bluuebunny/crossref_metadata_2025 huggingface dataset:
A search for possible effects of atmospheric electric discharge upon the potential gradient
Authors: Dwight C. H.
Published: February 2008

A search was conducted to determine whether there were at all times present in the atmosphere small electrical discharges, of the rapidity of lightning and perhaps continually taking place in the upper atmosphere. An apparatus was set up that would respond to rapid but not to slow fluctuations in the potential‐gradient. By photographic means as well as by direct inspection it was possible to count the number of rapid fluctuations in a given time. The possibility of any effect due to the motion of charged clouds nearby was shown to be nil.

It was found that, as far as the sensitivity of the apparatus permitted, there were no variations in the gradient that could not be attributed to lightning or other known causes. If there were any rapid changes in the atmospheric potential‐gradient, they were less than about 18 volts per meter, except in the case of thunder‐storms, when some interesting phenomena were observed.
Principal magnetic storms recorded at the Huancayo Magnetic Observatory, January to June, 1925
Authors: Parkinson W. C.
Published: February 2008

(Latitude 12° 02′.7S.; Longitude 75° 20′.4W., or 5h 01mof Greenwich.)

The first quarter was remarkably quiet magnetically, the following being the only disturbance worthy of note:
Principal magnetic storms recorded at the Cheltenham Magnetic Observatory, January to June, 1925
Authors: Hartnell Geo.
Published: February 2008

(Latitude, 38° 44′.0N; Longitude, 76° 50′.5, or 5h07m.4 W. of Greenwich.)
Studies concerning the relation between the activity of the Sun and of the Earth's magnetism
Authors: Bauer Louis A. , Duvall C. R.
Published: February 2008

Partial Abstract.—The variability with sunspot activity of the quantities a and b in the formula Q = a + b S, of the Wolf type, is investigated; Q is the quantity measuring the activity of the Earth's magnetism and S, the measure of solar activity. Using annual values of Q and S, it is found that a varies directly and b inversely with sunspot activity.

At first the Wolf‐Wolfer sunspot numbers, Sn, are used as measures of solar activity, but later other solar measures, sunspot areas, faculae, umbrae, flocculi, prominences, and solar‐constant values, are utilized. While the correlation coefficient, r, for a year‐to‐year comparison between various kinds of solar and of magnetic measures reaches values as high as 0.94, the comparison from month to month, or from day to day, may yield a correlation coefficient, considerably below 0.5, even after every care is taken to eliminate annual periodicities in the solar and magnetic measures.

The mean measures of solar activity for magnetically quiet and magnetically disturbed days during a solar cycle may be almost identical whereas the mean values of the magnetic measures for the two sets of days are very appreciably different.

None of the present measures of solar activity explain satisfactorily the various penomena of the Earth's magnetic activity on the assumption that there is a direct causal connection between sunspots and the Earth's magnetic disturbances.

For further conclusions, the interested reader may be referred to page 213.
The principles of the systematic application of geophysical methods of prospecting to mining and subterranean engineering
Authors: Ambronn Richard
Published: February 2008

Until a few years ago the research work accomplished by the geologist and the mining engineer for investigating the formations of mineral deposits in the Earth's crust—whether the object be purely or practically scientific—was confined almost exclusively to ascertaining and systematically arranging such empirical facts as could be derived by direct observation at easily accessible places on the surface of the globe, e. g., at exploring works, borings, or existing mines. The miner has been accustomed to say: “Behind the shoulder it is dark,” meaning thereby that the only facts to be taken into serious consideration as a certain basis for his technical and economic ventures and plans were those which he could observe with his own eyes. To such observations may be added all those which may be obtained by petrographic, chemical, or microscopic examinations of specimens taken from the localities in question.

The greater the progress of mining technique, the greater the depth at which ore, etc., can be profitably exploited. And on the other hand, the valuable deposits which can be discovered, and evaluated, by prospecting on the surface of the Earth only, are becoming more and more exhausted, so that one is obliged more and more to exploit formations lying in lower strata. The deeper these strata, the more difficult it becomes to draw, from the geological facts ascertainable on the surface, any reliable conclusions as to the conditions prevailing at these greater depths; at the same time the costs increase proportionately for the prospecting work requiring boring, sinking of shafts, and so forth. Thus the increased depth of the deposits involves a disproportionate increase of risk, when the old methods only are employed.
Principal magnetic storms and earthquakes, January 1926, at the Watheroo Magnetic Observatory with notes regarding aurora and cable and radio disturbances
Authors: Johnston H. F.
Published: February 2008

January 22–23, 1926.—This storm, though not of great severity, was characterized by a sudden commencement about 15h36m from previously very steady conditions. On the horizontal‐intensity trace, where the commencement was most marked, the change amounted to 54 gammas, if the commencement be regarded as being a sudden increase of the horizontal‐intensity Ordinate. However, it is possible that the beginning was a very rapid downward movement, followed by a more leisurely upward trend, since there is a slight darkening of the paper immediately under the point of commencement.
Principal magnetic storms recorded at the Apia Observatory, January to March, 1926
Authors: Thomson Andrew , Westland C. J.
Published: February 2008

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

January 26–27, 1926.—This storm is remarkable for the large number of rapid motions up and down shown on the horizontal‐intensity magnetogram. Maxima and minima sometimes follow one another at extraordinarily short intervals. A conspicuous example of this occurs at 23h 53m, when the value changes from 35166γ to 35293γ, a rise of 127γ in 7 minutes. Then the curve immediately turns back again and returns to 35178γ, a fall of 115γ again in 7 minutes. The curve is even steeper than this at 17h 57m, where a fall of 92γ is registered in two minutes (35253γ to 35161γ), and several other instances of movements not much less rapid could be mentioned. There are two maxima and minima which are conspicuous among the extreme values recorded, namely: January 25, 16h 28m, H = 35317γ and Z = 20488γ; January 25, 18h 40m, H = 35104γ and Z = 20420γ; January 26, 0h 04m, H = 35293γ and Z = 20490γ; January 26, 1h 12m, Z = 20435γ; January 26, 2h 23m, H = 35062γ. The end of the violent disturbance is at 4h, but there is still some milder disturbance after this time.
Provisional sunspot numbers for April and May, 1926
Authors: Wolfer A.
Published: February 2008

(Latitude 14° 35′ 48′′N.; longitude 121° 10′ or 8h 04.m 7. of Greenwich.)

Besides the above, miner disturbances occurred as follows: January 18 at 9h to January 19 at 4h; January 22 at 15h 37m to January 23 at midnight; February 17 at 15h 36m to February 18 at 5h; March 5 at 10h 10m to March 6 at noon; March 9 at 5h 26m to March 10 at 8h 30m; and March 11 at 0h to March 12 at 4h 40m.
On micromagnetic oscillations of type II
Authors: Pödder Arnold
Published: February 2008

In my article “Micromagnetic Oscillations as Observed at the Magnetic Section of the Observatory of Irkutsk (Zouy), 1925,” I considered the micromagnetic oscillations of type I, observed with the aid of the sensitive Eschenhagen magnetograph (the sensitiveness of the Lloyd's balance is 1 mm. = 1.3γ; that of the apparatus for horizontal intensity is 1 mm. = 0.34γ, and a velocity of rotation of the drum with the photographic paper is l min. = 15 mm.), and having periods from 4 to 15 seconds. As for the micromagnetic oscillations of type II, with periods averaging about 34 seconds, I calculated only the mean monthly values of the periods and the amplitudes for 1925.

Examination of this data revealed some regularity of a change of periods and amplitudes, consequently I decided to treat the above‐mentioned observations in another manner, namely as Dr. W. van Bemmelen treated micromagnetic oscillations or pulsations, as he denominates them, for Batavia and Buitenzorg.
Principal magnetic storms recorded at the Huancayo Magnetic Observatory for April to June, 1926
Authors: Goddard Richard H.
Published: February 2008

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

April 14, 1926.—A disturbance of considerable intensity began on April 14 at 14h 02m, with a sudden commencement. The horizontal intensity increased within six minutes of time by about 110γ. High values of H occurred at intervals until 20h with large fluctuations; within the next hour the force decreased greatly, the spot going beyond the limits of registration, remaining lost, except for brief periods, until 13h on April 15. A series of large fluctuations then brought the spot back to the paper, but the value remained low until the following day, when normal conditions were gradually resumed. The sudden commencement of this storm was also shown in the D and Z traces.
Comparison measurements between the Abinger and the N.P.L. standard horizontal force magnetometers
Authors: Dye D. W.
Published: February 2008

I. Introductory.

The National Physical Laboratory possesses a standard Absolute Horizontal Force Magnetometer based on a method due to Schuster. The construction and use of this magnetometer has been fully described in a paper by F.E. Smith.
Hourly ranges of the north component of magnetic force at Eskdalemuir
Authors: Watson R. A.
Published: February 2008

The range of the North Component of Magnetic Force during each hour centered at the hour G. M. T. has been measured from the Eskdalemuir magnetograms for many years. This preliminary investigation deals with the hourly ranges so obtained in June and December, 1915–1926, omitting 1920 and December, 1926. During this period the scale value was so constant that the curve readings can be used without individual conversion. The years 1921, 1922, 1923, 1924 are classed together as years of small sunspottedness (SM); 1915, 1916, 1917, 1918, 1919, 1925, 1926, are years of great sunspottedness (SX). 1920 is omitted as an intermediate year, and the values for December, 1926, are not as yet available.
A statistical study of the effects of the atmospheric‐electric elements on broadcast reception
Authors: Cairns J. E. I.
Published: February 2008

An attempt is made to correlate the variations in broadcast reception with the variations of the atmospheric‐electric elements, positive and negative conductivity, and potential gradient. Two analyses are given, the one dealing with the results obtained for all days, regardless of the local disturbing effects of smoke, rain, etc., on the atmospheric‐electric elements, and the other dealing with the results from “selected” days, that is, days that are considered to be free from any such local effects.

The result of the first analysis shows that when the conductivity, both positive and negative, is subnormal, there is a greater probability of there being better signal reception; the potential gradient, apparently, has little effect. However, the results of the analysis for “all days” is not considered to be of the same value as the results for “selected” days because of the disturbances caused by rain, etc., on the atmospheric elements, disturbances which are most prevalent during the winter, when signal strength is higher.

From the analysis for “selected” days it appears that the positive conductivity has little effect on the received signals, whereas when the negative conductivity is low the signals are stronger. Also, better signals are received when the potential gradient is high.

No comment is made on the results other than to state that they are of sufficient interest to induce the writer to carry out quantitative measurements during the year 1927.
On the use of a radioactive collector for potential‐gradient measurements
Authors: Tuve M. A. , Huff C.
Published: February 2008

The experiments reported in this paper comprise a laboratory study undertaken to gain a better understanding of the action of the ionium “collector” which is used in atmospheric potential‐gradient determinations. It has been possible to study also some of the sources of error which affect such observations. The investigation is more complete in some respects than that of M. Moulin.

APPARATUS.
The magnetic character of the year 1926
Authors: van Dijk G.
Published: February 2008

The “annual review” of the “Caractère magnétique de chaque jour” for 1926 has been drawn up in the same manner as for the preceding year. Forty‐three observatories contributed to the quarterly reviews; all of them sent complete data. In the introduction of the “review” a note has been inserted concerning disturbed days. In the meeting of the Commission for Terrestrial Magnetism and Atmospheric Electricity of the International Meteorological Committee at Zürich, September 17, 1926, it was agreed that certain days included amongst the five most disturbed days of the month, should be included amongst the days selected for the calculation of the diurnal irregularities. Days of character 2.0 should be excluded and other highly disturbed days, on which loss of trace had occurred.
Memorandum on the uncertainty in the amplitudes and phase‐angles of Fourier terms
Authors: Duvall C. R.
Published: February 2008

The word uncertainty, as used here, is a general term for the measures of accuracy used in least squares, viz.: probable error, mean error, and mean square error.

In any particular Fourier analysis the uncertainties may be gotten from the residuals in the usual way, since the Fourier analysis is a least‐square adjustment of the given ordinates to the harmonic form.
Magnetic storm of April 13–14, 1927, as recorded at the U.S. Coast and Geodetic Survey Magnetic Observatory at Cheltenham, Maryland
Authors: Hartnell George
Published: February 2008

The storm was of only moderate intensity but it is of especial interest because of the serious interference with telegraphic communication, especially in Canada, occurring at the same time, and the presence on the Sun of an unusual distribution of small sunspots. The storm began abruptly at 23h 48m, Greenwich mean time, on April 13th. After the characteristic features of a sudden commencement, conditions were fairly quiet from 1h to 5h 22m on April 14th, when the principal portion began, which lasted until about 17h.

At the beginning there was a sudden increase in west declination of 3′.2 followed immediately by a decrease of 5′; a sudden decrease in horizontal intensity of 27γ followed by an increase of 36γ to the maximum value of 18860γ at 23h 49m; the beginning in vertical intensity was scarcely perceptible. The extreme values occurred as follows:
Principal magnetic storms recorded at the Apia Observatory, July to December 1926, and preliminary report on annual values of the magnetic elements for the year 1926
Authors: Thomson Andrew , Westland C. J.
Published: February 2008

(Latitude, 13° 48′.4 S.; longitude, 171° 46′, or 11h 27m.1 W. of Greenwich.)
Preliminary report on Terrestrial Magnetism and Electricity at the Prague Assembly, September 3 to 10, 1927
Authors: Bauer Louis A.
Published: February 2008

There were nine meetings of the Section, all being well attended, to which reports were presented from many of the 27 nations represented at the Assembly.

The report on proposed French work in Indo‐China and in the Pacific was of special interest. Reports from the United States, including that of the United States Coast and Geodetic Survey and that of the Department of Terrestrial Magnetism of the Carnegie Institution of Washington, were well received; the latter contained much material relating to international work. Several progress reports were submitted on the development of instruments to record the abrupt beginnings of magnetic storms.
Principal magnetic storms and earthquakes recorded at the Watheroo Magnetic Observatory, January to October, 1927
Authors: Johnston H. F.
Published: February 2008

January, February, and March, 1927.—There were no marked disturbances during these months.

April 14, 1927.—Mr. D. Macpherson of Woodward Street, Coolgardie, Western Australia, reported that an aurora was visible there for a period of 15 to 20 minutes at approximately 20h on April 14. This is 12h Greenwich mean time and is near the midpoint of the storm of April 13 to 15. The second portion of this moderately severe and protracted storm was the heavily disturbed portion.
Principal magnetic storms recorded at the Huancayo Magnetic Observatory, April to July, 1927
Authors: Torreson Oscar W.
Published: February 2008

April 13–15, 1927. A magnetic storm of moderate intensity began at 23h 48m April 13, 1927, with a sudden commencement in all three elements. The horizontal intensity increased 54γ almost instantaneously, and the declination and vertical intensity were marked by smaller but conspicuous increases. After the sudden commencement there was a 5‐hour period of minor disturbance in all three elements.
Program of scientific work on cruise VII of the Carnegie, 1928–1931
Authors: Fleming J. A. , Ault J. P.
Published: February 2008

After an interval of over six years, the Carnegie is to start out again on May 1, 1928, for a world‐wide cruise extending over a period of three years. This will be the seventh cruise of the vessel and, as indicated by the tentative schedule below and Fig. 1, will add nearly 105,000 nautical miles to the present total of nearly 253,000 miles traversed in all oceans during cruises I to VI (1909–1921). A more general program of scientific work is to be undertaken than on previous cruises. In addition to investigations in terrestrial magnetism and atmospheric electricty, some work in physical and biological oceanography is to be attempted.
Ein Vorschlag von Leibniz zu ausgedehnten erdmagnetischen Beobachtungen
Authors: Kassner Von C.
Published: February 2008

Als im Jahre 1700 in Berlin die “Königliche Societät der Wissenschaften,” später Akademie genannt, gegründet worden war, suchte Leibniz auf alle möglichen Weisen dem preussischen König Friedrich I die Förderung der Wissenschaften nahe zu legen, und so entstand im November 1701 eine Denkschrift, worin Leibniz dem König empfahl, Missionäre in besonderen Anstalten wissenschaftlich ausbilden zu lassen und sie dann nach Russland, Türkei, Persien, Indien, und China zu senden. Dort sollten sie neben ihrer Predigertätigkeit teils als Lehrer der Wissenschaften auftreten, teils wissenschaftliche Studien machen und so die Beziehungen dieser Länder zu Preussen fördern, was sich dann auch in Handelsgeschäften auswirken werde.

In dieser Denkschrift rät Leibniz, man solle dem jetzt nach Moskau gehenden Residenten (Gesandten) einen so vorgebildeten jungen Mann beigeben, der dann vielleicht von dem Zaren (Peter dem Grossen)1 “in die Provinzen zu observieren geschickt würde. Ks ist nämlich bekannt, dass der Zar die Schiffahrtssachen liebt, und der Kompass gleichsam als die Sache der Seefahrt zu achten ist, er aber von Norden etwas abweicht und zwar an unterschiedenen Orten unterschiedlich. Hierin steckt ein noch nicht gelöstes Rätsel der Natur, das aber, wenn es vollends entdeckt würde, ein Hilfsmittel zur Längenbestimmung und eine überaus grosse Hilfe für die Schiffsführer darbieten würde. Zu solchem Zwecke habe man schon seit langem gewünscht, dass magnetische Linien auf einer Karte oder auf einem Erdglobus gezogen werden möchten, wobei die Linien immer durch örter mit gleicher Deklination gehen sollen. Diese Karte hat nun ein Engländer aus eignen und ändern Schiffstagebüchern ganz kürzlich entworfen (Halley 1701). Weil aber die Linien darin nur auf der See gezogen sind und aufhören, wo das Land anfängt, so wäre es höchst nützlich und, um dieses Geheimnis vollends zu entdecken, dienlich, dass in Königlicher Majestät Ländern vom Rhein bis an den Pregel und dann weiter durch das Moskauische Reich bis nach Persien, Indien, und China die magnetischen Beobachtungen fortgesetzt und damit die Linien durch den nördlichen Orient, allwo man am wenigsten solche Beobachtungen hat, fortgezogen würden. Hierzu wäre jemand besonders zu instruieren, und ohne Zweifel würde der Zar auf Eurer Königlichen Majestät Empfehlung und auch aus eigener Neigung zu allem, was die Schiffahrt angeht, sich dieser Sache wie eines eignen Werkes annehmen und den Beobachter überall mit Fuhrwerk.”
Principal magnetic storms recorded at the Huancayo Magnetic Observatory, August to December, 1927
Authors: Torreson O. W.
Published: February 2008

August 19–21, 1927.—A mild magnetic storm began at 11h55m on August 19, with a small but abrupt change in the horizontal intensity and the declination but with hardly noticeable change in the vertical intensity. The storm is prominent for duration rather than for large or severe perturbations. From the commencement until 20h on the 20th the usual diurnal variation is followed but with occasional small peaks and bays breaking up the uniform trend.
The sensitivity of magnetic variometers
Authors: McComb H. E.
Published: February 2008

Variation with ordinate in sensitivity of the horizontal‐intensity variometer, San Juan Magnetic Observatory, Puerto Rico, was determined in a short time by observing scale‐values over a wide range of ordinate, the ordinate being changed by torsion or by an auxiliary deflector. In order to test the efficiency of a new type of vertical‐intensity variometer pivot, scale‐values were observed at Cheltenham Magnetic Observatory, Maryland, U.S.A., over the complete range of sensitivity of the recording magnet‐system by method of deflections, of oscillations, and of weights. The values obtained from deflections were reconciled by the adoption of proper distribution‐coefficients using the method of least‐squares for their determination. The paper summarizes and discusses briefly the experimental data obtained at the two observatories.
Geophysical methods of prospecting, with special reference to magnetic, radioactive, and electric methods
Authors: Heiland C. A.
Published: February 2008

Geophysical methods of prospecting may be divided into two groups of a different character, as indicated in Tables 1 and 2. The first group comprises methods (for example, gravitational) by which direct effects of subterranean inhomogeneities are observed. The second group consists of procedures (for example, seismic, magnetic, radioactive, and electric) whereby artificial fields of force are produced and their distortion by subterranean bodies of different physical properties is measured. This paper is to discuss briefly the magnetic, the radioactive, and the electric methods of prospecting.
Depths of ground‐water and other subsurface features indicated by Earth‐resistivity surveys
Authors: Gish O. H.
Published: February 2008

In the course of the earth‐resistivity surveys made as part of the program for earth‐current investigations by the Department of Terrestrial Magnetism of the Carnegie Institution of Washington, it has become evident that the method used is capable of locating and ascertaining the depth of various subsurface geological features.

In the paper presented the general features of the method previously described elsewhere were briefly reviewed. The manner of adjusting and using the specially designed commutator so as to obtain measurements under steady current‐conditions; that is, obtaining the potential measurements over a portion of the “square‐wave” cycle well removed from the make and the break, was explained.
Transmission of elastic waves through surface‐rocks
Authors: Goranson Roy W.
Published: February 2008

Elastic disturbances are propagated through rock in a definite determinable manner. The path and speed of the waves set up are dependent on the elastic constants of the medium traversed. A knowledge of the subsurface structure of the Earth's crust is given from the data furnished by seismograph‐records of earthquake disturbances for distances up to a thousand kilometers, corresponding to depths of something over one hundred kilometers. Such rock‐structures, when reproduced on a small scale, give similar seismograph‐records.
Variations of solar radiation
Authors: Abbot C. G.
Published: February 2008

It will be recalled that while observations of the solar constant of radiation by the fundamental method of Langley, which involves measurements on clear days from low to high Sun, are made by the Smithsonian Institution under many types of sky as a basis, and later occasionally as check observations, most of the daily solar‐constant work is carried on by the abbreviated method depending upon measurements of the brightness of the sky around the Sun as an index of the atmospheric transparency. Inasmuch as the energy‐curves at the Earth's surface are greatly affected by the water‐vapor bands, and it is impossible to know just where the smooth curves would run over the tops of these wide bands in the bolographs, there is always a possibility that minute errors in the final results, either by the long or by the short method, depending upon the prevailing atmospheric humidity, will persist.

In order to eliminate these systematic errors it is necessary to collect a long series of observations made under comparable conditions of apparatus, and box them with reference to the quantity of precipitable water contained in the atmosphere on the days of observation to determine the residual correction as a function of the prevailing humidity. In doing this, allowance has to be made for the variability of the Sun during a long series of observations extending perhaps over several years, else effects due to solar changes would be confused with those really due to the atmosphere. In former discussions a combination of the observations made in the northern and southern hemispheres has been employed to fix these allowances for solar variation. This procedure, while theoretically sound, has been objected to by critics, as tending to take away the independence of stations, and accordingly we have substituted another method based upon the principle of selected pyrheliometry, so that each station now stands by itself, absolutely independent of all others.
Auroral observations, radio reception, and magnetic conditions at the Sitka Magnetic Observatory, August 1927 to June 1928
Authors: Ulrich Franklin P.
Published: February 2008

This report is a continuation of the investigation, begun in 1923, of the relation between aurora and the Earth's magnetic field and of the effect of the aurora and magnetic conditions upon radio reception.

The program of the work has been divided into four parts: (a) The observation of the aurora at the Sitka Magnetic Observatory with a comparison of the Earth's magnetic field; (b) reports of aurora observed at various radio stations throughout Alaska; (c) a record of the daily reception of radio at Sitka and Fort Yukon, with a comparison of the magnetic conditions, and (d) a log of the auroral frequency.
Principal magnetic storms recorded at the Watheroo Magnetic Observatory, April to May, 1928
Authors: Johnston H. F.
Published: February 2008

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

May 27–29, 1928—The storm of May 27 to 29 was prolonged but of mild severity and characterized by long‐period oscillations. The storm began May 27 at 13h 28m in declination and vertical intensity and at 13h 26m in horizontal intensity, and ended May 29 at 20h 17m, the ranges being as follows: Declination, 22′.2; horizontal intensity, 179 gammas; vertical intensity, 172 gammas. The preliminary comparatively quiet period lasted until 3h on May 28, when the greatest changes in the elements began. These were steady and progressive during the second period, which lasted until 8h. The third period of 16 hours was characterized by long‐period oscillations of moderate amplitude. The fourth period began at 0h on May 29, during which there was a gradual recovery to normal values.
Principal magnetic storms recorded at the Sitka Magnetic Observatory, April to June, 1928
Authors: Cotton Harold A.
Published: February 2008

(Latitude 57° 03′.0 N.; longitude 135° 20′.1 or 9h 01m.3 W. of Gr.)
Preliminary results of ocean magnetic observations on the Carnegie from Reykjavik to Barbados to Balboa, July to October, 1928
Authors: Ault J. P.
Published: February 2008

The Carnegie left Reykjavik at noon on July 27, 1928, going out under her own power against a head‐wind. By 14h the entrance point of the bay was cleared. Heading down toward Cape Farewell, good progress was made for the first four days. On July 31 the winds became unfavorable, and on the next day they went calm and it was necessary to operate the engine.
Einige wichtige planetare Ursachen für die Schwankungen der Sonnentätigkeit und des Erdmagnetismus im Jahre 1926
Authors: Göschl Von Franz
Published: February 2008

Im Augustheft 1927 der Annalen der Hydrographie behandelte ich “Kosmische Einflüsse auf die erdmagnetischen Schwankungen” und in einem Aufsatze des Jahrganges 1928 derselben Zeitschrift “Die Einwirkung der äussersten Planeten auf die Sonnenflecken.” Von der erstgenannten Abhandlung erschien ein Referat im Aprilheft 1928 der Meteorologischen Zeitschrift mit einer Anwendung auf die Erläuterung des erdmagnetischen Charakters 1926, die durch eine Tabelle veranschaulicht wurde. Hier möge mittels eines Diagrammes der Ablauf der magnetischen Schwankungszahlen des gleichen Jahrganges aus den im erstgenannten Aufsatze dargelegten Gesetzmässigkeiten erklärt werden. Da aber als primäre Erscheinung doch sicher die Einwirkung der Planeten auf die Sonnentätigkeit anzusehen ist, soll zuvor im ersten Teil in wenigen Strichen eine Tabelle die wichtigsten derartigen Beziehungen veranschaulichen.
Note on the ultraviolet light of the Sun as the origin of auroræ and magnetic storms
Authors: Maris H. B. , Hulburt E. O.
Published: February 2008

A theoretical investigation has been made of the outlying regions of the atmosphere of the Earth and of the effect of sunlight on these regions; certain of the conclusions are given in this preliminary note. By the usual methods the temperatures and the pressures of the atmosphere to great heights were calculated for a quiet Sun, that is for the Sun in its normal state, with no terrestrial auroræ or magnetic storms. Because of the unequal balance at cold temperatures between the solar energy absorbed in the ultraviolet by the atmospheric gases and the energy re‐emitted in the infra‐red by the gases, the daytime temperatures above 100 kilometers were found to increase with the height above the surface of the Earth until at 300 or 400 kilometers temperatures of 1000° Kelvin seem reasonable. (There is of course nothing novel in this, although we have been interested in working the matter out more exactly perhaps than has been done heretofore.)
The diamagnetic theory of undisturbed terrestrial‐magnetic variations
Authors: Gunn Ross
Published: February 2008

In an earlier paper2 the writer outlined a theory of the terrestrial‐magnetic variations based on diamagnetism existing in the upper atmosphere. The diamagnetism of the region was shown to follow from simple considerations of the motion of ions or electrons which spiralled about the Earth's magnetic field as a result of their thermal agitation. It is the purpose of this paper to extend the original ideas and supply certain evidence supporting the theory that was not advanced in the original paper.

It has been shown2 that the intensity of magnetization I of an ion gas due to the thermal agitation of the ions is given by

urn:x-wiley:00968013:media:tma31313:tma31313-math-0001where N is the number of ions of all kinds per cubic centimeter, m the mass of the ion, V the component of the velocity of the ion perpendicular to the impressed magnetic field H, κ the Boltzmann constant, and T the absolute temperature. These relations have been deduced on the assumption that the free‐path is long and it becomes necessary to establish a criterion for the existence of long free‐paths. The free‐path, λ, of an ion in a gas made up of N molecules or ions per cubic centimeter, and having a kinetic‐ theory diameter σ is given by
Variometer scale‐value determinations with a large deflector
Authors: Ludy A. K.
Published: February 2008

Vertical and horizontal‐intensity variometer scale‐values were determined by the usual method of using a small deflector at short distances and a large deflector at great distances. The results indicate that the latter method has several advantages and is to be preferred.
On certain sources of error in determinations of magnetic declination
Authors: Ljungdahl Gustaf S.
Published: February 2008

In a magnetometer, fitted with an optical collimating‐system attached to the magnet, a possibility exists of corrections, which are due to defects in the lens. A perfect magnetometer ought not to have any corrections at all in determinating D. A criterion of non‐correction is given. Errors of observation may be diminished by pointing on more than one reticle in the field of view of the telescope.
Sebastian Jacob Mauchly, 1878–1928
Authors: Gish O. H.
Published: February 2008

Dr. Sebastian Jacob Mauchly, Chief of the Section of Experimental Work in Terrestrial Electricity at the Department of Terrestrial Magnetism of the Carnegie Institution of Washington, died December 24, 1928 after a long and baffling illness. He was born at Swanton, Ohio, July 9, 1878, attended the University of Ohio, the University of Chicago, and the University of Cincinnati. From the latter institution he received the degree A.B. in 1921 and Ph.D. in 1913. His academic work was interspersed with the teaching of physics in high schools from which he carried a lasting interest in pedagogical problems.
Tilting deviations in magnetic declinations
Authors: Peters William J.
Published: February 2008

Experiments were made by swinging compasses in a wooden swing for the purpose of investigating deviations caused by the ship's rolling motion. Results obtained with various types of compasses are submitted in two tables. Dynamic deviations, the kinetic equilibrium error, and conditions other than those considered in these two theories are briefly discussed. Equations are given for computing the direction and relative strength of the apparent gravitational field as affected by the accelerations of the rolling motion. These are used to determine the maximum angle of tilt produced by the maximum angle of roll. The kinetic equilibrium error for an angle of tilt in one direction is shown to be different for an equal angle of tilt in the opposite direction for certain elements in certain directions of the axis of tilting and hence give rise to deviations. Examples are given for the three magnetic elements for instantaneous values of tilting. The computed deviation in declination that results in the case of a magnet having large moment of inertia, constrained to move about an axle parallel to the radius of swing, and having considerable damping has been found to be much smaller than would be indicated by the results of the experiments for the same conditions. It is concluded that this theory of tilting deviations does not account for the whole deviatipn observed and must be regarded as only contributing a part of the effect as does also the theory of dynamic deviations.
Die Energiemasse und der Elektrizitaetshaushalt der Erde
Authors: Maneff G.
Published: February 2008

Es wird versucht, mit Hilfe der Inversion des Gravitations‐ und Elektromagnetischen Feldes, den Elektrizitätshaushalt der Erde und die Frage nach der Natur des Gegenstromes, wie auch die physikalische Ursache des Erdmagnetismus klarzulegen.
The relative frequency of thunderstorms throughout the day over the oceans and in the tropics
Authors: Wait G. R.
Published: February 2008

The data published on the frequency of thunderstorms throughout the day over the oceans are not plentiful; those available seem to give a maximum during the night hours, particularly between 20 and 4 hours. Humphreys1 offers an explanation for this observed phenomenon, while Whipple2 would expect it to occur at another time of the day. The latter believes the observational data are at fault since storms are more easily observable during the night hours. To obtain a record of thunderstorms over the oceans entirely free from Whipple's objection, the hours during which a negative potential was recorded with the potential‐gradient recorder have been used (see Table 2).
Cheltenham Magnetic Observatory, April to July, 1929
Authors: Hartnell Geo.
Published: February 2008

There were no storms during April to June, 1929.

July 14–18, 1929—A magnetic disturbance began July 14 at 16h 30m but assumed no importance until from lh to 2h July 15. There were bends in the curves giving ranges: Declination, 32′; horizontal intensity, 84γ; vertical intensity, 80γ. There were bends July 15 from 6h to 7h giving ranges: Declination 15′; horizontal intensity, 60γ; vertical intensity, 60γ. During the hour preceding midnight July 15 there were bends giving ranges: Declination, 20′; horizontal intensity, 80γ; vertical intensity, 80γ. On July 16 from 19h 30m to 20h 30m there was a change in horizontal intensity of 100γ, and vertical intensity rose to 60γ above normal. At other times the curves were slightly disturbed.
Preliminary values of the annual changes of the magnetic elements in the Caribbean Sea and the Pacific Ocean, as determined from the Carnegie results, 1909–1929, and from the Galilee results, 1905–1908
Authors: Ault J. P. , Físk H. W.
Published: February 2008

This is the second paper giving the preliminary values of the annual changes of the magnetic elements for the various oceans, as deduced from all the observations on the Galilee, 1905–1908, and on the Carnegie, 1909–1929, including the results of Cruise VII to date. The first paper1 gave the results for the North Atlantic, including Cruise VII observations from Washington, May 1, 1928, to Barbados, September 17, 1928. The present paper gives the results for the Caribbean Sea, the South Pacific Ocean, with a few values in the North Pacific Ocean, including observations of Cruise VII from Barbados, October 1, 1928, to San Francisco, July 28, 1929.

Various stations in the vicinity of intersections of Cruise VII, 1928–1929, with previous tracks have been utilized. The 1928–1929 values are not final, but the small corrections to be made at the completion of the cruise will not change the annual‐change values given herein. The method used was the same as indicated in the first paper and as described on page 185 of Volume V, “Researches of the Department of Terrestrial Magnetism,” use being made of the United States Hydrographic Office magnetic charts for 1925. The observations have not been corrected for diurnal variations since corrections for these are in general negligible for the times of observation on board the Carnegie.
Zodiacal light and magnetic storms
Authors: Hulburt E. O.
Published: February 2008

From April 1853 to April 1855 Rev. George Jones, U. S. N., observed the zodiacal light every night, weather and other things permitting. A comparison of his record with the Greenwich magnetic storm‐list gave the following results: In this period there were 26 magnetic storms, or storm‐groups, and 23 periods of abnormal zodiacal light, 16 of which followed within three days after a magnetic storm. Ten storms occurred on dates for which there were no zodiacal‐light observations, and there were seven cases of abnormal zodiacal light with no accompanying magnetic storms listed. The abnormalities in the light were mainly fluctuations, and sometimes an unusual brilliance or distribution in the heavens.
Preliminary note on the atmospheric potentials recorded with ionium‐collectors
Authors: Builder Geoffrey
Published: February 2008

A laboratory investigation is discussed of the characteristics of ionium‐collectors preliminary to a fuller investigation of the potentials recorded by their use in atmospheric potential‐gradient installations. Earlier work on the permissible leak of such installations and the determination of the activity of the collectors is further developed.

An improved method of calculation, suggested by Gish, for the determination of the apparent conductance of the collectors is given. The values of conductance obtained vary with the air‐potential at the collector, the conduction not obeying Ohm's law. Determinations in stagnant air give values of the conductance which are much lower than those found in moving air.

The steady value of potential recorded in an air‐current is about four per cent lower than the calculated air‐potential at the collector for a disc‐collector placed face down. With rod‐collectors suspended horizontally and for disc‐collectors with the active face vertical the recorded potentials agree, within the limits of experimental error, with the calculated air‐potentials at the collector.

The potentials recorded in stagnant air are as much as ten per cent higher than the steady values obtained in a current of air, if the insulation of the system is good. With excessive leak from the collector‐system to earth the recorded potential is lowered by three to four times as much by the leak as it is if an air‐current is maintained between the parallel plates used to produce a steady artificial field. These effects are briefly discussed.
Provisional sunspot‐numbers for December 1929 to February 1930
Authors: Brunner W.
Published: February 2008

(Dependent alone on observation at Zürich Observatory and its station at Arosa)
Huancayo Magnetic Observatory October to December, 1929
Authors: Ledig Paul G.
Published: February 2008

(Latitude 12° 02′.7 S.; longitude 75° 20′.4 or 5h 01m W. of Gr.)

October 7, 1929—At about 9h a short magnetic storm of moderate intensity began in all three elements and continued through the day and until about 2h on October 8, though magnetic conditions continued disturbed for over two days more. The only distinctive phenomenon of the storm was the unusually, high maximum in the horizontal intensity; 390γ above the base‐line at 15h 46m.
A preliminary list of antarctic and a supplementary list of arctic magnetic determinations
Authors: Weinberg Boris
Published: February 2008

The purpose of publishing the following lists is the same as that for publishing the preliminary list of arctic magnetic determinations.1 The supplementary list of references for arctic determinations is based chiefly upon the researches of the author in the principal libraries of Berlin, London, and Paris, and upon communications of unpublished results by D. la Cour, the United States Coast and Geodetic Survey, and the Greenwich Observatory. The term “antarctic” is conventionally defined as that part of the globe to the south of latitude 65° south.
Earth‐inductor measurements aboard the Carnegie, Cruise VII
Authors: Soule Floyd M.
Published: February 2008

On the recently ended last cruise of the non‐magnetic vessel Carnegie the earth inductor was used for the routine measurement of inclination and, experimentally, for the measurement of the horizontal intensity of the Earth's magnetic field.
Preliminary report on atmospheric potential‐gradient observations at Christchurch, New Zealand, 1928–1929
Authors: Skey H. F.
Published: February 2008

Observations of the electric potential of the atmosphere have been obtained at Christchurch Magnetic Observatory (latitude 43° 32′ south, longitude 172° 37′ east, altitude 25 feet above sea‐level) since August 1, 1928. Continuous records are obtained by means of a Benndorf electrograph which is housed in a small building in Hagley Park. The building is placed in a clear area of the Park and is approximately three‐quarters of a mile from Cathedral Square in the center of the city of Christchurch. The electrograph gives a record of the potential of an ionium‐collector which is mounted on an insulated arm projecting horizontally from the side of the building.
Magnetic storms and disturbed days, Apia Observatory, Samoa, January, 1929, to March, 1930
Authors: Thomson A. , Westland C. J.
Published: February 2008

The magnetic records of 1929 resemble those of 1928 in showing a large number of disturbed days, but in both years, it is noticeable that although the disturbances are frequent, they are certainly small. The following table shows details of the principal storms recorded in 1929 and 1930.

The first storm of 1929 recorded on February 28 is merely part of a prolonged period of disturbance which sets in about February 26d 19h. There is a sharp deflection upward from a smooth part of the trace, but the amount of this increase in H is only 13γ. The minimum in H is 35039γ at 28d 0lh 25m.
Early declination‐observations, Kamchatka to Bering Strait
Authors: McFarland W. N.
Published: February 2008

This article contains a list of measurements of the magnetic declination at twenty‐three points along the Siberian coast from Kamchatka to Bering Strait, as observed by the officers of Bering's expedition of 1728 and 1729, together with a declination‐chart of the region based on the observations.
Das neue Observatorium in Niemegk
Authors: Nippoldt A. N.
Published: February 2008

Am 23. Juli ds. Jahres wurde das neue Observatorium in Niemegk feierlich eingeweiht. Ausser den Vertretern der staatlichen und städtischen Behörden waren eine grössere Anzahl Fachgelehrte aus dem ganzen Reiche erschienen. Eine besondere Bedeutung erfuhr die Weihe dadurch, dass der Tag zugleich der 70ste Geburtstag des früheren Leiters des Magnetischen Observatoriums Potsdam war, des Herrn Geheimrat Professor Dr. Adolf Schmidt und unter Anwesenheit des Jubilars vor sich gehen konnte. Der Staat ehrte ihn noch besonders dadurch, dass das neue Observatorium den Namen erhielt: “Adolf‐Schmidt‐Observatorium für Erdmagnetismus.”
Provisional sunspot‐numbers for July to November, 1930
Authors: Brunner W.
Published: February 2008

(Dependent alone on observations at Zurich Observatory and its station at Arosa)
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, April to September, 1930
Authors: Nicholson Seth B. , Sternberg Elizabeth E.
Published: February 2008

The solar activity during July and August was the lowest since January 1928 when the record of character‐figures was started.

No very great, magnetic storms were recorded during the second and third quarters of 1930. During all the magnetic storms from April to September, except the one between April 19 and 24, solar activity was observed with which the storms may be identified.
American URSI broadcasts of cosmic data
Authors: Clark Katherine B.
Published: February 2008

THE JOURNAL is pleased beginning with this number to add by courtesy of Science Service as one of its regular features pertaining to geophysical and cosmical data, decoded tabular summaries of the daily American URSI broadcast.

Cooperating with the American Section of the International Scientific Radio Union, Science Service is collecting daily data on terrestrial magnetism, the solar constant, sunspots, and the auroral displays in order that they may be broadcast and otherwise distributed to those interested.
Sitka Magnetic Observatory April to September, 1930
Authors: Ulrich Franklin P.
Published: February 2008

The second quarter of 1930 was one of unusually heavy magnetic activity, there being only twenty‐three (0) days during the entire quarter.

April 6–14t 1930—This was a very prolonged magnetic disturbance and for the most part the magnetic activity is not particularly large. There were four very short and active periods: 8d, 8h to 10h and 11h to 13h; 10d, 9h to 13h; and 11d, 8h to 10h. The curves can be followed at all times.
Cheltenham Magnetic Observatory July to September
Authors: Hartnell Geo.
Published: February 2008

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