bluuebunny/crossref_metadata_2025_split huggingface dataset:
Mesures magnétiques et carte magnétique des isogones de la Moldavie et Bessarabie (Roumanie)
Authors: Procopiu Par St. 
Published: February 2008

1. Variations séculaires en Roumanie—Les mesures précises de la déclinaison, inclinaison, et composante horizontale du magnétisme terrestre, effectuées par Kreil, en 1858, aussi bien pour les territoires qui appartenaient à l'empire au triche‐hongrois, que pour cinq localités de l'ancienne Roumanie, ont permis à Hepites et Murât, après une campagne magnétique dans l'ancienne Roumanie, où ils ont étudié 72 localités entre 1898 et 1900, de déduire les variations séculaires annuelles.Ces variations annuelles, pour l'époque 1858–1900, sontΔD=−5′.1 ΔI=−1′.5 ΔH= +0.00017 Pour les années suivantes, l'Observatoire magnétique de Bucarest qui a fonctionné pendant l'intervalle mai 1898 à mai 1901, toujours sous la direction de Hepites et Murât, d'après des mesures magnétiques absolues, a donné pour Bucarest les variations séculaires annuelles suivantes:1900 ΔD=−3′.4 ΔI=−0′.8 ΔH=+0.000101901 ΔD=−6′.7 ΔI=−1′.6 ΔH= +0.00011Ilen résulte que, jusqu'en 1901, la déclinaison et l'inclinaison y diminuaient et la composante horizontale augmentait annuellement.
Japanese ursigram, September to December, 1932
Authors: Nagaoka H. 
Published: February 2008

The following tables summarize the cosmic data as broadcast weekly (see this JOURNAL, 37, 487–488, 1932) from the Tokyo Radio Station, JAN. The following designations are used to indicate magnetic conditions as determined from records made at the Kakioka Observatory: 0 = calm; 0.5 = rather calm; 1 = slight disturbance; 1.5 = disturbance; 2 = great disturbance. The groups and numbers of sunspots are as observed at the Tokyo Astronomical Observatory.The table of Kennelly‐Heaviside Layer heights is self‐explanatory.
Correlation between sunspot‐activity and daily ranges of terrestrial magnetic elements at Apia, Western Samoa, 1905 to 1929
Authors: Glover P. W. 
Published: February 2008

This paper is an account of the attempt to correlate the annual mean daily ranges of the terrestrial‐magnetic elements horizontal force, vertical force, and declination as measured at the Apia Observatory during the 25‐year period 1905 to 1929 with the annual means of the Wolfer sunspot‐numbers.By the annual mean daily range of an element is meant the annual mean of the differences between the greatest and least of the monthly means of the hourly mean values. The reason for using the hourly mean values is that the data concerning the absolute ranges are not available over the entire period. The magnetic data are taken from the published reports of the Observatory, while the final relative sunspot‐numbers are those published by Wolfer and later by Brunner in Terrestrial Magnetism.
Possible stellar origin of high‐speed ions
Authors: Gunn Ross 
Published: February 2008

It is noted that the observed state of rest of numerous ionized calcium clouds guarantees that all interstellar space is substantially neutral. The author has shown that the solar atmosphere is permeated by strong electric fields and this suggests that negative ions might be accelerated and move off into space with energies of some millions of volts. Study of the process of emission indicates that only within a sunspot are conditions such that a negative ion can traverse the solar atmosphere and acquire energy comparable to the potential difference between the Sun proper and its high atmosphere. An electron or negative ion which succeeds in traversing the layer emerges at high speed and attracts to itself, from the high atmosphere, a neutralizing positive ion by a mechanism equivalent to electrostatic attraction; and, finally, the two ions, forming a neutral pair, leave the Sun at precisely the same velocity. The energy of the neutral stream is estimated to be a very small but appreciable fraction of the energy radiated by the sunspot. The effects of these ions plunging into the Earth's atmosphere are considered and it is possible that they produce the aurora.Neutral ion‐pairs of solar origin can have no relation to the penetrating‐radiation because of their low energy, but similar processes in early‐type stars will give rise to neutral ion‐pairs of approximately 1010 electron‐volt energies. It is suggested that these energetic neutral ion‐pairs which perhaps get separated on entering the Earth's magnetic field or by collisions in the Earth's atmosphere are identical with the penetrating‐radiation. Reasons are given for believing that the distribution of such particles in space is nearly uniform.
Summary of the year's work, Department of Terrestrial Magnetism, Carnegie Institution of Washington
Authors: Fleming J. A. 
Published: February 2008

Effort has been chiefly concentrated during July 1, 1932, to June 30, 1933, as in the previous year, on the study of the extensive observational material in hand, particularly that obtained on the last cruise of the Carnegie and at the Department's two observatories, rather than to the amassing of new data. However, the Department has taken an active part in the inauguration and maintenance of the two American Polar Year stations at Point Barrow and College‐Fairbanks, Alaska, and has collected data for secular‐variation studies at a number of repeat‐stations in South America.General statistical methods for research on diurnal variations, together with schemes for numerical and graphical work suitable for handling the largest possible amount of material, have been developed in a series of papers. The procedure has been applied to magnetic diurnal‐variation at Watheroo and Huancayo observatories and has already yielded convincing results. Thus, the diurnal variation of declination at such an equatorial station as Huancayo is found to vary considerably even on very quiet days. At Watheroo, on quiet days in southern summer, the horizontal intensity has, on the average, a small diurnal variation, because Watheroo is situated in the transitional zone between the equatorial and the polar types of the variation ; individual days, however, exhibit either the equatorial or the polar type quite markedly, indicating that the focus of the diurnal atmospheric current‐system passes on some days several degrees of latitude south, on other days north, of Watheroo. Furthermore, the passage of the focus is retarded or accelerated on some days by a few hours, and the intensity of the current varies by a large fraction of its average value; these features are indicated in simultaneous changes of the diurnal variations of declination and of vertical intensity.
Present status of the investigation on dynamic and tilting deviations in the Department of Terrestrial Magnetism, Carnegie Institution of Washington
Authors: Peters William J. 
Published: February 2008

This investigation began in 1928 with the study of tilting deviations produced by the inclinations of the planes of the compass‐card when subjected to simple harmonic motion over or under a horizontal axis, as in the ideal rolling of a ship in a non‐resisting medium or the bed of a swing under its horizontal axis, Such a swing was used in the first experiments, but the results showed the necessity of automatic action and of continuous records throughout the phases of the swing‐motion, which are not possible in visual observations.A swing was then designed and constructed in the instrument‐shop of the Department. It is made entirely of brass and actuated by an electric motor installed so far away that the motor has no magnetic effect on the compasses to be used in the experiments. The record is obtained by a motion‐picture camera located on the swing‐frame.
Johannes Paulus van der Stok
Authors: van Everdingen E. 
Published: February 2008

Johannes Paulus van der Stok was born January 14, 1851, at Zuilen, studied from 1867 at the University of Utrecht, and took his degree of doctor in mathematics and physics in 1874. Buys Ballot was one of his teachers.After having been about two years teacher at the gymnasium of The Hague, Dr. Van der Stok was appointed sub‐director of the Royal Magnetical and Meteorological Observatory at Batavia. In 1882 he succeeded Dr. Bergsma as director of the Observatory and resigned as such in 1899, when he returned to Holland.
American URSI broadcasts of cosmic data
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 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.
On the propagation of magnetic storms
Authors: Egedal J. 
Published: February 2008

In a report presented to the Association of Terrestrial Magnetism and Electricity of the International Union of Geodesy and Geophysics Professor A. Tanakadate has compiled the times of three sudden commencements of magnetic storms for more than twenty magnetic observatories distributed over the Earth. This material is of great interest for the study of the propagation of magnetic storms, especially on account of its homogeneity, arising from the fact that most of the instruments from the records of which the data have been derived, are of the same type (la Cour's quick‐running magnetographs and “Variomètres de Copenhague”).The data given in Professor Tanakadate's report refer for all observatories to the “first maximal deviation,” and only for a small number of observatories to the “very beginning” of the sudden commencement. For this examination only times for the “first maximal deviation” have been used.
Vilhelm Carlheim‐Gyllensköld 1859–1934
Authors: Ljungdahl Gustaf S. 
Published: February 2008

Dr. Vilhelm Carlheim Gyllensköld died in Stockholm December 13, 1934. Up to the last few weeks before his death, he was actively engaged on the work which had claimed his chief interest during life—the Earth's magnetism and allied phenomena.He was born in Stockholm October 17, 1859. In 1877 he became a student at the University of Uppsala, where he received his doctor's degree in 1897. He interrupted his studies to participate in the First International Polar Year 1882–83 as a member of the Swedish expedition to Cape Thordsen, Spitzbergen. Carlheim‐Gyllensköld's part in this Expedition, which was under the leadership of Ekholm, was to carry out the auroral observations, while Solander made those of terrestrial magnetism. Considering the technical difficulties with which an auroral observer of that time had to deal, it must be recognized that the results of this, his first geophysical work, were most remarkable, especially because of the care and devotion which thoroughly distinguish it. In particular, his investigations of the spectrum of the aurora seem to be among the most accurate ever made. During this Expedition his lifelong interest in the science of the Earth's magnetism appears to have been aroused.
American URSI broadcasts of cosmic data October to December, 1934
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.
Sur la variation diurne des eléments magnétiques au Scoresby Sund (Est‐Groenland)
Authors: Rothé J. P. 
Published: February 2008

En examinant rapidement les courbes enregistrées par les magnétographes La Cour à la station française de l'Année Polaire au Scoresby Sund (longitude, 21° 57′.7 W; latitude, 70° 29′.1 N), on est frappé par la régularité des variations diurnes des éléments magnétiques. Les résultats détaillés de nos observations sont publiés, sous la direction du Professeur Maurain dans les Annales de l'Institut de Physique du Globe de Paris1 et l'auteur résumera ici quelques observations inspirées par ce dépouillement.Variation diurne de la déclinaisonLe régime diurne de la déclinaison est particulièrement net, avec un maximum vers l'est, vers 6 à 7 heures du matin (T. M. G.) et un maximum plus étalé vers l'ouest le soir vers 20 à 22 heures. Le graphique (Fig. l) représente l'allure des différentes courbes mensuelles, toutes très concordantes; il montre aussi que l'amplitude diurne moyenne suit une marche annuelle très accentuée passant de 16 minutes en janvier à 38 minutes en avril. La seule série d'observations comparables directement à nos mesures est constituée par des lectures horaires de déclinaison faites en 1891–1892 à l'île de Danemark, dans le Scoresby Sund, au cours de l'hivernage de l'expédition danoise Ryder.2 La variation diurne de la déclinaison y présentait une marche tout à fait analogue à celle que nous avons constatée; toutefois l'amplitude diurne moyenne était plus forte au printemps, atteignant 61 minutes en mars, parce que 1891–1892, à l'encontre de 1932–1933, correspondait à une période de maximum d'activité solaire.
Apia Observatory January to March, 1935
Authors: Wadsworth J. 
Published: February 2008

(Latitude 13° 48′.4 S., longitude, 171° 46′.5 or 11h 27m.1 W. of Gr.)January 27—A slight disturbance began at 14h 50m, G. M. T., with a sudden increase of 22 gammas in the horizontal intensity. A minimum value was shown at 5h 40m on January 28, the range of the disturbance being approximately 94 gammas. The vertical intensity increased initially by 4 gammas and then underwent slight irregular changes.
Earth‐current observations at Chesterfield, Canada
Authors: Currie B. W. 
Published: February 2008

This is a summary of the report on the earth‐current observations made near Chesterfield Inlet (63° 20′ north, 90° 42′ west) during the International Polar Year to be published shortly by the Meteorological Service of Canada. The value of the earth‐current data in relation to the magnetic and auroral observations at Chesterfield is indicated.Earth‐current observations had not been made in any part of northern Canada prior to 1932–33, and information was lacking concerning the nature and the magnitude of the earth‐current that might be expected inside the zone of maximum auroral frequency and close to the magnetic pole. The Department of Terrestrial Magnetism of the Carnegie Institution of Washington, had designed a recording circuit for use at the International Polar‐Year Station at College‐Fairbanks, Alaska, which provided a large range of sensitivities. That Department kindly loaned an earth‐current outfit embodying this circuit to the Meteorological Service of Canada for use at Chesterfield. A description of this circuit and a statement of its advantages can be found elsewhere1,2.
American URSI broadcasts of cosmic data April to June, 1935
Authors: Ennis C. C. 
Published: February 2008

The data for terrestrial magnetism, sunspots, solar constant, and aurorae 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.
Comment [on “Measures of terrestrial‐magnetic activity” by G. van Dijk]
Authors: Bartels J. 
Published: February 2008

G. van Dijk presents evidence that the discrepancy between C and u (or u1), especially for the year 1930, may not be due to a break in the homogeneity of C, and stresses the usefulness of the international character‐figure C as a measure of magnetic activity not only for intervals of days and weeks (which is undisputed) but also for months and years. Some remarks on the latter point may be permitted, because it now seems quite feasible to ascribe most of the discrepancy found for 1930 not so much to inherent faults or failures of C and u1, but to the different conceptions of magnetic activity underlying both measures.(1) April 1930 has the highest average monthly character‐figure, C = 1.04, of the whole series from 1906 to 1934. In the lists of “Principal magnetic storms” published in this Journal, however, all observatories, except Sitka, reported “no storm” for this month. On the other hand, May 1921, famous for two of the most intensive magnetic storms ever recorded, has only C = 0.83. The u1‐measure gives 52 for April 1930, and 132 for May 1921 (the second highest value for the series 1872 to 1934). This means that the mean monthly C fails to indicate the conspicuous absence of storms in April 1930 as compared with the outstanding storms in May 1921, while u1 represents these conditions satisfactorily.
American URSI broadcasts of cosmic data July to September, 1935
Authors: Ennis C. C. 
Published: February 2008

The data for terrestrial magnetism, sunspots, and solar constant are the same as given in previous tables.The first three columns of the Table give (1) the magnetic character according to the scale 0–2 of the International Commission of Terrestrial Magnetism and Atmospheric Electricty, (2) the type featuring the day other than normal by the letters b, p, o, and i for days marked by bay, rapid pulsations, long‐period oscillations, and irregular oscillations, respectively, and (3) the hour and minute of Greenwich mean time marking the beginning of a storm, the end of the storm being indicated in the footnote to the Table. The next two columns give the data relating to sunspots: (1) the number of groups of spots and (2) the total number of spots. It is to be noted that sunspot‐numbers such as those from Zürich can be obtained from the number of groups and spots given in the Table by the formula N = k (10g+s), where k for Mount Wilson is about 0.7.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, July, August, and September, 1935
Authors: Nicholson Seth B. , Sternberg Elizabeth E. 
Published: February 2008

The magnetic storm of July 7 began with a sudden decrease of 4 gammas in the horizontal intensity followed immediately by an increase of 27 gammas. The most active spot‐group on July 7 was in latitude 34° south and longitude 45° east. A smaller group in latitude 22° north first appeared on July 7, 65° east of the central meridian, and developed its maximum area on July 9.The most active group on September 10 was in latitude 18° south and longitude 72° west. This group first appeared on September 7 in longitude 27° west, and was moderately active from September 7 until it disappeared at the west limb on September 11.
Maxima of potential gradient at Apia
Authors: Sapsford H. B. 
Published: February 2008

The average values of potential gradient of the atmosphere between successive hourly periods 0h–1h, 1h–2h, 23h–24h, on complete days free from negative potential during the period 1924–34 have been tabulated and the means of these average values for each year are given in Table 1. The departures of the hourly means from the daily mean have been plotted to give the curve (full line) in Figure 1, the departure for 0h–1h having been plotted as the ordinate at 1h and so on.The harmonic analysis for this period of eleven years, using 24 ordinates and taking the mean average value for the period 23h–24h as the midnight value givesdV/dh = 115.3 + 15.8 sin (280° + 15t) + 33.6 sin (183° + 30t)+ 6.5 sin (30° + 45t) + 18.2 sin (295° + 60t) + 4.2 sin (146° + 75t)+ 9.1 sin (50° + 90t) where local midnight (zone time, that is, 165° west meridian time at Apia) is the epoch. Figure 1 also shows the curve (dotted line) for the above harmonic series omitting the first (constant) term. The fifth and sixth harmonics have been included because it was found that they decidedly improve the shape of the harmonic curve. The phase‐angle of the 24‐hour wave referred to midnight G. M. T. is 115° (280° zone time) and this agrees very well with the mean phase‐angle of 113° G. M. T. obtained at Mount Stromlo, Australia; but, as C. W. Allen1 points out, this represents a considerable retardation if compared with the 24‐hour wave of the world gradient, the phase‐angle of which is about 183° G. M. T. The maximum of the 24‐hour component at Apia is at 11h.3 zone time (22h.3 G. M. T.), whereas the actual maximum of potential gradient occurs between 8h and 9h (19h and 20h G. M. T.) in the morning and a secondary maximum occurs between 20h and 21h (7h and 8h G. M. T.) in the evening. From the analysis it is seen that the times of the maxima are determined mainly by the 12‐hour and 6‐hour terms, both of which have greater amplitudes than the first harmonic and hence the diurnal‐variation curve shows little resemblance to a single sine‐oscillation. In fact, under normal conditions the potential gradient in Samoa shows a strong 12‐hourly variation in the form of these two well defined maxima, the morning maximum usually being of higher potential and more protracted than the evening maximum.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, October, November, and December, 1935
Authors: Nicholson Seth B. , Sternberg Elizabeth E. 
Published: February 2008

The only magnetic storm in the last quarter of the year 1935 began on October 20 at 10h 38m, G. M. T., and ended on October 22 at 6h. The range in the horizontal intensity (H) was 115 gammas. On October 24 at 6h 40m a sudden increase in H of 29 gammas was followed by a very moderate disturbance.Sunspots have been numerous, large, and active but with apparently no effect on the Earth's magnetic field. Eighty‐seven spot‐groups were observed during the quarter, eight of which were large enough to be seen under favorable conditions without a telescope. Exceptionally bright hydrogen eruptions were observed on December 16, 17, 23, and 31.