bluuebunny/crossref_metadata_2025 huggingface dataset:
Additional notes on observations of magnetic anomalies with a variometer
Authors: Koenigsberger J. G.
Published: February 2008

Referring to my article in the preceding number of this JOURNAL (pp. 243–249), I have pleasure in sending herewith a graph with another abscissæ‐axis to take the place of Figure 5; this now is a projection on a north‐south line and shows further and improved analysis as regards part of the line of the magnetic profile through the Black Forest, the Swiss Jura, and the Swiss Alps, including the additional observations obtained (and summarized in Table 1 of the previous communication) to extend it to Lago di Lugano and Chiasso in Italy.

The curvatures of the profiles for the differences of H and Z against the normal values as shown in the Figure herewith indicate the depth of the center of the disturbing rock on the first 25 km of the line to be about 7 to 12 km between kilometers 15 and 20 for the principal anomaly, and that of a second anomaly to be about 5 km in the same region between kilometers 15 and 20—more probably caused by intrusive basic rocks than tectonics. The same or similar anomaly was detected on the other side of the Rhine (Alsatia, France) by J. Jung and C. Alexanian [Ann. Office Nation. Combustibles Liquides, 6, 43–58 (1931)]. Anomalies having depths of centers about 5 km are indicated at kilometer 100 and at kilometer 150, and another center of depth more than 10 km at kilometer 200, as well as indications of some weak and shallow maxima at kilometers 163 and 190, Shallow minima (values under zero) for vertical intensity appear to extend from kilometers 120 to 180 and from kilometer 215 farther south. It is possible, however, that the normal gradient of the whole region Freiburg to Chiasso was taken a little too high for Z, namely, 600 gammas per 100 km, and that instead of two minima there are really two less shallow maxima extending from kilometers 140 to 160 and from kilometers 170 to 240. Smaller anomalies are not easily detected in case their effects are not far‐reaching.
The Agincourt Schuster‐Smith coil‐magnetometer
Authors: Jackson W. E. W.
Published: February 2008

In August 1931 a Schuster‐Smith coil‐magnetometer was installed in the Magnetic Observatory at Agincourt, and is now being used as the standard for horizontal‐force determinations.

It may be of interest to other observatories to know how it has functioned during the several months it has now been in operation, and also the results obtained in a series of intercomparisons with our Elliott Magnetometer No. 98, which was in use formerly as the standard, and whose correction on the Department of Terrestrial Magnetism provisional International Magnetic Standard, had been obtained through intercomparison with DTM CIW Instrument No. 15, which was standardized at Washington, D.C., U.S.A.
A note upon vertical intensity at the Apia Observatory
Authors: Westland C. J.
Published: February 2008

At the Apia Observatory the north pole of the magnet rises, so that vertical intensity is negative. The practice adopted to facilitate tabulation is to disregard signs, and in this way the reading which has the largest numerical value is called the maximum. The hourly values of vertical intensity, Z, are computed in the same manner as those of horizontal intensity, H, and of declination, D, namely from the mean ordinate to the curve during the entire period of 60 minutes commencing at the hour of Greenwich mean time stated. In the harmonic analysis the notation is
Thunder‐storm problems in atmospheric electricity
Authors: Deppermann C. E.
Published: February 2008

Cumulus caps—Because of conflicting claims with reference to their connection with thunder‐storms, special attention was given to the so‐called cumulus “caps.” “Cap” is used to mean one of those limited sheets of cloud which often appears right above a cumulus top, but which soon after is either pierced by the cumulus as it rises or gently falls upon the cumulus, or clings to it. While in the first stage, that is, while a small sheet, usually curved, directly above the cumulus, it is most properly called a cap.

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

The following Tables contain the final relative sunspot‐numbers for 1931, for the whole disc of the Sun, based on observations made at the Zurich Observatory, supplemented by series furnished by other cooperating observatories for days (indicated by asterisks) where no observations were possible at Zurich.

Table 1 gives the yearly mean of the relative numbers, R, since the last minimum 1923 and of the number of days without spots.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, January, February, and March 1932
Authors: Nicholson Seth B. , Sternberg Elizabeth E.
Published: February 2008

In addition to the following magnetic storms, in which the total range in H exceeded 100γ, two storms of slightly less intensity were recorded on February 19 and 20, and March 18, respectively.

No solar observations were made at Mount Wilson from January 30 to February 3, inclusive. On February 4 the only spot observed was a small one, 40° west of the central meridian. The hydrogen spectroheliograms on that date showed no unusual activity.
Cooperative work of the Department of Terrestrial Magnetism under the directorship of Louis A. Bauer—An acknowledgment
Authors: Sverdrup H. U.
Published: February 2008

In Volume I of the “Researches of the Department of Terrestrial Magnetism” Bauer summarizes the first part of the program of the Department of Terrestrial Magnetism of the Carnegie Institution of Washington by saying: “The chief endeavor is to secure magnetic results in the regions where most needed and where there are no organizations prepared to undertake the work.”

Under Bauer's directorship the Department of Terrestrial Magnetism has, through its expeditions and observatories, contributed infinitely more than any other institution to the completion of the magnetic survey of the globe. When studying the volumes in which the results are published, the reader is impressed not only by the vast amount of information but also by the painstaking care which has been exercised to develop adequate instruments and to facilitate the work of the observers.
Magnetic characterization of days
Authors: van Dijk G.
Published: February 2008

At its meeting in Paris in September 1900, the International Meteorological Committee, on the recommendation of the Magnetic Commission, adopted a resolution that the directors of the magnetic observatories be requested to furnish periodically a list of the days which they considered as calm. Dr. Maurits Snellen, member of the Commission and director of the De Bilt Observatory was, from the end of 1903, entrusted with collecting and distributing these lists.

At the meeting of the Commission in Innsbruck in September 1905, it was resolved that the magnetic observatories should be requested to prepare, beginning January 1, 1906, statements showing the magnetic character of each day on the scale 0 to 2, proposed by Professor Ad. Schmidt: 0, to indicate calm days; 1, disturbed days; and 2, very disturbed days. It was left to the discretion of the individual directors to fix limits for defining these divisions. The collection and distribution of the statements were again confided to Dr. Snellen.
Einige Ergänzungen der klassischen Deviationstheorie
Authors: Meldau Von H.
Published: February 2008

Die klassische Deviationstheorie, wie sie z.B. im “Admiralty Manual for the Deviations of the Compass” enthalten ist, nimmt zunächst an, dass nur “fester” und “flüchtiger” Magnetismus im Schiffe vorhanden sind. Unter der weiteren Voraussetzung, dass die Komponenten des vom “flüchtigen” Magnetismus am Kompassort erzeugten Feldes lineare Funktionen der Komponenten des erdmagnetischen Feldes seien, gelten für den “Kompassort” bei aufrecht auf ebenem Kiel liegendem Schiffe die bekannten, zuerst von S. D. Poisson aufgestellten Gleichungen2

urn:x-wiley:00968013:media:tma31653:tma31653-math-0001
Aus diesen Gleichungen lässt sich die Ablenkung eines im Kompassort aufgestellten Kompasses berechnen, wenn man noch voraussetzt: (1) dass die Kompassnadeln als unendlich klein im Vergleich zur Entfernung der nächstgelegenen Eisenmassen oder Magnetpole angesehen werden können; (2) dass keinerlei Nadelinduktion im Spiele ist, d.h., dass die Kompassnadeln nicht ihrerseits eine merkliche Induktion in den nächstgelegenen Eisenmassen hervorrufen. Das Erfülltsein dieser Forderungen seitens der Eisenmassen des Schiffes selbst ist bei vernünftig gewähltem Kompassort gewährleistet, es ist aber dann in Frage gestellt, wenn Magnete und Weicheisenmassen zur Kompensation der vom Schiffe erzeugten Ablenkung am Kompasshause angebracht werden. Das zeigte sich zuerst um das Jahr 1860 bei der Kompensation der Kompasse des berühmten “Great Eastern.”
A demonstration of the geologic possibilities of resistivity and magnetic prospecting methods
Authors: Heiland C. A.
Published: February 2008

In his studies of terrestrial‐magnetic and atmospheric‐electric phenomena, Bauer's interests were not confined to the pure science‐problems in these fields. He also gave a great deal of attention to the question as to how the instruments and methods used in terrestrial‐magnetic and terrestrial‐electric research could be best adapted to the needs of the prospector. The writer in particular has enjoyed his advice and cooperation in a number of problems which arose in the development and calibration of magnetic instruments. While Bauer was Director of the Department of Research in Terrestrial Magnetism of the Carnegie Institution of Washington, this Institution became actively interested in the measurement of ground‐resistivities as a means of attacking certain problems related to earth‐current phenomena.
American URSI broadcasts of cosmic data
Authors: Clarke Katharine B.
Published: February 2008

The data for terrestrial magnetism, sunspots, solar constant, and aurora are the same as given in previous tables.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, April, May, and June 1932
Authors: Nicholson Seth B. , Sternberg Elizabeth E.
Published: February 2008

The only magnetic storms during the second quarter of 1932 in which the total range in H exceeded 100γ were on April 7 and May 29. The storm of April 7 was reported in the last number of this publication.

On May 29 only one spot was visible. No observations were made with the spectrohelioscope on that date. On May 28 the activity of the bright hydrogen near this group had increased slightly over that observed on May 27.
Remarks on Dr. Kennelly's notes
Authors: Bartels J.
Published: February 2008

The readers of this JOURNAL will be grateful to Dr. Kennelly for his clear summary. He stresses the usefulness of the international conventions for a uniform adoption of units—a usefulness which is rather independent from theoretical considerations about which there is no unanimity.

As to terrestrial magnetism it is a question whether the new conventions, especially the rather vague recognition of a physical dimension of the magnetic permeability, make a change in the usual practice necessary. I should like to support the unchanged use of the gauss (and of the γ as its 100000th part) as a unit even more strongly than Dr. Kennelly, for the following reasons: Practically all writers of text‐books or papers on terrestrial magnetism neglected from the outset the susceptibility of air, a procedure fully justified by the negligible numerical difference between B and H, as Dr. Kennelly also points out. Thus, if we speak of the magnetic field of the Earth and of its intensity, we need not state definitely whether we mean the quantity which the convention calls magnetic field‐strength H, or that which it calls flux‐density B. (Furthermore, it is usual in terrestrial magnetism—and sanctioned by the International Meteorological Conference at Paris in 1896—to reserve the letter H for horizontal force. We therefore may as well talk of the total force or total intensity of the north component, etc., and express them in the unit gauss, as heretofore. A physicist adhering to the conventions is at liberty to take the values as expressing “flux‐density”.) As Dr. Kennelly states, with the electric magnetometers —for instance, the Schuster‐Smith magnetometer—measurements are in fact made in the unit gauss as defined by the new international conventions.
Progress in the photography of the aurora borealis
Authors: Störmer Carl
Published: February 2008

In pursuance of the collaboration of German and Norwegian scientists in the Aurora‐Borealis investigations initiated by Dr. Brüiche, the Notgemeinschaft der deutschen Wissenschaft, Heinrich Hertz Institute, and the AEG furnished the means for carrying out exhaustive research during the past winter on the instantaneous photography of the Aurora Borealis.

In this research work, reduction of the exposure‐time is not only of profound importance from the standpoint of recording rapidly‐moving phenomena, but is also the hypothesis for the employment of the cinematographic principle for recording the behaviour of the Aurora Borealis as a function of time, as used for establishing any possible correlation with other phenomena (fluctuations of ionized‐region layers, rapid magnetic disturbances, etc.). In order to carry out the research work, Dipl. Ing. Bauer, assistant at the photophysical laboratory of the Danzig Technical University, worked as guest in the Aurora‐Borealis Observatory at Tromsö from December 1931 to April 1932 with apparatus from the AEG Research Institute.
Influence of Louis A. Bauer on knowledge of terrestrial magnetism throughout the United States
Authors: Heck N. H.
Published: February 2008

With reference to the last publication listed under section 2 of the article “Principal published papers of Louis A. Bauer” on page 222 of the September 1932 number of the JOURNAL, further comment may be made. The publication “Principal facts of the Earth's magnetism” was remarkable for being in constant demand on the part of the public from 1902 to 1925. By 1925 the advances in terrestrial magnetism had become so great that a new publication along the same lines was necessary and this was done by Daniel L. Hazard. The revised publication, which owes a great deal of its material to the earlier publication, is still in steady demand.
American URSI broadcasts of cosmic data
Authors: Clarke Katharine B.
Published: February 2008

The data for terrestrial magnetism, sunspots, and aurora are the same as given in previous tables.

The first three columns of the Table give (1) the magnetic character according to the scale 0–2 of the International Commission of Terrestrial Magnetism and Electricity, (2) the type featuring the day other than normal by letters b, p, o, and i for days marked by bay, rapid pulsations, long‐period oscillations, and irregular oscillations, respectively, and (3) the hour and minute of Greenwich mean time marking the beginning of a storm, the end of the storm being indicated in the footnote to the Table. The next two columns give the data relating to sunspots: (1) the number of groups of spots and (2) the total number of spots. It is to be noted that sunspot‐numbers such as those from Zürich can be obtained from the number of groups and spots given in the Table by the formula N = k (10g + s), where k for Mount Wilson is about 0.77.
False cirrus and atmospheric potential‐gradient
Authors: Sil J. M.
Published: February 2008

It has been observed on five occasions at Poona that a false cirrus overhead increases the intensity of the Earth's normal electrical field to a considerable extent. A particularly good example of this effect was observed August 27, 1932, when a thin sheet of false cirrus was seen spreading out of the head of a large towering cumulo‐nimbus cloud, which was lying at a great distance to the northeast of Poona. This false cirrus came over the observatory at 6:20 P. M.; after about half an hour it became spongy in appearance and then gradually grew thinner till it disappeared at about 7:45 P. M. Thin sheets of cirro‐stratus were however seen in the southwest horizon after 8 P. M.
Cheltenham Magnetic Observatory October to December, 1932
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 fourth quarter of 1931.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, April, May, and June, 1933
Authors: Nicholson Seth B. , Sternberg Elizabeth E.
Published: February 2008

The only magnetic storm in the second quarter of 1933 in which the total range in H exceeded 100γ began April 30 at 16h 28m G. M. T., and ended May 2 at about 2h; the range in horizontal intensity was 190γ. No sunspots were visible during this storm and no exceptional activity was recorded with the spectroheliograph.
Graphical aids in the reduction of magnetic observations
Authors: Ennis C. C.
Published: February 2008

In view of the voluminous computational work involved in the ordinary reductions of magnetic observations resulting from the photographic registrations at observatories, it is important to have in mind the development of methods for simplifying and expediting the computational work, and especially to devise methods of checking which are independent of the original computations. To this end the graphs presented herein were developed in the Department of Terrestrial Magnetism of the Carnegie Institution of Washington, primarily as aids in checking the diurnal‐variation values as determined from the differential expressions

ΔX = cos D ΔH − H sin D sin 1′ ΔD

ΔY = sin D ΔH + H cos D sin 1′ ΔD

ΔF = cos I ΔH + sin I ΔZ

ΔI = (1/F sin 1′) (cos I ΔZ − sin I ΔH

Using as an example the magnetic elements at Watheroo Magnetic Observatory for all days for 1929, where D = 4° 12′.1 west, I = 64° 15′.5 south, H = 24646γ, Z = − 51116γ, west declination and south inclination being reckoned minus, the above expressions reduce to
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, July, August, and September, 1933, and note on values December, 1929, and January, 1930
Authors: Nicholson Seth B. , Sternberg Elizabeth E.
Published: February 2008

In the third quarter of 1933 there were two magnetic storms in which the total range in H exceeded 100γ. No spots were visible at the time of the storm which began on August 5 nor was any exceptional activity recorded with the spectroheliograph.

On September 6 an active group appeared and developed rapidly. Exceptionally bright hydrogen clouds were present over this group until it disappeared at the west limb on September 10. The magnetic storm which began September 8 was probably due to this activity, although it may have been caused by a less active region in which no spots were visible but which was near the central meridian on September 8.
Auroral observations and magnetic conditions at the Sitka Magnetic Observatory, July 1932 to June 1933
Authors: Ulrich Franklin P.
Published: February 2008

This paper is a continuation of the reports,2 begun in 1923, of the investigation concerning the relation between aurora and the Earth's magnetic field. The investigation of the Earth's magnetic field and its relation to radio reception was discontinued with the report for 1928–29 because of the lack of proper sensitive instruments and because this investigation is being taken up elsewhere in a more detailed manner than was possible at this Observatory.

Instruments and methods—The instruments and methods as outlined in the report for 1923–24 were used during these observations.
Summary of the year's work, Department of Terrestrial Magnetism, Carnegie Institution of Washington
Authors: Fleming J. A.
Published: February 2008

The work of the Department during the report‐year, July 1, 1933, to June 30,1934, may be generally grouped under four divisions of endeavor. These were: (1) Reduction and study of the observational material already gathered; (2) development of methods and technique to obtain continuous records of the electrical conditions and their variations in the ionosphere ; (3) continued attack in the laboratory on basic phenomena of magnetism through experimental work in nuclear physics; (4) maintenance of field‐operations to preserve continuity of secular‐variation material and of records at observatories for seasonal, diurnal, and irregular fluctuations of the Earth's magnetic and electric field.

Perhaps a most significant immediate advance is that in the ionosphere‐research which was initiated by the Department in 1925. In its latest development, it appears the most promising of recent methods of approach and one greatly enhanced by the rapid progress in nuclear physics and in wave‐propagation. It is not at the stage where continuous photographic records may be secured, manual observational methods meanwhile having shown fundamental results. This method appears also a sure means to obtain definite information not only of the conditions of the, as yet, otherwise inaccessible regions above the Earth's surface but of cosmical phenomena and of their relations to terrestrial ones. An understanding of the mechanism connecting the ionosphere and the external portion of the Earth's surface must improve knowledge of the relation of cosmical radiations in the ionosphere to their images represented by magnetic and electric phenomena at the Earth's surface and below the Earth's surface.
Huancayo Magnetic Observatory, July to September 1934
Authors: Cairns J. E. I. , Torreson O. W.
Published: February 2008

July 3—A minor disturbance of short duration beginning with a marked sudden commencement was recorded at 10h 32m, G. M, T., when the H‐trace moved suddenly upwards, increasing 42 gammas in 5 minutes. At the same time D increased 0′.3 and Z increased 5 gammas. Oscillations of small amplitude superimposed on slow larger movements then set in and continued until 19h, G. M. T., when the disturbance ceased rather abruptly, though slightly disturbed conditions prevailed for the next few days.
Apia Observatory, July to September 1934
Authors: Wadsworth J.
Published: February 2008

July 3—A sudden commencement with a sharp rise of 25 gammas in horizontal intensity took place at 10h 32m, G. M. T. The trace rose to a maximum of 35080 gammas at 11h 59m and then fell to a minimum of 35039 at 12h38m. It was slightly irregular during the next 36 hours. Declination increased suddenly by 0′.5 towards east and vertical force likewise increased by 5 gammas, the fluctuations of the Godhavn balance being similar to those of the H‐variometer.
Final relative sunspot‐numbers for 1934
Authors: Brunner W.
Published: February 2008

The following Tables contain the final sunspot‐numbers for 1934, for the whole disc of the Sun, based on observations made at the Zürich Observatory, supplemented by series furnished by other cooperating observatories for days (indicated by asterisks) on which no observations were possible at Zürich.

Table 1 gives the yearly means of the relative numbers, R, since the last minimum 1923 and the number of days without spots.
Watheroo Magnetic Observatory October, 1934, to March, 1935
Authors: Parkinson W. C.
Published: February 2008

(Latitude 30° 18′.1 S., longitude, 115° 52′.6 or 7h 43m.5 E. of Gr.)

October 24, 1934—This small disturbance began with a sudden commencement at 1h 02m, G. M. T., the horizontal intensity showing a decrease of 5 gammas in two minutes. The declination changed 0′.7 westerly, while the commencement was not well marked in vertical intensity.
Sur la variation annuelle du champ magnétique terrestre à Paris
Authors: Eblé Louis
Published: February 2008

La variation séculaire du champ magnétique, même lorsqu'elle est rapide, n'est pas linéaire, ni représentable par une fonction algébrique du temps; si l'on s'en tient aux moyennes mensuelles, les résidus sont tantôt en excès, tantôt en défaut. Cela ne doit pas étonner, car l'effet des perturbations suffit à l'expliquer: Après une forte perturbation, par exemple, la valeur de H reste relativement faible pendant plusieurs jours, ce qui doit abaisser légèrement la moyenne mensuelle. Les écarts présentent‐ils une répartition annuelle? c'est ce qui a été controversé. On possède aujourd'hui des séries d'enregistrements assez longues pour essayer de déterminer les marches annuelles superposées aux variations séculaires des éléments magnétiques.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory April, May, and June, 1935
Authors: Nicholson Seth B. , Sternberg Elizabeth E.
Published: February 2008

The storm of May 1 began with a sudden commencement in which the horizontal intensity increased 23 gammas. No observations with the spectroheliograph were made at Mount Wilson from April 27 to May 3. A group of spots, which in four days developed into a large group, was first seen on May 2 in latitude 32° south, 22° east of the central meridian.

An active group which reached its maximum area on June 10 was first seen on June 8 in latitude 32° south, 19° east of the central meridian. On June 9 at 18h, G. M. T., very bright hydrogen‐clouds were observed over this group.
Apia Observatory April to June, 1935
Authors: Wadsworth J.
Published: February 2008

(Latitude 13° 48′.4 S., longitude 171° 46′.5 or 11h 27m.1 W. of Gr.)

April 9—There was a fairly low minimum value of horizontal intensity at 8h 15m G. M. T.
Measures of terrestrial‐magnetic activity
Authors: van Dijk G.
Published: February 2008

In the abstract of his paper1, “Terrestrial‐magnetic activity and its relation to solar phenomena,” Professor Bartels states, “A break in the homogeneity of the international character‐figures in recent years is discovered.” From the contents of the paper it appears that by “recent years” especially the year 1930 is meant.

Bartels bases his conclusion principally on the fact that while the international character‐number C shows a considerable increase from 1929 to 1930 (from 0.672 to 0.826) the u‐ and u1‐measures of magnetic activity indicate a small decrease (u from 1.05 to 1.00, u1 from 67 to 63).
The magnetic character of the year 1934 and the numerical magnetic character of days 1934
Authors: van Dijk G.
Published: February 2008

The annual review of the “Caractère magnétique de chaque jour” for 1934 has been drawn up in the same manner as for preceding years. Fifty‐two observatories contributed to the quarterly tables, forty‐seven of them sent complete data.

Table II (reproduced as Table 1 below) of the annual review, contains the mean character of each day for each month. The lists of calm days and disturbed days, and the days recommended for reproduction are also reprinted here as Table 2.
Mitteilung über erdmagnetische und elektrische Arbeiten in der U. d. S. S. R. in den jahren 1931–35
Authors: Puschkow N. W.
Published: February 2008

Der Umfang der erdmagnetischen und elektrischen Arbeiten in der Sowjetunion wächst von Jahr zu Jahr. Diese Arbeiten werden jetzt von einer grossen Anzahl verschiedener Organisationen geleitet und durchgeführt: Geomagnetischen, hydrographischen, geologischen Instituten, Universitäten, und Hochschulen.

Das Netz der magnetischen Observatorien—Die Sowjetunion verfügt zur Zeit über 18 magnetische Observatorien, von denen sechs sich in der Polarzone befinden. Wir halten diese Zahl aber für ungenügend: es wird beabsichtigt in der nächsten Zeit noch fünf bis sechs Observatorien in der Arktis und im asiatischen Teil der Union zu stiften. Nebst dieser Ausbreitung des Netzes wird auch beabsichtigt seine Ausrüstung bis zu einem Niveau zu heben, das unseren Observatorien gestatten wird eine allseitige Erforschung der magnetischen Erscheinungen mit allen zur Zeit zugänglichen Mitteln zu führen. Die Polarobservatorien werden mit je drei Serien von Magnetographen versehen, inklusive Magnétographe grosser Geschwindigkeit. Auch elektrische Messungsmethoden werden eingeführt.
Watheroo Magnetic Observatory July to September, 1935
Authors: Parkinson W. C.
Published: February 2008

September 10–12—This was a disturbance of moderate intensity presenting some unusual features. The exact time of beginning is doubtful. At 21h 50m G.M.T., September 10, there was a sharp but small movement shown in all three elements, and this possibly marked the commencement of the disturbance. The horizontal intensity increased 5 gammas, the vertical intensity decreased 7 gammas, and the westerly declination decreased 1′.2; all these changes took place in about two minutes of time. However, for the ensuing three hours the traces fluctuated very mildly until 1h 20m, September 11, when there was a sudden impulse in all three elements, the amplitude being practically equal to that described above but the movement occupying about 30 seconds of time. Thence onward the traces showed irregular fluctuations, rapid but generally of only moderate amplitude. Between 13h 10m and 14h 20m, September 11, there was a remarkable westerly swing in the declination; the highest value, 19′ above the normal, occurred at 13h 30m. A similar swing occurred in vertical intensity, but the horizontal‐intensity trace showed nothing outstanding. Irregular flucuations ensued until 8h, September 12, after which normal conditions prevailed. The ranges recorded were: Declination, 20′.2; horizontal intensity, 95 gammas; vertical intensity, 160 gammas.
Harmonic analysis by means of linear combinations of ordinates
Authors: Labrouste H. , Labrouste Mrs.
Published: February 2008

This memoir on the method of analysis by means of linear combinations of ordinates comprises three chapters. The first is devoted to the statement of the principle of the method and the examination of the properties of the simple combinations by which are formed the multiple and resultant combinations which are dealt with in the second chapter. In the latter, the curves of selectivity of the different combinations are also discussed. Lastly, Chapter III deals with the practical method of analysis based on the theoretical considerations developed in the first two chapters. A numerical example is given, which illustrates the method. The case of damped sine‐waves is considered both from the theoretical (Chap. I) and the practical (Chap. Ill) point of view. So as to facilitate the reading of the memoir, we have put in small print the various paragraphs which, important though they may be from a theoretical or practical point of view, may however be left aside on a first perusal.
Some evidences of the dependence of diurnal variation on magnetic disturbance in the polar latitudes on longitude
Authors: Kwei C. T.
Published: February 2008

(1)Introduction—This paper originated in an attempt to find out whether the characteristic curves of diurnal variation of magnetically disturbed elements observed during auroral displays at Little America on the First Byrd Antarctic Expedition, as analyzed and presented by C. C. Ennis1, could be found also in a polar station in the Northern Hemisphere. The station chosen was Gjöahavn whose geographical coordinates are: Latitude,ϕ, =+68°.6 (+ signifying north),; longitude, λ, =264°.1 east. This station was occupied by Amundsen's Arctic Expedition from November 1903 to May 1905, a period of considerable solar activity.
Sitka Magnetic Observatory October to December, 1935
Authors: Hershberger John
Published: February 2008

(Latitude 57° 03′.0 N., longitude 135° 20′.1 or 9h 0lm.3 W. of Gr.)

October 20—The storm began about 10h.6, G. M. T., with a large increase in east declination and corresponding decreases in the two intensity‐components. The three elements immediately went into oscillations of large amplitudes and relatively short periods, which reached their maximum intensity about 11h.6. These continued until about 15h, when the amplitudes began to diminish and the elements gradually returned to their normal values. By 17h the storm had practically ended.
Cheltenham Magnetic Observatory October to December, 1935
Authors: Ludy Albert K.
Published: February 2008

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

October 20–22—A disturbance of moderate intensity began October 20 at about 9h. The ranges were not great, the disturbance being chiefly short‐period fluctuations. At about 11h 20m there began a bay in horizontal intensity, lasting about 45 minutes, followed immediately by another bay in the opposite direction of about the same duration. Beginning at about 5h 45m October 21, there occurred a bay in all three elements of about one‐hour duration. Other bays in declination occurred at 22h 30m October 21 and 2h 20m October 22. The disturbance ended about 22h October 22.
Biographical sketch of reverend father J. de Moidrey
Authors: Burgaud M.
Published: February 2008

Reverend Father Joseph Tardif de Moidrey passed away quietly at Shanghai, February 7, 1936, at the age of 78. A constant and interested reader of this JOURNAL, he was also a faithful correspondent. Born at Metz in 1858, he entered the Society of Jesus in 1876. In addition to the ordinary course of studies given in the Order, he began to prepare for a licentiate degree in mathematics.
Zürich Observatory
Authors: Brunner W.
Published: February 2008

The number of groups and spots on the Sun counted by the various observers may often differ widely. This applies particularly for the number of single spots, and much less for the number of groups. There are various reasons for the discrepancy in the counting of sunspots. A great difference may be due to the fact that observers use different instruments and also observe with different magnifying power, or one observer is counting the spots directly at the eyepiece of the telescope, a second in the projection on the screen, and a third observer is counting the spots from photographic plates.
Cheltenham Magnetic Observatory January to March, 1936
Authors: Ludy Albert K.
Published: February 2008

(Latitude 38° 44′.0 N., longitude 76° 50′.5 or 5h07m.4 W. of Gr.)

January 24–28—A moderate disturbance began at about 16h.5, January 24 and continued for several days, gradually diminishing until about 21h January 28. The greatest intensity of the disturbance occurred between 20h, January 24, and 5h, January 25. The ranges were: Declination, 21′; horizontal intensity, 100 gammas; vertical intensity, 87 gammas.
Sixth general assembly of the Association of Terrestrial Magnetism and Electricity at Edinburgh, Scotland, September 17–26, 1936
Authors: Fleming J. A. , Harradon H. D.
Published: February 2008

The Sixth General Assembly of the Union of Geodesy and Geophysics was held at Edinburgh, Scotland, September 16–26, 1936. The British National Committee, under the chairmanship of Professor S. Chapman, made excellent arrangements for the meetings of the Union and its seven associations. Social entertainment was provided by receptions by the Lord Provost, Magistrates, and Town Council of Edinburgh, and by His Majesty's Government, as well as by a number of teas and minor social functions. Two general excursions, in which social and educational elements were happily blended, were arranged—an all‐day journey by railway to the Highlands and an excursion on the Firth of Forth in the steamer Fair Maid. Special excursions were arranged for the various associations. Thus on September 23 the Association of Terrestrial Magnetism and Electricity was given a memorable motor‐coach trip, under the efficient direction of Dr. J. M. Stagg, to Eskdalemuir, where the Observatory was inspected and opportunity for personal contacts was afforded the delegates. On the return journey, the imposing ruins of Melrose and Dryburgh abbies were visited.
Publications relating to the polar year 1932–1933
Authors: la Cour D.
Published: February 2008

During the last few years many publications pertaining to the Polar Year 1932–1933 have appeared in the different countries. Nevertheless, a large number of these publications have not yet been supplied for the archives of the International Commission for the Polar Year despite the resolution on this point adopted by the International Meteorological Committee at its meeting at De Bilt in 1933, and again emphasized by the Conference of Directors at Warsaw in 1935.

In view of these facts, it is requested that there be sent to the Commission, if possible, five copies of all publications (small or large) relating directly or indirectly to the Polar Year which have not already been sent for its archives.
Watheroo Magnetic Observatory July to September, 1936
Authors: Green J. W.
Published: February 2008

(Latitude 30° 19′.1 S., longitude 115° 52′.6 or 7h 43m.5 E. of Gr.)

July 2—The disturbance recorded July 2 was of moderate intensity with definitely marked beginning at 1h 24m 40s GMT, as shown by record of the Crichton‐Mitchell vertical‐intensity inductometer. The elements were at their greatest divergence from normal between 12h and 13h. The disturbance ended at about 20h Ranges: Declination, 14′; horizontal intensity, 197 gammas; vertical intensity, 135 gammas.
On diurnal variation in cosmic‐ray intensity
Authors: Forbush S. E.
Published: February 2008

Cosmic‐ray data from precision cosmic‐ray meter records obtained at Cheltenham, Maryland, for 273 complete days during April 1935 to October 1936 are subjected to rigorous statistical analysis. The results indicate that the real barometric coefficient does not change from hour to hour or from month to month. It is shown that the barometric coefficient obtained at this station is in good agreement with certain results obtained from altitude‐intensity curves. It is furthermore shown, in two independent ways, that there is no indication of any external air‐temperature effect upon the recorded intensity. Finally, the data have been subjected to modern statistical methods which provide an objective measure for the probability that the observed diurnal‐variation is real. The results indicate, for the period covered by this analysis, a physically significant 24‐hour wave in apparent cosmic‐ray intensity, with an amplitude of 0.17 per cent of the total intensity having its maximum at about 11h, 75° west meridian mean time.
Hansteen's magnetic instrument
Authors: Wasserfall K. F.
Published: February 2008

Hansteen's historic magnetic instrument was, according to old documents, used on but one occasion after his death in 1873. This observation was made by the well‐known meteorologist H. Mohn in July 1882. As shortly afterwards a new unifilar magnetometer, Elliott No. 38, was provided, no further attention appears to have been given it.

In 1922 it was decided to undertake the study of the long series of observations with a bifilar at the Oslo Observatory, begun by Hansteen in 1843 and which has continued without interruption until the present time. When the author began the reduction of the series, he found the oscillation‐box among some other equipment left by Hansteen but the magnet belonging to the box could not be found. This absolute instrument was very primitive, but the exactness of Hansteen's observations with it is none the less astonishing.
Further studies on the vertical movements of the air in the upper atmosphere
Authors: Harang Leiv
Published: February 2008

Introduction—In a previous paper a number of observations partly of auroras and partly resulting from ionospheric studies were discussed and it was shown that a considerable diurnal temperature‐variation from night‐ to day‐conditions must exist at heights of and above 100 km. The following paper contains a discussion of the same subject supported by further observations. At the end of the paper a summary and discussion of the critical‐frequency determinations at noon of the ionized regions during April 1935 to November 1936 by the Breit and Tuve pulse‐method are given.
American URSI broadcasts of cosmic data October to December, 1936
Authors: Ennis C. C.
Published: February 2008

The data for terrestrial magnetism, sunspots, and solar constant are the same as given in previous tables.

The first three columns of the Table give (1) the magnetic character according to the scale 0–2 of the International Commission of Terrestrial Magnetism and Atmospheric Electricty, (2) the type featuring the day other than normal by the letters b, p, o, and i for days marked by bay, rapid pulsations, long‐period oscillations, and irregular oscillations, respectively, and (3) the hour and minute of Greenwich mean time marking the beginning of a storm, the end of the storm being indicated in the footnote to the Table. The next two columns give the data relating to sunspots: (1) the number of groups of spots and (2) the total number of spots. It is to be noted that sunspot‐numbers such as those from Zürich can be obtained from the number of groups and spots given in the Table by the formula N = k (10g + s), where the mean value of k for Mount Wilson was 0.53 during 1936.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory October, November, and December, 1936
Authors: Nicholson Seth B. , Sternberg Elizabeth E.
Published: February 2008

The magnetic storm of October 16–18 occurred during cloudy weather at Mount Wilson. An active group which crossed the central meridian on October 17.1 was 25° south of the center of the solar disc when the storm began, while another much smaller group, which crossed the central meridian on October 16.8, was 7° north of the center.

At the time of the November storm two large active spot‐groups were nearly at the central meridian, one crossing it on November 29.4,16° north, the other on November 29.4,11° south of the center of the solar disc.
Principal magnetic storms Sitka Magnetic Observatory October to December 1936
Authors: Hershberger John
Published: February 2008

(Latitude 57° 03′.0 N., longitude 135° 20′.1 or 9h 01m.3 W. of Gr.)

October 9–10—A moderate disturbance began about 7h.5 GMT, October 9, and continued with gradually‐increasing intensity until at about 8h 21m, October 10, the amplitudes suddenly became very large and the periods short, continuing so for about an hour, After this the elements gradually quieted down, and by 17h, October 10, the disturbance was practically over.
Apia Observatory October to December, 1936
Authors: Baird H. F.
Published: February 2008

(Latitude 13° 48′.4 S., longitude 171° 46′.5 or 11h 27m.1 W. of Gr.)

October 9–10—A moderate disturbance was introduced at 7h 28m GMT, October 9, by a slight sudden rise in horizontal intensity. The H‐trace showed undue fluctuations and gradually fell to reach a minimum of 34921 gammas at 7h 41m, October 10, thereafter gradually returning to normal.
Electrical potential‐gradient and conductivity of air near Rapid City, South Dakota
Authors: Sherman K. L. , Gish O. H.
Published: February 2008

Air‐potentials and air‐conductivity were recorded at a location about 15 miles south and west of Rapid City, South Dakota, during periods of preparations for the flight of Explorer II in 1935. The semi‐portable apparatus was installed in a hut on the rim of the natural bowl in which the balloon was to be inflated. The recorded values of air‐potentials were compared with several series of eye‐observations made on a plain about one mile away, in order to reduce the registrations to volts per meter. Positive and negative conductivity were recorded on alternate days with the single apparatus. The average values for selected complete days of record during June to July and during September to November, respectively, were: Potential‐gradient, 80 and 69 volts per meter; positive conductivity, 3.09 and 3.44×10−4 electrostatic unit; negative conductivity, 2.43 and 3.14×10−4 electrostatic unit. Harmonic analyses show that a 24‐hour component exists in gradient, in agreement with Mauchly's findings. A comparison with ocean‐values indicates that but a small part of the diurnal variation is of local character. The diurnal variation in air‐conductivity is approximately the inverse of that in gradient but of less amplitude. The product of the gradient and total conductivity—the electrical conduction‐current—therefore varies in a manner similar to the gradient.
Observations at secular‐variation stations in Mexico during April and May, 1937
Authors: Gallo Joaquín
Published: February 2008

During April and May 1937, R. O. Sandoval of the Magnetic Section of the National Astronomical Observatory of Mexico made observations of the absolute values of the magnetic elements at Oaxaca and Puebla. The results of these observations are shown in Table 1. Mr. Sandoval's instrument was CIW‐type magnetometer‐inductor No. 107 manufactured by the Precise Instrument Company, and the values shown in the Table are corrected to International Magnetic Standards.

At Oaxaca the station is at the airport 2.5 km from the Cathedral, ISO meters northwest of the north end of the hangar and four meters east of road to farm. It is marked by a wooden peg. True azimuths from south through west are: Cross, Merced Church, 34° 11′.2; cross Santo Domingo Church, 52° 18′3.
Auroral observations on August 1, 1937, at Malcolm Island, Canada
Authors: McNish A. G.
Published: February 2008

An interesting report of an auroral observation made at Pultney Point, Malcolm Island, near Vancouver Island, Canada, on August 1, 1937, has been received from Dr. T. G. Thompson of the Oceanographic Laboratories, University of Washington. The report states:

“About 23h 30m (probably 120° west meridian time) we noted a great beam of greenish light to the southeast. The beam shifted and moved from southeast toward the west and eventually took the form of an enormous shaft of light extending across the sky. It was considerably above the clouds and we got a very beautiful cloud‐effect. The light was reflected in the waters of Johnstone Strait much the same as moonlight.
Tucson Magnetic Observatory April to June, 1937
Authors: Hershberger John
Published: February 2008

(Latitude 32° 14′.8 N., longitude 110° 50′.1 or 7h 23m.3 W. of Gr.)

April 2–3—A disturbance began at 05h 02m GMT, April 2, the chief movement being an increase of 13 gammas in H. This was followed by several long, shallow bays, and at 12h the disturbance seemed to have ended. But at 16h there were a few shorter‐period oscillations in H and D, of small amplitude. These were followed by a marked depression in the average value of H, which lasted until about 07h, April 4. During this period the traces were relatively quiet except for a few bays between 02h and 07h, April 3.
The magnetic character of the year 1936 and the numerical magnetic character of days 1936
Authors: van Dijk G.
Published: February 2008

The annual review of the “Caractère magnétique de chaque jour” for 1936 has been drawn up in the same manner as for the preceding years. Fifty‐four observatories contributed to the quarterly tables; fifty‐two of them sent complete data.

Table 1 (reproduced from Table II of the annual review) contains the mean character of each day for each month. The lists of calm days and disturbed days, and the days recommended for reproduction are also reprinted here as Table 2.