipse of June 8, 1918: Continued
Authors: Bauer L. A. , Fisk H. W. , Mauchly S. J.
Published: February 2008

26. The effects are especially noticeable at stations where the normal diurnal variation of the Earth's magnetism at the time was large—for example, near the morning or afternoon elongations of the declination‐needle. Kakioka, Japan, was somewhat favorably situated as far as the morning elongation was concerned, and Sitka with regard to the afternoon elongation. At the stations in the United States the eclipse occurred generally in the late afternoon hours when the normal diurnal declination‐changes were themselves small. At Goldendale, the most western station in the United States, the eclipse began just after the time when the afternoon elongation would have ordinarily occurred; the local mean time of totality was 2h 57m P.M., hence when the course of the diurnal variation of declination had already been reversed and the amount reduced to less than that at the afternoon elongation.
Magnetic observations at Lukiapang, China, during lunar eclipses, December 28, 1917 and June 24, 1918
Authors: de Moidrey J.
Published: February 2008

The total eclipse of the Moon on December 28, 1917, was visible at Lukiapang. Fig. 1 reproduces the magnetograms for D and H; the Z‐magnetogram turned out bad. Care was taken to have the magnetograph in good condition. Absolute determinations had been made for D on the 27th, and for H and I on the 28th.
Proposed magnetic and allied observations during the total solar eclipse of May 29, 1919
Authors: Bauer L. A.
Published: February 2008

Special magnetic and allied observations will be made at certain stations inside and outside the shadow belt of the total solar eclipse of May 29, 1919, by the Department of Terrestrial Magnetism of the Carnegie Institution of Washington, and by various magnetic observatories, institutions and individuals who have offered their cooperation. The stations of the Department of Terrestrial Magnetism will be probably: 1. La Paz, Bolivia; 2. Huancayo (north of belt of totality); 3. Near Sobral, Brazil; 4. Île Principe or Libreville, French Congo; 5. Stations outside belt of totality by field parties as found possible. At station 3 complete magnetic and electric observations will be attempted.

The general scheme of work proposed by the Department of Terrestrial Magnetism is as follows:
Additional magnetic observations obtained by the Cinco de Outubro off the coast of Portugal
Authors: de Serra Guedes Raúl Mário
Published: February 2008

Besides the data given in the Reports of the Missão Hidrográfica da Costa de Portugal the following additional values, all referred to the year 1915, were determined:

Latitude 39° 52′ N, longitude 9° 18′ W: Declination 16° 15′ W; inclination 58° 26′ N; total intensity 0.4396 C. G. S.; horizontal intensity 0.2302 C. G. S.
Auroral lights, August 25, 1919, observed at the Yerkes Observatory
Authors: Barnard E. E.
Published: February 2008

On 1919 August 25 before 10h 0m, 90th Meridian Time, there was a low auroral arch in the north. This was not bright nor active. At 11h 10m this arch was faint, but in the low east, south of the Pleiades, a large bright auroral light appeared in the form of an irregular cloud‐like mass several degrees wide and 10° in length (horizontally). Above this was a similar but fainter mass.
Procedure at the magnetic observatories of the United States Coast and Geodetic Survey
Authors: Hazard Daniel L.
Published: February 2008

In Nature for March 20, 1919, Dr. Charles Chree, under the title of “New Procedure at American Magnetic Observatories,” reviewed the publications of the results of observations made at the United States Coast and Geodetic Survey magnetic observatories at Sitka and Honolulu for 1915 and 1916 and called attention to some changes in procedure and to the need of more information regarding certain details of the methods employed. As the questions raised must be settled before there can be that uniformity in the methods of reduction and publication which is essential to the most advantageous, use of magnetic observatory results, it is well to give in some detail the considerations which led the Coast and Geodetic Survey to adopt at its five observatories the practices now in use.

Up to the end of 1914 each hourly value of declination (D), horizontal intensity (H), and vertical intensity (Z) in the monthly tabulations represented the momentary value of the quantity for the specified hour, local mean time. This was in accordance with the general practice at the time the observatories were established, a practice adopted before continuous photographic registration came into use, when eye readings were made once an hour, and when attention was paid mainly to the local features of the variations of the Earth's magnetism. This method has the disadvantages that only a very small portion of the observational data is utilized, undue weight is given to the portion which happens to occur at the arbitrarily selected time, and the results at one station cannot be compared in detail with those at another, particularly at the time of a disturbance, because the use of local mean time renders the tabulated values non‐simultaneous.
Description of glass magnetogram scale used by the Department of Terrestrial Magnetism
Authors: Fleming J. A.
Published: February 2008

To facilitate obtaining the mean ordinate of a 60‐minute interval on the magnetograms obtained at the magnetic observatories of the Department of Terrestrial Magnetism, scales have been constructed in the Department's shops somewhat similar to the type introduced by the Potsdam Magnetic Observatory and as used by the United States Coast and Geodetic Survey. The only difference in our glass scale from the Potsdam one arises from the fact that the Potsdam type makes use of a double scale, the actual mean ordinate in millimeters being obtained from the sum of two readings, whereas we scale the mean ordinate in millimeters direct.

The scale is a piece of plate glass 12.5 cm. wide by 20 cm. long, on which are ruled two sets of lines at right angles to each other. The vertical lines parallel to the long sides are 20 mm. apart, corresponding to the distance between hour‐breaks on the Eschenhagen magnetograms, there being however for direct scaling of ordinates an extra vertical line half‐way between the vertical lines inclosing the right‐hand 20 mm. of the scale. The horizontal lines parallel to the short sides are 10 mm. apart. The first space at the bottom is subdivided to millimeters by short horizontal lines midway between the vertical lines.
Remarks on magnetogram‐scalings and international magnetic data
Authors: Schmidt Adolf
Published: February 2008

I note that in recently published results of the magnetic observatories under the direction of the United States Coast and Geodetic Survey the procedure has been adopted to tabulate the mean ordinate for Greenwich hourly intervals, centering around the half hour, the same as at Potsdam. The non‐cyclic effect may be determined from the adopted procedure just as satisfactorily as from that advanced by Dr. Chree, namely, by obtaining the value at the beginning and end of the day from the two adjacent hourly means. There is no ground for assuming that it is necessary for this purpose to adopt simply the mean of one hourly interval.

As to the adoption of the Greenwich day for the daily tabulations, I put less weight upon this matter. To prefer not to use the Greenwich day but instead some day corresponding to the nearest 15‐degree meridian time, is natural from practical considerations. If anyone prefers to use, nevertheless, the Greenwich day (not simply the Greenwich hours which is the matter of chief importance), this may always be done; it will only be necessary to divide up the hourly series at some other point. However, I would suggest that at the observatories where the Greenwich day is not generally adopted, those data for which strict simultaneity over the Earth is actually requisite be also computed for the Greenwich day and published along with the other results; this suggestion would entail only a small amount of additional work. Such desired data are:
Magnetic character figures for Kew Observatory, May 23–30, 1919
Authors: Chree Charles
Published: February 2008

In allotting magnetic “character” figures for De Bilt I have at no time taken much cognizance of the V (vertical force) curves; because here these almost never show serious disturbance unless the two other elements D and H are highly disturbed. Occasionally, when in doubt as between a 1 and a 2, I may have let the V‐trace decide. Now the artificial disturbance in V renders it all the less useful for help in fixing “characters”.

My normal procedure is to go first through the D‐curves (taking 2 or 3 months' curves at a time to assist in uniformity of standard) and assign to each day the following “character” figures in ascending order of disturbance:
Having completed the D‐curves and put them aside I similarly deal with the H‐curves.
Magnetic storm of August 11–12, 1919
Authors: Hazard D. L.
Published: February 2008

A comparison of the magnetograms from four of the magnetic observatories of the United States Coast and Geodetic Survey for the period of the very large magnetic disturbance of August 11–12, 1919, shows that while the storm had the same general characteristics at all of the observatories, there were very radical differences in detail. Unfortunately the motion of the magnets became so rapid at times that portions of the records were lost or rendered unintelligible, either because the spots of light passed beyond the limits of the paper or because they moved too rapidly to affect the sensitized paper or because the records of the three variometers could not be distinguished with certainty. At Cheltenham the records of the auxiliary Adie magnetograph supplied most of the gaps in the record of the Eschenhagen magnetograph and at Sitka the observer, while changing paper, noticed that a severe storm was in progress and widened the slit of the lantern, so that a good record was secured of the rapid oscillations which characterized the middle and end portions. Greenwich mean civil time is used throughout this paper.
The construction and equipment of the Watheroo Magnetic Observatory in Western Australia
Authors: Fleming J. A. , Wallis W. F.
Published: February 2008

The general magnetic survey of the Earth nearing completion, the next step in the program of the Department of Terrestrial Magnetism of the Carnegie Institution of Washington is the establishment of additional observatories for the study of the variations of the Earth's magnetism, and investigations in atmospheric electricity and earth currents. The paucity of magnetic observatories in the Southern Hemisphere led first to consideration of the region between Mauritius and Melbourne, Australia. Dr. Bauer, the Director of the Department, in 1911 visited Australia and conferred with those interested in geophysical investigations; as the result of these conferences Western Australia was chosen as the site of the Department's first observatory.

SITE OF THE WATHEROO OBSERVATORY.
Sonnentaetigkeit, Sonnenstrahlung, Lufttemperatur und erdmagnetische Aktivitaet im Verlauf einer Sonnenrotation
Authors: Angenheister Von G.
Published: February 2008

Zusammenhänge zwischen der Sonnentätigkeit einerseits und der Sonnenstrahlung, Lufttemperatur und Erdmagnetismus andererseits sind zweifellos vorhanden. Es ist jedoch noch nicht zweifelsfrei festgestellt, wie diese Zusammenhänge physikalisch zu erklären sind, und ob gesteigerter Sonnentätigkeit immer erhöhte oder erniedrigte Sonnenstrahlung, Lufttemperatur und erdmagnetische Feldstärke entspricht. Nach Abbot deuten die Solarkonstantenmessungen von Mt. Wilson darauf hin, dass in der elfjährigen Periode eine gesteigerte Sonnentätigkeit von einer gesteigerten Sonnenstrahlung begleitet ist.1 Die Lufttemperatur der Erde ist zur Zeit gesteigerter Sonnentätigkeit niedriger.
Ueber die Fortpflanzungs‐Geschwindigkeit erdmagnetischer Stoerungen und Pulsationen
Authors: Angenheister G.
Published: February 2008

(Auszug aus den Berichten über die erdmagnetische Schnell und Feinregistrierung in Apia, Batavia, Cheltenham und Tsingtau im September 1911 und Oktober 1912.)

Die Aufgabe der erdmagnetischen Beobachtung ist eine zweifache: Erstens die Ermittelung der geographischen Verteilung des erdmagnetischen Feldes durch eine magnetische Vermessung der Länder und Meere. Landesvermessungen und besonders die zahlreichen Expeditionen und Seereisen dienen diesem Zwecke. Die zweite Aufgabe ist die Verfolgung der zeitlichen Veränderungen dieses erdmagnetischen Feldes durch fortlaufende photographische Registrierungen der erdmagnetischen Elemente, die durch absolute Messungen kontrolliert werden. Ein Netz von erdmagnetischen Observatorien, verbreitet über die ganze Erde, sucht dies zu erfüllen.
Concerning magnetogram‐scalings at the Batavia‐Buitenzorg Magnetic and Meteorological Observatory
Authors: van Bemmelen W.
Published: February 2008

With great interest I have looked over the articles concerning the procedure with regard to magnetogram‐scalings, published in the December, 1919, issue of Terrestrial Magnetism and Atmospheric Electricity.

Carefully examining the advantages and disadvantages of the three methods in question, I came to the conclusion that for Batavia should be adopted:
Concerning glass magnetogram‐scales
Authors: Baker Thos. Y.
Published: February 2008

In the December, 1919, number of Terrestrial Magnetism and Atmospheric Electricity, an article appears describing a glass magnetogram‐scale used in the Department of Terrestrial Magnetism. I do not know how the glass slides are prepared but in case anyone has not seen the “graticules” prepared by the Rheinberg process, may I suggest the possibility of having them done in that way rather than by direct ruling on the glass.

The process is described in the Transactions of the Optical Society, May, 1919. It consists of a photographic transference of the diagram or pattern required, onto the surface of the glass and a subsequent deposit of platinum which is burnt into the surface of the glass.
Magnetic observations at Dehra Dun, May 28–30, 1919
Authors: Bond Captain E. C. T.
Published: February 2008

In response to the co‐operation requested by the Department of Terrestrial Magnetism for special simultaneous magnetic observations during the solar eclipse of May 29, 1919, I have the honor to forward abstracts of the declination, horizontal force, vertical force, and dip observations taken at the Dehra Dun Observatory, India, on the 28th, 29th, and 30th, May, 1919, in accordance with the published program. It will be observed that no unusual changes occurred in the magnetic elements during the observations; I hope, however, that these observations will be of use in the investigation of the effects of the eclipse on the Earth's magnetism.

The geographic position of the Observatory is: Latitude, 30° 19′.3:N.; longitude, 78° 03′.3 or 5h 12m.2 E.
Magnetic observations at Tortosa, May 29, 1919
Authors: Cirera Rev. R.
Published: February 2008

J'ai le plaisir de vous envoyer une copie de deux courbes magnétiques: l'une, le jour de l'éclipse; du 29 mai 1919, et l'autre un jour calme (8–9 Mai) du même mois. En outre, je vous remets la Mémoire No. 3, La Section Magnétique, quoiqu' elle se trouve sans doute dans votre bibliothèque, afin que vous puissiez plus aisément l'utiliser pour l'étude de nos courbes.

Vous trouverez dans chaque copie les valeurs des lignes de repére de la déclinaison D, composante horizontale H, et composante verticale Z.
Magnetic observations at Lukiapang, May 28–30, 1919
Authors: de Moidrey Rev. J.
Published: February 2008

[Copies of the magnetograph‐curves, D, H, and Z, for the prescribed G. M. T. interval and for the 5 days, May 27–31, 1919, were supplied, together with the requisite information as to times, values of base‐lines and scale‐values. Table 1 contains the hourly values as furnished, N here being the mean of the 4 days, May 27, 28, 30, and 31, instead of simply May 28 and 30. Table 1 also contains the differences, ΔD, ΔH, and ΔZ, as derived by subtracting the value N from the corresponding one for May 29, taking west D as minus. The geographic coordinates are : Latitude, 31° 19′ N.; longitude, 121° 02′ or 8h 04m.1 E.—Ed.]
The magnetic character of the year 1919
Authors: van Dijk G.
Published: February 2008

The annual review of the “Caractère magnétique de chaque jour” for 1919 has been drawn up in the same manner as the preceding years. Forty observatories contributed to the quarterly reviews, 37 of them having sent complete data. Table II of the annual review, containing the mean character of each day and each month, the list of “calm days” and the days recommended for reproduction, are reprinted on page 183.
On a special form of magnetic disturbances
Authors: Steiner L.
Published: February 2008

On days which are magnetically almost quiet, or only slightly disturbed, we sometimes find in the curves small disturbances of very regular course. Their period is of about one and one‐half to two and one‐half hours, and their chief characteristic feature is, that the horizontal intensity, starting from the quiet march of the curve, is in general gradually increasing or decreasing till it has attained a maximum or minimum value, and then gradually or with small oscillations returns to the undisturbed value, and the curve continues its quiet course. The disturbance appears in declination and vertical intensity, too. In the vertical intensity there is a gradual decrease or increase, and after the extreme values being attained there is a gentle return to the undisturbed value.
Magnetic disturbances of December 4–5, 1920, at Cheltenham Observatory, Maryland
Authors: Hartnell George
Published: February 2008

A magnetic disturbance with a sudden beginning in H, and a fairly well pronounced beginning in D and Z, began December 4, 1920, at 0h 03m, 75th meridian standard time, hence on December 4, at 5h 03m, G.M.T. H increased from the beginning of the disturbance until 0h 30m, the maximum for the day, and returned to its original value at about lh 54m, the increase being 54γ. D and Z were only slightly disturbed.

The period of the largest disturbances extended from 18h to 19h, there being a decrease in D of some 26′, a decrease of 70γ in H, and an increase of 17γ in Z. The minimum in D occurred at 18h 22m; the minimum in H at 18h 18m; and the maximum in Z at 18h 18m. H was again rather violently disturbed from 14h on December 5, to 17h 30m, with a range of some 60γ. Except during the intervals stated, the curves were only slightly disturbed. The magnetic disturbance appears to have ended at about 24h on December 5th.
Imperial Marine Observatory at Kobe, Japan
Authors: Okada T.
Published: February 2008

I have great pleasure in stating that this new government observatory was opened on August 26, 1920. The principal aims of the observatory are to make researches on meteorological, oceanographic, and magnetic subjects. We have to repair and test marine chronometers, magnetic compasses, and other measuring instruments for navigation. Funds for the buildings have been contributed by various shipowners at Kobe.

As far as magnetic work is concerned, we make a complete set of absolute measurements of the three elements by means of a magnetometer of the Indian survey pattern and an inclinatorium in the middle of each month. We further have a project to build a variation‐house in the neighborhood of this port.
Zur physikalischen Theorie des Erdmagnetismus
Authors: Nippoldt Von A.
Published: February 2008

The following chief conclusions are reached: The principal part of the Earth's magnetic field consists of a non‐homogeneous magnetization of the Earth's crust down to a depth of about 20 km. In addition, there may exist, for the Earth's nucleus, a magnetic field symmetrical both about the Earth's axis of rotation and the equatorial plane, which may have arisen in the same manner as has the Sun's general magnetic field. Besides these two fields there may be, in general, a third, interplanetary, field, whose axis is perpendicular to the plane of the ecliptic and which may be caused by the Sun's electric radiation. How this latter field may be interrelated with the other two fields is not at present discussed.
Earthquake records on the Eschenhagen magnetograms at the Watheroo Magnetic Observatory, western Australia, August 13 and 23, 1921
Authors: Parkinson W. C.
Published: February 2008

All the times given below are referred to G.M.T.

In horizontal intensity the first impulse is shown at 13h 02m 40s August 13, 1921, gradually subsiding by 13h 04m 30s; at 13h 05m 00s there is another impulse. There are some small undulations in the trace after this time, but the seismic effect gradually dies away by 13h 12m 00s, when there is another distinct broadening of the trace, lasting for about 90 seconds, after which the trace resumes its normal character. The amplitude of the movements is about 0.6 mm.
Auroral observations at High River, Alberta, Canada, December 28, 1921
Authors: Bryant Owen
Published: February 2008

lh A. M.—Two curtains observed; largest runs from N.W. to E., another below it extends from nearly North to N.E., latter is very bright at the W. end i. e. N., which appears to be bright because the curtain is running nearly away from the observer and hence more light is observed looking along the curtain than in looking through it. I have observed the same effect before, but I think it was the E. end that seemed to be in line with the eye. It was narrower on the E. end.

7h45m P.M.—Faint curtain observed, center nearly N. 9h00m P.M.—Faint arch low down, center N.E.
On the non‐simultaneity of magnetic storms
Authors: Rodés Rev. Luis
Published: February 2008

Dr. Bauer in a study based chiefly on data collected by Faris, reached the conclusion that “magnetic storms do not begin at precisely the same instant all over the Earth.” The abruptly beginning ones, investigated by him, appeared to progress more often towards the east than towards the west, with a velocity such that it would require, on the average, about four minutes to encircle the Earth at the equator.1

I should like to call attention to the fact that in the case of five well‐defined storms which occurred subsequent to those examined by Bauer, namely, those of January, February and May, 1919, March, 1920, and May, 1921, I have found a simultaneous beginning at Tortosa and at Honolulu, which lies 158 degrees to the west, within the limits of measurement. The photographic paper at Tortosa runs at the rate of 2.8 minutes to the millimeter and the base line is shown every hour by an electric lamp in connection with the astronomical clock, hence, I do not think we can be in error by a minute. The measures for each storm were accurately made by the writer, and the corresponding times of the beginning as registered at the other stations were kindly communicated to me by Col. E. Lester Jones, director of the U. S. Coast and Geodetic Survey, at Washington, and by Capt. R. L. Faris, acting director.2
Proposed magnetic and allied observations during the total solar eclipse of September 10, 1923
Authors: Bauer Louis A. , Fleming J. A.
Published: February 2008

Special magnetic and allied observations will be made at stations inside and outside the shadow belt of the total solar eclipse of September 10, 1923, by the Department of Terrestrial Magnetism of the Carnegie Institution of Washington, and by various co‐operating magnetic observatories, institutions, and individuals. The distribution of the magnetic observatories within the limits of the eclipse and on both sides of the belt of totality is shown by the accompanying map taken from the American Ephemeris and Nautical Almanac for 1923 and on which the positions of these observatories have been indicated.

The observatories, either within or near the limits of the eclipse, are: North of the belt of totality, Sitka (Alaska), Meanook (Alberta), Tucson (Arizona), Agincourt (Ontario), Cheltenham (Maryland), and Vieques (Porto Rico) ; to the south of the belt of totality, Honolulu (Hawaii), Cuajimalpa (Mexico), and Huancayo (Peru); while just outside the limits of the eclipse, at beginning and ending, are Kakioka (Japan) and La Quiaca (Argentina). Of the observatories, that at Tucson is particularly well situated, being only about two hundred miles from the central path of the eclipse; the maximum obscuration at Tucson will be about ninety‐two per cent. It is planned that the Department of Terrestrial Magnetism will have parties at two (possibly three) stations within the belt of totality to make magnetic and atmospheric‐electric observations. The United States Coast and Geodetic Survey will have one special party for taking magnetic observations within the belt of totality in southern California and will have special observations carried out at its observatories.
Earthquake records, Huancayo magnetograms, September 1922 to April 1923
Authors: Wallis W. F.
Published: February 2008

There were records of two small earthquakes on the magnetograms of the Huancayo Magnetic Observatory, in Peru, on September 4 and November 22, 1922. Each one appears to have been due to a short, sharp local shock. On September 4 the effect in declination occurred at 12h 07m with maximum range of 0.7 mm; in horizontal intensity at 12h 07m, the maximum range not measurable owing to rapid change in H, and in vertical intensity at 12h 09m with maximum range of 0.4 mm. On November 22 the effect in declination occurred at 14h 14m with maximum amplitude of 1.0 mm, and in horizontal intensity at 14h 14m, the effect being indistinct owing to rapid change in H, while there was no effect shown in vertical intensity.
The magnetic character of the year 1922
Authors: van Dijk G.
Published: February 2008

The annual review of the “Caractère magnétique de chaque jour” for 1922 has been drawn up in the same manner as the preceeding years. Forty‐three observatories contributed to the quarterly reviews, 37 of them having sent complete data.

The following table contains the mean character of each day and each month, the list of “Calm Days” and the days recommended for reproduction.
The anomalies of terrestrial magnetism and gravity in the Kursk Government, Russia
Authors: Lasareff P.
Published: February 2008

In a preceding article,2 we have given the results of the operations carried out during 1919–1920 in connection with the work undertaken by the Commission des Forces Productives de la Russie cooperating with the Academy of Sciences, for investigating the anomalies of terrestrial magnetism and gravity in the Government of Kursk. The purpose of our note, presented at the Academy of Sciences, on May 2, 1923, was to summarize briefly the results obtained in 1921, 1922, and 1923.

As already indicated in the preceding note, a zone (the northern zone) of strong anomaly, consisting of a narrow strip of 2 to 3 kilometers, extends from the northwest towards the southeast and passes through the districts of Kursk, Stschigry and Tim fer a distance of about 250 kilometers. It has a considerable maximum over an extent of 4 kilometers, the value of Z (vertical intensity) ranging from 1.6 to 1.9 gauss.
On the observations of Earth potential‐gradients at Ebro
Authors: Chapman S. , Whitehead T. T.
Published: February 2008

1. In a recent paper1 the writers have re‐investigated the mathematical relations between the observed terrestrial magnetic variations and the external and internal (induced) magnetic fields which give rise to them. In the course of this paper we compared the diurnal variation of electric potential‐gradient within the earth, given for Berlin, in arbitrary units, by Weinstein, with that derived from the potential of the field of the diurnal magnetic variations, as previously determined by one of us.2 A moderate similarity in type was found; the question of agreement in absolute magnitude could not be tested, however, Weinstein's unit being unknown.

2. The recent appearance of Dr. Bauer's discussion of the measurements of earth potential‐gradients at Ebro3 affords the opportunity for further examination of the question. It may be said at once that the results prove extremely puzzling. The observed potential‐gradients are, as in Weinstein's case, nearly of the type to be expected from the magnetic variations, but are five or six times as large in amplitude. As Dr. Bauer's tables refer to the means for groups of five magnetically quiet days, it seemed just possible that allowance for the factor 5 might have been overlooked, but on enquiry Dr. Bauer kindly confirmed our expectation that this was not the cause of the discrepancy.
Relations between the diurnal and annual variations of Earth currents, terrestrial magnetism and atmospheric electricity
Authors: Bauer Louis A.
Published: February 2008

An investigation is made as to correlations in the diurnal and annual variations of earth‐currents, with those of terrestrial magnestism and atmospheric potential‐gradient, as based on the observations at the Ebro Observatory, Tortosa, Spain, for the magnetically‐quiet days during the five‐year period, 1914–1918.

It is found that the diurnal and annual variations of the horizontal components (X towards north, and Y towards east) of terrestrial magnetism are of such a character, quantitatively and qualitatively, as to indicate that only to a certain extent may they ba the direct electromagnetic effects of the observed corresponding earth currents (W towards west, and N towards north). On the other hand there is a high probability that the observed earth‐currents may be the combined result of a varying magnetic field and a varying electric field as indicated by the rate of variation in terrestrial magnetism and atmospheric electricity, during the day and year. The correlation between the variations of earth‐currents and the rate of variation, or time‐gradients, of the atmospheric potential‐gradient is found to be even higher than that for the time‐gradients of terrestrial magnetism, both as regards the diurnal variation and the annual variation.
On the magnetic anomaly in Poland
Authors: Kalinowski St.
Published: February 2008

When I began magnetic investigations in Polish territory in 1910, I could not be guided in any way by previous surveys, because they were mostly disconnected and not sufficiently worked out.

From separate investigations conducted here and there at different times, we could only estimate with some approximation the annual changes. As a fundamental distance between observation points, I took 40 kilometers, though realizing that later on it would be necessary to diminish this; however, when it was possible (the facility of communication had to be thought of and it is to be remembered that I was doing this at the time of Russian rule), I tried to use also smaller distances, about half as large. The above explains why the distribution of my observation points is not uniform over the whole of Congress (Russian) Poland which has been examined. But, thanks to it, I may draw with still greater assurance conclusions as to the abnormal course of isomagnetic lines, and form other plans as to further investigations. Figs. 1, 2, and 3 show the observation‐points mentioned for the years 1910–1913, together with the respective values of D, H, and I, all reduced to average annual value of 1912, and so they are comparable with each other.
On the characterization of terrestrial magnetism and the variability of natural phenomena
Authors: Ono Suminosuke
Published: February 2008

1. One of the more important problems in terrestrial magnetism is how to express its “characterization.” Many eminent authors have already discussed this problem, and several methods of expressing it have been proposed, but it is difficult to satisfy the following two conditions for the purpose of international cooperation: a. The method of the calculation must be simple for the purpose of operating regularly and expeditiously; b. it must be free from personal bias. These conditions are to some extent contradictory. The simplification of a method is often made at the cost of some physical meaning, and it is unavoidable in general that the maintenance of accuracy in a physical sense complicates the problem.
A method for determining the total intensity of the Earth's magnetic field from a moving support
Authors: Grummann H. R.
Published: February 2008

W. Ujanin2 has used the earth inductor for the measurement of intensity. He does not, however, discuss the feasibility of his various schemes for observations on a vessel or in an airship. Of the two marine methods for determining intensity used by the Department of Terrestrial Magnetism, viz., the Dip Circle and the “Sea Deflector,”3 the second is undoubtedly the better. The instrument is essentially a sine magnetometer, the suspended magnet being a compass card (liquid).
Magnetic declination results, Topographical Survey of Canada, Franklin District, Northwest Territories, Canada, 1923
Authors: Deville E.
Published: February 2008

During the summer of 1923 Mr. F. D. Henderson, D.L.S., accompanied the Canadian Government northern expedition on C.G.S. “Arctic” to make land surveys, and declination observations if time permitted. The instrument used was a five‐inch Bausch and Lomb theodolite fitted with a sensitive trough compass of the same make, mounted on the standard. The index correction of the needle was determined at the Magnetic Observatory, Agincourt. Results are therefore given in “L M. S.” No diurnal‐inequality correction has been applied, but L.M.T. is given instead.
Records of earthquakes and of principal magnetic storms at the Watheroo Magnetic Observatory in 1923
Authors: Wait G. R.
Published: February 2008

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

EARTHQUAKE RECORDS, MARCH TO DECEMBER, 1923.
Values of the magnetic declination in 1924 at principal stations in the Union of the Soviet Socialist Republics
Authors: Pödder Arnold
Published: February 2008

Because of the increasing number of requests by various institutions and persons for a magnetic declination chart for the principal stations of the Union of the Soviet Socialist Republics, the following table was compiled. The work of summarizing the material and reducing it to 1924 was assigned to me, and, thanks to N. N. Trubiatchinskii, in charge of Konstantin Magnetic Observatory at Pavlovsk, who made many valuable suggestions, I have summarized the data as accurately as the scientific material at hand allowed.

The latest observations of declination in Russia are given; for a few stations only, at which no new observations have been made, the magnetic map of European Russia by A. Tillo, for the epoch 1880, was used.
Concerning the computation of tabular quantities
Authors: Neumann Frank
Published: February 2008

In the September, 1924, number of this Journal, pages 121–124, Messrs. Duvall and Ennis, of the Department of Terrestrial Magnetism, describe an interesting graphic method for computing diurnal variations from differential formulae. It is gratifying to know that the problem of simplifying magnetic observatory computations is receiving the attention it deserves for there is no doubt that the great amount of labor involved in the computation of tabular quantities is a serious problem in the preparation of many observatory reports.

In considering the relative merits of various methods of computing diurnal variations, it is practically impossible to reach a wholly satisfactory decision because the personal preference and aptitude of the individual computer and the facilities available are decisive factors. This is particularly true of the addition method1 in which efficiency is almost wholly dependent upon the computer's ability to operate the computing machine. The preparation of the special tables necessary in this method is an insignificant factor, as compared with the construction of any graph.
Terrestrial Magnetism and Electricity at the Madrid meeting, October, 1924
Authors: Bauer Louis A.
Published: February 2008

The second General Assembly of the International Geodetic and Geophysical Union met at Madrid, October 1–8, 1924, twenty‐five of the twenty‐seven countries which already adhere to the Union being represented by delegates and guests.† The total number was about one hundred and fifty.

At the opening meeting on the morning of October 1, His Majesty the King of Spain presided. The address of welcome was delivered by the President of the National Committee of Spain, Señor Cubillo y Muro, and the response by the President of the Union, M. Lallemand. In the afternoon of the same day the officers of the Union and of the sections met, in order to complete arrangements for the plenary meetings of the Union and for the meetings of the various sections, of which there are now seven, namely, Geodesy, Seismology, Meteorology, Terrestrial Magnetism and Electricity, Oceanography, Vulcanology, and Scientific Hydrology. All sessions of the Union and of the Sections were held in the Chamber of Deputies.
Perturbation magnétique du 1er novembre 1924 à Lu‐kia‐pang et à Tsiing‐tao
Authors: de Moidrey J.
Published: February 2008

Le 1er novembre dernier, jour magnétiquement très calme, en relève sur l'enregistreur de Lu‐kia‐pang une perturbation assez violente, de fort courte durée, et telle que je ne me rappelle pas en avoir vu sur nos courbes depuis 1877.

Elle a un début brusque à 0h 07m, temps de Greenwich, Au déclinomètre et à la balance la forme générale est celle d'une baie profonde et peu ouverte. La durée est d'environ un quart d'heure, après lequel le tracé redevient presque aussi uni qu' auparavant.
Principal magnetic disturbances at the Apia Observatory, Samoa, October to December, 1924
Authors: Thomson Andrew , Westland C. J.
Published: February 2008

Between November 27d 20h 12m and 28d lh 30m a range in D of 7′.7 was registered. This is the largest variation in D occurring in a period of 24 hours during 1924 at Apia, and it took place without any corresponding changes in H or Z. The mean daily range in D during November is 4′.O. The range of H on November 27 and 28 was 6lγ and 80γ which although above the mean range is not uncommon.
Provisional sun‐spot numbers for January to March, 1925
Authors: Wolfer A.
Published: February 2008

1. The foregoing article (pp. 69‐77) by Dr. Chree has particular reference to an item of the Madrid meeting of the International Section of Terrestrial Magnetism and Electricity pertaining to the application of non‐cyclic corrections in terrestial magnetism and atmospheric electricity which, owing to limited time, could not fully be discussed and regarding which no agreement was reached. Dr. Chree has concerned himself with the application of non‐cyclic corrections for a period of about two decades, but he has had few followers in the method adopted by him. It should be recalled that he has chiefly dealt with the discussion of the so‐called quiet days (limited to 5 per month in the case of terrestrial magnetism, and to 10, in atmospheric electricity).

2. The mean values of results from the selected quiet days are frequently termed “normal” values, though, as a matter of fact investigations have repeatedly shown that the quiet clays are as subject to a special kind of disturbance, though to be sure to less extent, as are the greatly disturbed days. This fact is admirably shown in Father de Moidrey's timely article (pp. 79‐82). Instead of the quiet‐day values representing normal conditions they should be looked upon as representing subnormal conditions; it is as bad at times for a patient to have a sub‐normal temperature as a high temperature. On the average, about 65‐70 per cent of the five magnetically‐quiet days per month selected at the De Bilt Observatory, on the basis of characterization lists received from the operating observatories, are the days of minimum range in horizontal intensity. Sometimes it happens that a magnetic‐activity measure based on the assumption that the quiet days represent normal conditions turns out negative, and, hence, does not admit of physical interpretation. It has even occurred that the monthly mean diurnal range for the selected 5 quiet days was higher than the monthly mean diurnal range obtained from the 10 least disturbed days per month. We, accordingly, deem it safer in general, not to apply non‐cyclic corrections by Chree's method, with all the suppositions it implies, e.g., progressive linear change throughout the day, but we are quite ready to give all the information in our observatory publications which others may require for any procedure they may make themselves responsible for. Fortunately in terrestrial magnetism the “non‐cyclic” correction, as derived from differences of successive midnight values, is, in general, small, however, the case is entirely different in atmospheric electricity where the accidental or disturbing features may play a predominant part. We have repeatedly determined the Fourier coefficients from a series of diurnal‐variation observations extending over several months, or over several years, and have invariably found that the differences in the essential quantities, computed with or without application of a supposed non‐cyclic correction, are inconsequential from a physical standpoint.