bluuebunny/crossref_metadata_2025 huggingface dataset:
Einige Bemerkungen zu dem Aufsatze von A. Nippoldt: Zur physikalischen Theorie des Erdmagnetismus
Authors: Schmidt Von Adolf
Published: February 2008

The author briefly states his reasons for not being able to accept the conclusions drawn by Dr. Nippoldt in his recent article, on “The Physical Theory of the Earth's Magnetism”. Judging from the appended paragraph, it would appear that Nippoldt himself has now modified some of his conclusions.
Five‐minute values of the magnetic elements at Antipolo, Rizal, Philippine Islands, during the total eclipse of the Sun, October 1st, 1921
Authors: Masó M. Saderra
Published: February 2008

The geographical position of the Observatory is: Latitude, 14° 35′ 48′′ N.; longitude, 121° 10′ E. The elevation above sea‐level is 215 meters.
Proposed magnetic and allied observations during the total solar eclipse of September 21, 1922
Authors: Bauer Louis A. , Fleming J. A.
Published: February 2008

Special magnetic and allied observations will be made at stations inside and outside the shadow belt of the total solar eclipse of September 21, 1922, by the Department of Terrestrial Magnetism of the Carnegie Institution of Washington, and by various cooperating magnetic observatories, institutions, and individuals. The distribution of the magnetic observatories within the limits of the eclipse and on both sides of the belt of totality is unusually good, as will be seen from the accompanying map taken from the American Ephemeris and Nautical Almanac for 1922 and on which the positions of these observatories have been indicated. These observatories are: North of the belt of totality, Alibag, Dehra Dun, Kodaikanal, and Toungoo, India; Batavia‐Buitenzorg, Java; and Antipolo, Philippines; before beginning of eclipse, Helwan, Egypt; after ending of eclipse, Apia, Samoa; to the south, Port Louis, Mauritius Island ; Watheroo, Western Australia; Toolangi, Victoria; and Christchurch, New Zealand. This distribution is all the more fortunate since the greater part of the belt of totality is over ocean areas.
Earthquake records, Watheroo magnetograms, November, 1921
Authors: Wait G. R.
Published: February 2008

There was a record of an earthquake on the magnetograms of the Watheroo Magnetic Observatory, Western Australia, on November 11, 1921. The declination and horizontal‐intensity traces showed a slight broadening, while there was a very slight blurring of the vertical‐intensity trace. The extreme Greenwich mean times of the record were from 18h 45m to 19h 0lm for declination, 18h 44m to 18h 56m for horizontal intensity, and 18h 52m to 18h 59m (uncertain) for vertical intensity. Mr. Curlewis, Government Astronomer at Perth, reported the following times of phases as obtained on the seismograph: 18h 43m 56s.6, P; 18h 46m 00s.5, uncertain; 18h 50m 10s.4, L.
Results from magnetic east‐west paths around the Earth
Authors: Peters W. J.
Published: February 2008

In the preliminary analysis of the Earth's magnetic field for 1922 by Dr. Louis A. Bauer,1 it was found desirable to ascertain how an east‐west path around the Earth would close that was everywhere throughout its length perpendicular to the direction of the compass needle, or to the horizontal component of the Earth's magnetic field. The considerations involved and the method adopted in constructing eleven such paths are given in these notes, together with the results.

The actual tracing of a path with the required accuracy, exactly magnetic east or exactly magnetic west, on land and over sea, presents many practical difficulties. Periodical time changes all along the path introduce uncertainties. Over land, local disturbances2 interfere and cities and other constructional culture obstruct the necessary surveying operations, while over the seas, where the only available method at present is to continue the path on a non‐magnetic ship, ocean currents and leeway affect the closure sought, not only by precisely the sum of their components perpendicular to the path, but also by shifting the path in regions of critical or steep gradients of the declination, and thereby introducing errors in its direction. The tracing of a path upon isogonic charts of the world is free from these sources of error though subject to others. Local disturbances have been effaced in the smooth isogonics, and time changes are taken care of in the reduction to a common epoch. Cultural detail, ocean currents and winds no longer enter the problem. Hence the plotted closure of a circuit extending exactly magnetic east or west around the Earth depends in this method only upon the systems of magnetization represented by the particular isogonics and upon the accuracy with which data can be scaled from the chart or plotted thereon. Unfortunately, the errors of plotting usually accumulate. It is possible to compute the closure of the path by a long process involving repeated approximations, provided that the magnetic declination is given as an analytical function of the latitude and longitude. The work entailed, however, renders this method practically useless.
Proposed magnetic and allied observations during the total solar eclipse of January 24, 1925
Authors: Ault J. P. , Fisk H. W.
Published: February 2008

Special magnetic and allied observations will be made at stations in or near the path of totality of the solar eclipse of January 24, 1925, by the Department of Terrestrial Magnetism of the Carnegie Institution of Washington, and by various co‐operating magnetic observatories, institutions, and individuals. One magnetic observatory, that at Agincourt, near Toronto, Canada, lies within the shadow belt. The Coast and Geodetic Survey magnetic observatory at Cheltenham, Maryland, is also very favorably situated, being within 200 miles of the southern edge of the path. The observatories of Great Britain lie near the path, although the Sun will set while still eclipsed at those stations.
Principal Magnetic Storms recorded at the Huancayo Magnetic Observatory August to September, 1924
Authors: Parkinson W. C.
Published: February 2008

(Latitude, 12° 02.′7 S.; Longitude, 75° 20′.4 W, or 5h 01m.W, of Greenwich.)
Principal Magnetic Storms recorded at the Cheltenham Magnetic Observatory, April to September, 1924
Authors: Hartnell Geo.
Published: February 2008

(Latitude, 38° 44′.0 N.; Longitude, 76° 50′.5, or 5h 07.m4 W. of Greenwich.)
Calm and disturbed days
Authors: de Moidrey J.
Published: February 2008

There seems to be a difference of opinion regarding the utility of investigating the disturbed as well as the calm days.

At Lu‐kia‐pang, in addition to the diurnal ranges which have been published in the Bulletin only since 1909, as has been done at Eskdalemuir since 1916, the last 18 years at Zi‐ka‐wei have been studied from this point of view for declination and for the horizontal, vertical, north, and west components. We venture to give some details regarding the case of the horizontal component, confining our study to the three seasons of four months.
Principal magnetic storms recorded at the Apia Observatory, January to June, 1925
Authors: Thomson Andrew , Westland C. J.
Published: February 2008

(Latitude 13° 48′.4S.; longitude 171° 46′ (11h 27m1)W. of Greenwich.)

During the first quarter no pronounced magnetic disturbance was recorded.
Principal magnetic storms recorded at the Cheltenham Magnetic Observatory, July to December, 1925
Authors: Hartnell Geo.
Published: February 2008

(Latitude, 38° 44.′0N.; Longitude, 76° 50.′5 or 5h 07m.4W. of Greenwich.)
Ein Beitrag zur Frage der scheinbaren Fortpflanzungsgeschwindigkeit erd‐magnetischer StÖrungen
Authors: Bock Von R.
Published: February 2008

C. Chree1 gibt die Anregung, bestimmte erdmagnetische Observatorien mit geeigneten Registrierapparaten auszurüsten, um Material zu schaffen für die Untersuchung der Frage, ob sich die erdmagnetischen Störungen mit einer kleineren Geschwindigkeit als die des Lichtes fortpflanzen and welche Richtungen sie in diesem Falle bevorzugen. Das erdmagnetische Observatorium Potsdam unterhält bereits seit Anfang 1925 eine derartige Registrierung, deren nähere Beschreibung schon anderen Ortes2 erfolgt ist. Die Ergebnisse einer nach der Richtung unternommenen Auswertung gibt Tabelle l wieder, die den Beginn der seit Anfang 1925 plötzlich eingetretenen Aenderungen der HorizontalintensitätTABELLE 1. h m1925, April 27 : 14 57.1, M. G. Z.August 22 : 14 47.6,1926, Januar 22 : 15 35.0,Januar 26 : 16 18.0,Februar 23 : 16 25.0,März 5 : 10 4.0,April 14 : 14 1.9,Mai 3 : 21 9.4,Juni 1 : 11 9.6,enthält. Bemerkt sei, dass nur die characteristischten Fälle ausgewählt sind, die auch auf der Schnellregistrierung nach einem ruhigen Verlauf einer scharfen Knick, sei es nach zunehmender oder abnehmender Intensität zeigen.
Principal magnetic storms recorded at the Cheltenham Magnetic Observatory, April to June, 1926
Authors: Hartnell George
Published: February 2008

(Lat. 38° 44′.0 N.; long., 76° 50′.5, or 5h 07.4mW. of Gr.)
The lunar‐diurnal magnetic variation and its relation to the solar‐diurnal variation
Authors: Egedal J.
Published: February 2008

The lunar‐diurnal magnetic variation is not large, but still the study of the phenomenon may be of interest, as it may throw light on some other geophysical problems.

At present it is not claimed that the observed lunar‐diurnal variation is due to a direct magnetic effect of the Moon, although such an effect may exist. Assuming the magnetic state of the Moon to be similar to that of the Earth, the variation produced in this way on our magnets would be very small, and of a type different from that observed. The action of the Moon must therefore be indirect, and it may be a screen‐effect or the effect of attractive forces acting on the Earth. Even if solar‐diurnal variations are produced by electric particles coming from the Sun, it is not probable that the Moon, acting on those particles, could produce a variation like that observed. It is therefore natural to expect that the lunar‐diurnal magnetic variation originates from the mechanical action of the Moon on the Earth and her atmosphere.
Preliminary results of ocean magnetic observations on the Carnegie from Washington to Plymouth, Hamburg, and Reykjavik, May to July, 1928
Authors: Ault J. P.
Published: February 2008

The seventh cruise of the Carnegie began when the vessel left her wharf at Washington, under tow, at 9h May 1, 1928. Shortly after midnight on May 2 she came to anchor at the mouth of the St. Mary's River to await sunrise for beginning the swings in the lower reaches of the Potomac River. The day broke fair, and six swings under her own engine were made to detect any deviations in declination or horizontal intensity. Simultaneous observations were made ashore by the Department's field‐parties, which had established numerous magnetic stations on both the Maryland and Virginia sides of the Potomac around the position previously selected for the swings.
Report on magnetic storm of July 7 and 8, 1928, as recorded at the Cheltenham Magnetic Observatory and on accompanying aurora observed at Brandywine, Maryland
Authors: Hartnell Geo.
Published: February 2008

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

A magnetic storm of the first magnitude, characterized by a sudden beginning, great intensity, and short duration, began at 23h 30m G.M.T., July 7, and continued until 11h 00m G.M.T., July 8. The ranges were: Declination, 4° 00′; horizontal intensity, 1270+ gammas; vertical intensity, 642+ gammas, perhaps two or three times as great. The maximum value of declination, 10° 00′.6, was at 5h 48m July 8, and the minimum, 6° 00′.4, at 6h 34m on the same day. The maximum value of horizontal intensity was 19119 gammas at 1h 10m July 8, with a minimum value of less than 17849 gammas, at which point the record went off sheet. In vertical intensity the maximum value recorded was 54932 gammas at 2h 02m July 8, with a minimum value of less than 54290, when the record went off sheet. The storm was accompanied by a fine display of aurora and serious interference with telegraph and telephone transmission.
Observatoire de Tsingtao, Juillet 1928
Authors: Tsiang P. J.
Published: February 2008

Remarque—C'est une perturbation extraordinaire telle que nos instruments n'ont pas enregistré de pareille depuis leur instalation. Elle est caracterisée surtout par un commencement très brusque et une amplitude extrêmement rapide. A 16h du 8 la perturbation s'est déjà adoucie, mais de petites oscillations ont continué jusqu'à 14h du 9.
Cheltenham Magnetic Observatory July to September, 1928
Authors: Hartnell Geo.
Published: February 2008

(Latitude 38° 44′.0 N.; longitude 76° 50′.5 or 5h 07.4m W. of Gr.)
Note on Kennelly‐Heaviside layer observations during a magnetic storm
Authors: Hafstad L. R. , Tuve M. A.
Published: February 2008

Observations of the Kennelly‐Heaviside layer by the echo‐method during the magnetic disturbance of October 17, 1928, showed an unusually great effective height and a change in echo‐pattern. Brief description is given of the method, and of the results obtained on undisturbed days, which are compared with those obtained during the disturbance. The marked changes observed make it clear that further records of this kind will be of great interest.
Summary of the year's work, Department of Terrestrial Magnetism, Carnegie Institution of Washington
Authors: Fleming J. A.
Published: February 2008

The preparations for and the initiation of the seventh cruise of the Carnegie have made large demands upon the energy, initiative, and interest of the entire personnel. The vessel left Washington on this three‐year cruise May 1, 1928, as planned. At the end of the year June 30, 1928, excellent progress had been made, which, despite the ambitious program undertaken in magnetic, electric, oceanographic, and meteorological observations, gives good promise of worth‐while results in all these fields. An inspiring feature of the preparations has been the generous cooperation extended by interested investigators and organizations everywhere.
Atmospheric‐electric researches made in 1928 during the Nobile Arctic Expedition in collaboration with Professor A. Pontremoli (Milan) and Professor F. Malmgren (Upsala)
Authors: Běhounek Francis
Published: February 2008

The researches into atmospheric electricity made during the Arctic Expedition of General Nobile comprised partly the measurements made in the airship Italia (Fig. 1) during the flights (see Figs. 2 and 3) Milan to Stolp (Pomerania), Stolp to Vadsö to Kings Bay (Spitsbergen), Kings Bay to Franz‐Josef Land to North Land (or Lenin Land) to Novaya Zemlya to Kings Bay, and Kings Bay to Greenland to North Pole to Charles XII Island (north of Spitsbergen), and partly the measurements made in Kings Bay on board the S.S. Città di Milano. The measurements included intensity of the penetrating radiation of the atmosphere, electric conductivity, ionic content, potential gradient, and radioactivity of the air. This paper deals merely with the measurements made during the flights of the Italia and their interpretation.
Sitka Magnetic Observatory, January to March, 1929
Authors: Ulrich F. P.
Published: February 2008

February 17–18, 1929—This storm began gradually, being active several hours before large fluctuations were recorded. From 10h to 19h on February 17 the curves show considerable motion but relatively slow so that the curves can be clearly followed at all times.

February 26–28, 1929—This storm had a very definite point of beginning. The storm was of magnetic character (1) for nearly a day before it shows the features of a (2) day. From 12h to 21h, February 27, and from 7h to 15h, February 28, considerable activity was recorded, particularly rapidly around 14h February 28 for about one hour. The light was increased at 17h February 27 so that the curves can be followed at all times.
In appreciation of the work of James Percy Ault of the Department of Terrestrial Magnetism
Authors: Wright Fred E.
Published: February 2008

Disaster on the sea rarely strikes singly. The explosion that destroyed the ship Carnegie on November 29, 1929, in Apia, took also the life of its commander, Captain James Percy Ault, under whose direction all scientific work was being done and to whose initiative and enthusiasm the success of the expedition was primarily due.

The cruise that ended so tragically was the seventh cruise of the Carnegie. During the past twenty years it covered more than than three hundred thousand miles; the results obtained on its cruises over the seven seas are the most important contributions that have been made to terrestrial magnetism and electricity. The ship was a floating laboratory and was thoroughly equipped for geophysical work at sea; its records are, in many respects, of pioneer character, establishing new methods of approach.
The effect of condensation‐nuclei in atmospheric‐electric observations
Authors: Builder Geoffrey
Published: February 2008

Curves are given, based on observations made at the Watheroo Magnetic Observatory, showing the relations found between the counts of condensation‐nuclei made with an Aitken counter and the simultaneous values of the atmospheric conductivity and potential‐gradient. There is some disagreement with the data given by Wait, based on fewer observations. It is concluded that, for the range of observation, there is an approximately linear relation between the nuclei‐count and the reciprocals of the polar conductivities and between the nuclei‐count and the atmospheric potential‐gradient. Owing particularly to the influence of the distribution of the pollution with respect to height the potential‐gradient curves are not very definite. The effect of the pollution on the conductivity is expressed in terms of the linear recombination‐law of Schweidler and the extension of this to explain the effect of high values of humidity is noted. An approximate and non‐linear extrapolation of the curve for reciprocals of negative conductivity against nuclei‐count is given based on Schweidler's equation of recombination in the presence of Langevin ions and uncharged nuclei.
A comparison of sunspot‐numbers, terrestrial‐magnetic activity, and long‐wave radio signal‐strength
Authors: Austin L. W.
Published: February 2008

The figure shows a comparison of the monthly averages of sunspot‐numbers, terrestrial‐magnetic activity (horizontal range) as measured at Cheltenham (Maryland), and the daytime radio field‐strength of signals received in Washington from the transmitting stations FYL at Bordeaux, France (f = 15.9 kc, λ = 18,900 m) and DFW at Nauen, Germany (f = 23.4kc, λ = 12,800m).

The resemblance of the sunspot‐curve to the other three is not close, but the similarity in the changes in magnetic activity to those in daylight signal‐strength seems to be. unmistakable. The resemblance of the Bordeaux signal‐curve to that of the magnetic activity seems closer even than the resemblance between the two signal‐curves. The deep drop of both the magnetic and signal‐values in November (more rarely in December) is especially striking. This early winter drop in signals has often been noticed, and in the case of transmission between Europe and America, has been sometimes ascribed to the proximity of the signal‐path to the area of Arctic darkness. It now appears that this and other seasonal variations both in magnetic activity and east‐west long‐wave signal‐strength may be due to common causes.
Watheroo Magnetic Observatory June to December, 1929
Authors: Johnston H. F.
Published: February 2008

(Longitude 30° 09′.1 S.; longitude 115° 52′.6 or 7h 44m E. of Gr.)

November, 1929—In addition to the mild storm on November 2, there was a small sudden commencement on the earth‐current and magnetic records at 18h 21m November 26.
Communication de l'observatoire magnétique à Godhavn
Authors: Par Olsen Joh.
Published: February 2008

Dans un rapport1 relatif aux travaux magnétiques de Danemark M. la Cour a mentionné 5 points d'importance pour les travaux de l'observatoire à Godhavn. Sans suivre le numérotage de M. la Cour les cinq points sont les suivants: (a) Enregistrement toutes les minutes (T.M.G.) de la force magnétique avec un écart de l'heure exacte plus petit que deux secondes; (b) observations tout à fait simultanées des valeurs des éléments magnétiques; (c) diminution de la confusion des traces des trois éléments sur le papier photographique; (d) détermination exacte des valeurs de base des variomètres en dépit des grandes et fréquentes variations du champ magnétique terrestre dans les régions polaires, (e) détermination exacte de la valeur d'échelle des variomètres.

On donne ci‐dessous quelques renseignements sur la manière dont on a envisagé ces questions.
A comparison of magnetic disturbance at different stations
Authors: Wallis W. F.
Published: February 2008

A brief discussion of the magnetic records obtained during the MacMillan Baffin Island Expedition of 1921–22 is given with comparison of results from several other well‐distributed observatories. For comparison a short, well‐defined, world‐wide magnetic storm (March 14, 1922) was selected, and departures from normal values were compiled and compared by three methods: (1) Difference between the disturbed and normal total‐intensity vectors; (2) excess energy of the magnetic field due to the disturbance; (3) magnetic activity proposed by Chree, using absolute daily ranges in three rectangular components of the total magnetic intensity. It is concluded that the geographic distribution of magnetic activity during disturbance bears a close relation to the auroral zone, and there is evidence that the zone of maximum auroral frequency is also a zone of maximum magnetic activity. If we take average values of the disturbance‐vectors over several months, there is a marked regularity in their directions for the individual stations, and for all stations the general direction of the horizontal‐intensity disturbance‐vectors is southward. This indicates that the disturbing currents in the upper atmosphere flow in general from east to west around the Earth.
The magnetic section of the Sverdlovsk Observatory in “Wyssokaja Dubrowa”
Authors: Sitnoff
Published: February 2008

In the year 1929, the Magnetic‐Meteorological Observatory in Sverdlovsk was forced to share the fate of many other observatories. On account of the installation of electric‐tram service in the city of Sverdlovsk, the Observatory was obliged to transfer its magnetic section to a new site, namely, to a point 33 km to the east of the city known as “Wyssokaja Dubrowa” about 2 km distant from the Kossulino station on the Omsk Railway Line.

Shortly before the inauguration of the tram‐service in November 1929, an overground wooden hut was erected for housing the magnetograph and accessories, in which the darkroom is surrounded by a corridor for the purpose of thermal insulation. In addition, a dwelling‐house for the observer and other structures were built. In December, the Edelmann magnetograph which had been in use at the Sverdlovsk Observatory since 1904, was transferred to “Wyssokaja Dubrowa.“
Atmospheric‐electric survey in the vicinity of Washington, D.C.
Authors: Johnston H. F. , Wait G. R.
Published: February 2008

Atmospheric‐electric observations obtained through a survey in the District of Columbia and vicinity, indicate the existence of high‐, medium‐, and low‐conductivity areas. Approximately normal high total conductivity‐values, on the average 2.3×10−4 E.S.U., were found in regions outside the District of Columbia. This value is about three times that for the low‐conductivity region which is roughly included by the District boundary‐lines, except for an extension towards the city of Baltimore. The total air‐earth current tends towards equality over all three regions; this was interpreted to mean that the factor causing subnormal conductivity is operative to only small altitudes. The results suggest that atmosphereic pollution may be a large factor in producing small conductivities in the low area and that the subnormal values at the Washington Observatory of the Department of Terrestrial Magnetism, 16 meters above the surface of the ground, are in addition affected by a lower rate of ionization than are those nearer the Earth's surface.

When the total air‐earth current is computed from the potential gradient and the total conductivity, true values will be obtained only at stations where there are undisturbed equipotential surfaces. Where disturbances exist in the equipotential surfaces, a reduction‐factor for conductivity as well as for potential gradient will be required in order to compute true values of air‐earth current for the reduction‐factor station. The reduction‐factor for the conductivity as recorded at the Washington Observatory, based on the series of intercomparisons with all survey‐stations reported upon, is about 4; this large value is due probably to the unusual height of the apparatus above the surface of the ground. For measurements of potential gradient and of the conductivity made at similar heights above the ground and sufficiently near each other, probably no great error results by assuming a value of unity for the reduction‐factor, that is, when the air‐earth current is computed from the potential gradient and conductivity.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, January to March, 1931
Authors: Nicholson Seth B. , Sternberg Elizabeth E.
Published: February 2008

Three moderate magnetic storms were recorded in the months of January and February. During the first storm, January 16 to 18, an active group in north latitude 8° was near the west limb. This group had been especially active on January 15. At the beginning of the second storm, February 13 to 16, no solar observations were possible at Mount Wilson.
Ordre du jour préliminaire de la réunion de la Commission Internationale de Magnétisme et d'Électricité Atmosphérique à Innsbruck du 21 au 23 Septembre 1931
Authors: la Cour D.
Published: February 2008

Sur la demande du Président j'ai l'honneur de convoquer les membres de la Commission à une réunion qui aura lieu à Innsbruck du 21 au 23 septembre 1931. Le Bureau de la Commission mettra les points suivants à l'ordre du jour:

(I) Rapport du Président

)II) Election de nouveaux membres
Watheroo Magnetic Observatory September 1930 to March 1931
Authors: Parkinson W. C.
Published: February 2008

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

November 13–15, 1930—This moderate storm began with a sharp sudden commencement, there being an increase of thirty γ in horizontal intensity. There were irregular but small fluctuations until the end of the storm.
Geophysical stereograms
Authors: Bartels J.
Published: February 2008

The use of stereograms for the representation of geophysical data is discussed. Formulae and practical rules for constructing stereograms and anaglyphs (stereoscopic drawings in two colors) are given. Ten sample stereograms, based on unpublished material, are reproduced and discussed. With the exception of No. 1, which illustrates the principle of construction, and No. 10, which shows upper‐air currents at Apia, Samoa, the stereograms bear on magnetic phenomena, namely: Nos. 2 to 5—Diurnal and annual magnetic variation at Watheroo (Australia); No. 6—Changes during part of a magnetic storm; No. 7—Differences of the mean magnetic vector on disturbed and quiet days at Potsdam, 1915 to 1928; No. 8—World‐chart of secular variation for 1925; No. 9—Globe showing magnetic axes of the Earth, and distribution of magnetic observatories. While some of the stereograms present only new illustrations of well‐known facts, the discussions which accompany Nos. 4 to 8 suggest some novel points.
Preliminary report of the magnetic observations made during the aeroarctic expedition Graf Zeppelin, 1931
Authors: Ljungdahl Gustaf S.
Published: February 2008

The magnetic work during the arctic expedition of the airship Graf Zeppelin in July 1931 was undertaken for the purpose of studying the possibilities of making magnetic measurements under the conditions involved and of obtaining as valuable observations as possible.

A preliminary report of the results is here presented. In the reduction of the observations, I hope later to have the privilege of utilizing the registrations of Sloutzk and Matotchkin Shar. It is to be noted that the present values have not been reduced. The geographical positions have been fixed by interpolation from the time‐records. The positions as given in Tables 1 and 2 are preliminary. They will be recalculated and in a later, more complete, report probably somewhat corrected.
Apia observatory
Authors: Glover P. W.
Published: February 2008

A magnetic storm of not violent character was recorded at the Apia Observatory (latitude 13° 48′.4 south, longitude 171° 46′5 west) on October 29–30, 1931, The commencement was not of the “sudden” type, but developed gradually, the time being 7h 30m G. M. T. on the 29th. The ranges between the extreme maxima and minima were: Declination, 7′.0; horizontal intensity, 79γ. The range in vertical force is not known owing to the vertical‐force variometer being out of action.

The H‐trace fell jerkily by 52γ to a minimum at 11h 30m, after which there was a rise to the greatest recorded maximum by 58γ, which was reached at 12h 48m. This was followed by a fall of 78γ to a minimum at 15h 34m, which was followed by a series of small maxima and minima in which at 6h 12m on the 30th was the extreme minimum, 79γ below the greatest maximum. At 10h 02m on the 30th occurred the second largest maximum, 77γ above the extreme minimum, after which the disturbance gradually died away.
Sitka Magnetic Observatory January to March 1932
Authors: Ulrich Franklin P.
Published: February 2008

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

There were no large magnetic storms during this quarter.
The magnetic survey of New Zealand
Authors: Farr C. Coleridge , Skey Henry F.
Published: February 2008

L. A. Bauer's connection with such magnetic work as has been done in New Zealand was continuous from 1895 until ill health prevented him from taking so active an interest in these things.

We remember well, in the days before observational work on the magnetic survey of New Zealand was begun, his support in the proposals that were being put forward, and how intensely valuable that support was when matters had advanced enough (about 1897) to bring the proposal before the notice of the New Zealand Government.
Secular change of the Earth's magnetism
Authors: Hazard Daniel L.
Published: February 2008

It is appropriate at this time to review briefly the development of our knowledge of the secular change of the Earth's magnetism, particularly in the United States, in view of Bauer's lifelong interest in the subject and his noteworthy contributions to it.

Henry Gellibrand, professor of mathematics at Gresham College, England, is credited with the discovery of the fact that the magnetism of the Earth changes with time. On June 12, 1634, he made a careful determination of the magnetic declination at Diepford, about three miles southwest of London Bridge, and got a value of 4° 06′ east, where Borough and Norman had found 11° 15′ east in 1580. He announced his discovery in “A Discourse Mathematicall on the Variation of the Magneticall Needle, together with its Admirable Diminution Lately Discovered,” published in 1635.
The significance and accuracy of measurements of Earth‐current potentials
Authors: Rooney W. J.
Published: February 2008

The superficial simplicity of measurements of earth‐current potentials makes them liable to error due to inadequate appreciation of the requirements for securing satisfactory records and has led to faulty interpretation of the results obtained. Records from the multiple systems at Watheroo and Huancayo demonstrate the lack of significance of the absolute values of potential recorded and of the long‐period changes in them, most of which are due to meteorological conditions. The value of independent records as a check on the satisfactory operation of the recording equipment and as an indication of anomalous results due to local structural inhomogeneity is shown by examples taken from the records from these two observatories. Duplicate potential records and earth‐resistivity data both are essential for adequate study of the phenomenon.
The temperature of the auroral region determined by the rotational series of the negative nitrogen‐bands
Authors: Vegard L.
Published: February 2008

1—Preparations and preliminary work

When in 1921 the spectrographic work on the auroral spectrum was taken up in a systematic way, one of the problems to be dealt with was to determine the temperature of the auroral region by means of the rotational nitrogen‐bands.
Watheroo Magnetic Observatory January to June 1932
Authors: Parkinson W. C.
Published: February 2008

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

May 29–30, 1932— The storm of May 29–30, 1932, was the only magnetic storm of any magnitude recorded at the Watheroo Magnetic Observatory during January to June 1932. The beginning of the storm was recorded at 11h 16m in D and in Z and at 11h 15m in H, its ending being May 30 at 8h 12m as recorded in D and Z and at 8h 17m as recorded in H. The ranges were: D, 24′.0; H, 173γ; Z, 151γ.
Notes on the July 1932 meeting of the Committee on Symbols, Units, and Nomenclature of the International Union of Pure and Applied Physics, to discuss magnetic units
Authors: Kennelly Arthur E.
Published: February 2008

Purpose and Scope—The purpose of this communication is to lay before readers of TERRESTRIAL MAGNETISM AND ATMOSPHERIC ELECTRICITY an unofficial historical outline of the international actions on C. G. S. magnetic units during the last five years, up to and including those of the Committee on Symbols, Units, and Nomenclature (S. U. N. Committee) at its recent meeting in Paris, July 9, 1932,—together with certain deductions that seem to follow there from. For more precise and authentic information, reference may be made to the official minutes of these various meetings, which are too lengthy to be included here.

Brief historical outline of C. G. S. magnetic units up to 1925—Gauss showed in 1833 how to reduce terrestrial magnetic observations with suspended magnets to absolute measure, that is, to units of length, mass, and time, Weber, cooperating with him, extended the scope of these researches in 1840 and 1851. They employed the millimeter‐milligram‐second (M. M. S.) system. Magnetic observatories began to keep records in these units about 1845. The rapid growth of electric telegraphy in 1860, created a demand among telegraph engineers for electrical units. At a meeting of the British Association for the Advancement of Science (B. A.) in 1861, a paper was presented by the telegraph engineers Clark and Bright, pointing out the need for scientific measurements and units in that field. The first B. A. committee was then appointed to report upon “Standards of electrical resistance” It issued several annual reports and continued until 1867. It recommended the adoption of units in the meter‐gram‐second (M. G. S.) absolute system. It issued standard B. A. resistance‐coils, and standard condensers in that system, as ohms and microfarads, respectively. It proposed the volt, approximately at its present unit magnitude; but did not reach the stage of issuing standards of electromotive force.
Huancayo Magnetic Observatory July to September 1932
Authors: Ledig Paul G.
Published: February 2008

(Latitude 12° 02′.7 S.; longitude, 75° 20′.4 or 5h 01m W. of Gr.)
The rôle of the space‐charge in atmospheric electricity
Authors: Brown Joseph G.
Published: February 2008

The idea of an electrified atmosphere was generally accepted in Franklin's time, but the experiments of Ermann and Peltier led to the idea of a negatively charged Earth. Lord Kelvin,1 however, saw that both ideas were correct and pointed out that the electric field of the Earth is similar to that of a condenser. This analogy is not very close since only the negative plate is a conducting surface, while the positive plate is the first 8 or 10 kilometers of the atmosphere. The dielectric, moreover, which corresponds with the positive plate, is an ionized gas and for the potentials involved the “leaks” are very significant.
Watheroo Magnetic Observatory April to June, 1933
Authors: Parkinson W. C.
Published: February 2008

April 30‐May 2 1933—This magnetic storm of moderate intensity began at 16h 27m 50s on April 30 with a sudden commencement which was very definitely recorded in all three elements. During the half‐hour preceding the commencement there appeared on all the traces rapid fluctuations of small amplitude; the la Cour rapid trace showed the period of these oscillations to be about 90 seconds and their average amplitude (semi‐range) about 2γ. In the sudden commencement a decrease in H of about 2γ was followed immediately by an increase of 33γ within 5 minutes. In Z the initial impulse represented a slight increase of the force followed by a decrease of 12γ in six minutes. The declination increased westerly at the time of commencement and immediately showed an easterly swing of about one minute of arc in three minutes of time. Irregular movements of only moderate intensity follow in all three elements and continued until 0h 30m on May 1; then followed a quiet period of 12 hours after which what was presumably the same disturbance again became manifest by large irregular movements in all elements, continuing until 2h on May 2 when the traces resumed their normal appearance. It is during this last period of the disturbance that the maximum ranges occurred. The ranges were: Declination 24″; horizontal intensity, 125γ; vertical intensity, 144γ. Time of commencement was taken from the la Cour horizontal‐intensity trace; the Mitchell inductometer showed time of commencement also as 16h 27m 50s. All times are Greenwich mean time.
The magnetic character of the year 1932 and the numerical magnetic character of days, 1930–1932
Authors: van Dijk G.
Published: February 2008

The annual review of the “Caractère magnétique de chaque jour” for 1932 has been drawn up in the same manner as for the preceding years.1 Forty‐eight observatories contributed to the quarterly tables, forty‐four of them sent complete data.

Table II of the annual review, containing the mean character of each day and each month, the lists of calm days and disturbed days, and the days recommended for reproduction are reprinted here.
Sitka Magnetic Observatory October to December, 1933
Authors: Hershberger John
Published: February 2008

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

October 7—This storm began with a sudden increase in declination of 40 minutes, followed immediately by a decrease of 58 minutes. This was accompanied by minor changes in the horizontal and vertical intensities, which, however, remained relatively undisturbed until about 9h 30m. Then the two intensity‐components decreased rapidly, all the elements reaching their minimum values at about 11h 10m. Then they gradually returned to their normal values.
A study of atmospheric dust using a continuous recording jet‐counter
Authors: Nielsen Russell A.
Published: February 2008

A new device for continuously recording the dust‐content of the air has been used to obtain records of atmospheric dust at Stanford University, California. Continuous dust‐records from January 13 to March 17, 1934, have been taken and the variations in the dust‐content of the air correlated with other atmospheric phenomena recorded at this station. In particular, the space‐charge tended to vary inversely as the dust‐content, while the potential gradient seemed to be unaffected by changes in the amount of dust.
Cheltenham Magnetic Observatory, July to September 1934
Authors: Hand Eoline R.
Published: February 2008

There were no storms of importance recorded during the third quarter of 1934.
American URSI broadcasts OF cosmic data January to March, 1935
Authors: Ennis C. C.
Published: February 2008

The data for terrestrial magnetism, sunspots, solar constant, and auroræ 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 Electricity, (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 k for Mount Wilson is about 0.7.
A report of work on the aurora borealis for the years 1932–1934
Authors: Fuller Veryl R.
Published: February 2008

It is the purpose of this paper to give a summary of the visual observation of the aurora at the Alaska Agricultural College and School of Mines (to be designated University of Alaska from July 1, 1935) during the years beginning August 1932 and ending December 31, 1934. The data used represent practically a continuous watch during the hours of darkness for these years and it is felt that it is rather complete in detail. For the methods of observation and the type of data taken reference is made to an earlier publication.1

Since the auroral season begins in August and continues until the following May the data have been grouped by seasons rather than by years. For the two and one‐half seasons covered, an idea of the number of displays relative to the total number of days in each group may be gained from Table 1.
The annual and diurnal variation of ions in an urban community
Authors: Gagge A. P. , Moriyama I. M.
Published: February 2008

Results of annual and diurnal ion‐counts made at a station located in New Haven, Connecticut, are reported. The counter used was of the Zeleny type. For both positive and negative ions four mobility‐thresholds were used, namely: 0.07, 0.017, 0.0014, and 0.0006 cm per second/volt per cm. The total ion‐count was analyzed into three groups; the small‐ion group with mobilities greater than 0.07, the intermediateion group with mobilities between 0.07 and 0.0014, and the large‐ion group with mobilities between 0.0014 and 0.0006. There is a rise in positive light ions during the summer months while the negative ions, usually less in number than the positive, show a fall during the summer months. The heavy‐ion group increases two‐fold in number during the winter months over the summer months, while the intermediate group increases only slightly in number during the same period. The diurnal variation of the heavy‐ion group shows two daily maxima at 8 a. m. and 6 p. m., eastern standard time (E. S. T.), during the heating season (October through April) while the 6 p. m. maximum nearly vanishes for the non‐heating season (May through September); on the other hand the intermediate group shows an inverse relationship with the heavy‐ion group for both seasons. From a characteristic curve based on assumptions justified partially by experiment the intermediate group is shown to be composed of ions with a mobility whose value varies seasonally between 0.01 and 0.0025 cm per second/volt per cm. The highest mobility‐value appears in the summer months.
Sitka Magnetic Observatory April to June, 1935
Authors: Hershberger John
Published: February 2008

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

April 10—This storm began at about 10h 20m, G. M. T., with moderate, long‐period fluctuations in all the elements, which continued for about ten hours, followed by about five hours of relative calmness. Then came a period of more rapid fluctuations, increasing irregularly until they reached their maximum intensity about 11h, April 11. By 13h these had ceased, and they were followed by several large oscillations with a period of about two hours. The storm proper ended at 17h, but the record continued moderately disturbed for two days longer. Ranges: Declination, 107′, horizontal intensity, 670 gammas, vertical intensity, 741 gammas.
Cheltenham Magnetic Observatory April to June, 1935
Authors: McComb H. E.
Published: February 2008

(Latitude 38° 44′.0 N., longitude 75° 50′.5 or 5h 07m.4 W. of Gr.)

April 9—Beginning at 2h 09m, G. M. T., H decreased about 75 gammas within one hour, after which there was a decrease of about 30 gammas in Z. D slowly decreased as H decreased.
Watheroo Magnetic Observatory October to December, 1935
Authors: Parkinson W. C.
Published: February 2008

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

October 20–22—A disturbance of moderate intensity but long duration began with a series of short‐period oscillatory movements shown in all three elements at 11h 25m 30s, G. M. T., October 20. The period of these fluctuations was about 50 seconds and the amplitude (whole range) in horizontal intensity 5 gammas, in vertical intensity 7 gammas, and in declination 1′.8. Leisurely movements showing a series of peaks, the times of maximum in horizontal intensity being at 11h 51m, 14h 48m, 16h 37m, and 19h 29m, follow, and from then onwards the traces very gradually subsided in activity without any noteworthy features, normal conditions being regained by midnight on October 22. The ranges recorded were: Declination, 15′.2; horizontal intensity, 81 gammas; vertical intensity, 102 gammas.
The space‐gradients of the Earth's magnetic field
Authors: Chapman S.
Published: February 2008

§1. The space‐gradients of the Earth's magnetic field, like those of the gravitational field, are of both scientific and practical interest. The Eötvös gravity‐balance is available for measuring the gravitational gradients, and the possible importance of the magnetic gradient in geophysical prospecting has led to the proposal by H. Haalck1 of a device for measuring them, while I. Roman and T. C. Sermon2 have actually developed a (different) device for the same purpose. This consists of two similar coils rotated on parallel shafts in such a manner that the planes of the coils always remain parallel. Theratio of the electromotive forces induced in the two coils is measured, by means of a specially devised Kirchhoff net, and affords a measure of theproportionate magnetic gradient, that is, the gradient of any component, divided by that component.
Final relative sunspot‐numbers for 1935 and monthly means of prominence‐areas for 1909–1935
Authors: Brunner W.
Published: February 2008

Table 1 contains the final sunspot‐numbers for 1935, 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 2 gives the yearly means of the relative numbers,R, since the last minimum 1933 and the number of days without spots.
AmericanURSI broadcasts of cosmic data January to March, 1936
Authors: Ennis C. C.
Published: February 2008

The data for terrestrial magnetism, sunspots, solar constant, and auroræ 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 Electricity, (2) the type featuring the day other than normal by the lettersb,p,o, andi 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 formulaN =k (10g +s), wherek for Mount Wilson is about 0.7.