bluuebunny/crossref_metadata_2025_split huggingface dataset:
Correlations between solar activity and atmospheric electricity
Authors: Bauer Louis A. 
Published: February 2008

The question is revived whether atmospheric electricity is in any way dependent upon solar activity. The present investigation is based chiefly upon the accumulated data for electrically‐quiet days pertaining to the atmospheric potential‐gradient and its diurnal and annual variations. It is found that during the past two sun‐spot cycles (1901–1923), the atmospheric potential‐gradient and the amplitudes of the diurnal variation and of the annual variation generally increased with increased sun‐spot frequency; the increase in the particular electric element considered is about 20 to 35 per cent, on the average, for a change of 100 in the sun‐spot number. The correlation coefficient, on the average, is about 0.75.If reliance can be placed on older series of atmospheric‐electric observations, made prior to 1901, then there are indications that during two periods, centering about 1855 and 1889, the reversed relationship applied, namely, that increased atmospheric potential‐gradient and increased amplitudes of diurnal and annual variation were associated with decreased sun‐spot frequency. The forthcoming sun‐spot cycle will afford opportunity to examine into this matter more thoroughly.An interesting correlation is exhibited by the atmospheric‐electric and magnetic data for 1893, which unite in showing a decrease in the electric and in the magnetic activity at the time of maximum sun‐spot frequency. There is thus an indication that the usual measures of solar activity are not always an adequate measure of such solar radiations and emanations as may affect the electricity of the atmosphere and the magnetic field of the Earth.The hope is expressed that the results of the present investigation will contribute towards the multiplication of widely distributed atmospheric‐electric stations where all possible care will be taken to ensure continuity of strictly comparable data for a sun‐spot cycle, and longer.
The Kursk magnetic anomaly
Authors: Lasareff P. 
Published: February 2008

In a previous note I gave the results of investigations carried out during 1921–1923, and in the present paper I propose to give the details of work executed in the period of 1923–1925. I have already indicated the dimensions and direction of the anomalous zone in the Kursk Government, Figure 1 is a general map of the anomalies of magnetism and gravity; it also shows the direction of the anomaly and the relative value of the vertical intensity Z, which has two maxima, one in the Stschigry district and the other in the Stary Oscol district.The details of the variation of the vertical intensity along the anomaly are given in Fig. 2.
Principal magnetic storms recorded at the Sitka Magnetic Observatory, October to December, 1927
Authors: Ulrich F. P. 
Published: February 2008

October 9–11 1927.—This storm is peculiar because of the short rapid oscillations of the elements on October 10 at 13h to 23h. After 15h the mean values of the oscillations are about the mean values of the normal curves. The oscillations are so rapid that the curves are mostly spots up to 21h, but, each curve being separated, the path can be accurately determined.October 12 1927—The motion of the curves is so rapid that in places the curves consist of spots only from 11h to 17h. At that time the trace was changed and the light increased. From 17h to 22h the curves consist of fairly large rapid oscillations.
Charles Chree
Authors: Chapman S. 
Published: February 2008

Charles Chree, for many years one of the most eminent and indefatigable workers on terrestrial magnetism, died on August 12, 1928, after an illness, patiently and bravely borne, lasting for several months.He was the second son of the Rev. Charles Chree, D.D., minister of Lintrathen in Forfarshire, a country parish a few miles from Kirriemuir—Barrie's “Thrums”; he was born on May 5, 1860. He was educated at the Grammar School, Old Aberdeen, and at the Universities of Aberdeen, where he gained distinction in classics as well as in mathematics and physics, and Cambridge. At the latter he was sixth wrangler in 1883, and also took a first‐class in the Natural Science Tripos, Part 2. In 1885, he was elected to a fellowship, extended in 1890 as a research fellowship, at King's College, where he had been a mathematical scholar. He worked in the Cavendish Laboratory, and wrote many papers, to which numerous references may be found in Love's treatise, on the mathematical theory of elasticity.
Correction‐factors and corrected daily means of the solar indices as given in the International Astronomical Bulletins
Authors: Brown Howell C. 
Published: February 2008

An attempt was made to use the solar character‐numbers, as given in the International Astronomical Union Bulletins, for correlation with radio‐fading. The daily reports from the cooperating observatories varied so greatly that it was considered necessary to make a corrected average.The various stations were compared by groups, in three‐month periods when possible, but at times it was necessary to make use of a six‐month period. From these comparisons a multiplying‐factor was prepared and the daily reports thus corrected. The corrected figures were then averaged to obtain a new daily mean.Some general comments on the use of standard plates are included.
Magnetic secular variation for epoch 1930
Authors: Ennis C. C. 
Published: February 2008

In the JOURNAL for September 1931 appeared a paper by J. Bartels on geophysical stereograms. It was the privilege of the writer to assist the computations incident to the construction of the various stereograms accompanying that paper, and it seems a worth‐while contribution in the field of magnetical investigation to make available the data employed in the construction of stereogram 8 which shows the secular variation of the magnetic field‐vector at the intersections of the meridians 0°, 20°, 40°, etc, with the circles of latitude 60°N, 40°N, . .40°S.As the resulting salient features of the secular variation were pointed out by Bartels, it is intended herein to give only the data upon which the stereogram depends. These are embodied in Table 1.
Terrestrial‐magnetic activity and its relations to solar phenomena
Authors: Bartels J. 
Published: February 2008

A homogeneous series of monthly means of terrestrial‐magnetic activity for the years 1872 to 1930 is derived and extended backward, in annual means, to 1835. The annual variation of magnetic activity and of the relative sunspot‐numbers is discussed by means of new tests for periods. Only the semi‐annual wave in magnetic activity is recognized as physically significant. Its maxima prefer the times when the Sun is in the celestial equator, and not, as has been suggested, the times when the Sun's axis is most inclined towards the ecliptic. This view is supported by tests using the harmonic dial and the probable‐error circle, and several independent considerations.The close relations between sunspot‐numbers and terrestrial‐magnetic activity in the annual and monthly means are discussed. Some general statistical aspects are given for the treatment of the correlation between such series with after‐effects, for which both solar activity and terrestrial‐magnetic activity are typical. The homogeneity of the whole available series for relative sunspot‐numbers and for areas of sunspots and faculae is tested; some inhomogeneities are found, apart from a general lag of terrestrial‐magnetic activity that has occurred in some sunspot‐cycles. A break in the homogeneity of the international magnetic character‐figures in recent years is discovered.The individual 27‐day recurrences in terrestrial‐magnetic activity during 1906–31, and their relations to solar activity are discussed with the help of a graphical day‐by‐day record. They indicate the existence of persistent active areas on the Sun's surface, called M‐regions, which, in many cases, cannot be coordinated to such solar phenomena as are observable by direct astrophysical methods. This holds in particular for the new solar indices which are available for the years 1928–30, and which are found so closely correlated to sunspot‐numbers, that they fail to improve the correlation between solar activity and terrestrial‐magnetic activity. Observations of terrestrial‐magnetic activity yield therefore not only information about geophysical influences of such solar phenomena that may be traced in astrophysical observations, but supplement these direct observations themselves.
Cheltenham Magnetic Observatory October to December 1931
Authors: Hartnell Geo. 
Published: February 2008

(Latitude 38° 44′.0 N.; longitude, 76° 50′.5 or 5h 07m.4 W. of Gr.)There were no large magnetic disturbances during the quarter. A mild storm began at about 5h, G. M. T., October 29, and continued to about 22h, October 30; the ranges were 57.7′, 196γ, and 141γ in declination, horizontal intensity, and vertical intensity, respectively.
Apia Observatory October to December, 1934
Authors: Wadsworth J. 
Published: February 2008

November 7—A slight disturbance began at 4h 50m, G.M.T., with a gradual increase of 6γ in H. It reached a maximum increase of 32γ at 8h 45m and afterwards fell by 24γ between then and 9h 10m. The corresponding movements in Z were much smaller, namely, increases of 2γ and 5γ and then a fall of 6γ.December 1—A sudden increase of 22γ occurred in H at 4h 57m, G.M.T., and an increase of 5γ in Z.December 11—A sudden increase of 15γ took place at 10h 34m, G.M.T., with an increase in Z of 3γThe statistical aspects of the application of harmonic analysis, introduced by A. Schuster in his famous paper on the investigation of hidden periodicities, are discussed on the basis of recent developments in the theory of probability. Between the two extreme cases of random fluctuations and persistent waves, hitherto discussed exclusively, the intermediate case of quasi‐persistence is introduced and recognized as a common phenomenon in the time‐functions of meteorology, geophysics, and cosmical physics. Statistical methods, based on the conception of the harmonic dial, are given for dealing with quasi‐persistence and its effect on tests for persistent waves, and they are generalized for the case of periodicities of other form than that of the sine‐wave. Typical examples are given illustrating various forms of random fluctuations, quasi‐persistence, and persistence, as well as questions related to harmonic analysis, such as the periodogram, non‐cyclic change, curvature‐effect, equivalent length of sequences, effective expectancy, random walk, interference, and the infective property of quasi‐persistence on adjacent periods (see summary at end of paper).
Concerning the magnetic numerical character‐numbers
Authors: Egedal J. 
Published: February 2008

In a communication presented to the Assembly of the Association of Terrestrial Magnetism and Electricity held at Lisbon September 19331 the author gave the results of a comparison of numerical character‐numbers with international character‐numbers. It was shown that the numerical character‐number corresponding to the international character‐number 0.2 for the magnetic observatory at Rude Skov was about 120 in the winter (December) and about 240 in the summer (June).In the present note the magnitude of the numerical character‐numbers for magnetically quiet days for observatories at different latitudes is examined. The numerical character‐numbers for the five international quiet days of June and of December for the years 1932 and 1933 are considered.
The hundredth anniversary of the Sverdlovsk Magnetic Observatory
Authors: Abels R. G. 
Published: February 2008

Introduction—On January 1, 1836, in Sverdlovsk (formerly Ekaterinburg) regular meteorological and, at the end of that same year, magnetic observations were initiated. Accordingly we celebrated the hundredth anniversary of the Sverdlovsk Magneto‐Meteorological Observatory on June 25, 1936. The Anniversary Symposium of the Observatory published at that time contains the following articles dealing with the magnetic activities of the Observatory during the past 100 years.G. F. Abels, Magnetic observations in Sverdlovsk (formerly Ekaterinburg).
Tucson Magnetic Observatory July to September, 1936
Authors: Joyce J. Wallace 
Published: February 2008

(Latitude 32° 14′.8 N., longitude 110° 50′.1 or 7h 23m.3 W. of Gr.)July 5–8—A moderate disturbance was characterized by an abrupt commencement in all three elements at 02h.5 GMT, July 5. H increased 29 gammas in six minutes. In general, the storm consisted of a series of long bays with a three‐hour interval of short‐period activity starting at 9h, July 6. The storm ended at about 3h, July 8. Total ranges: Horizontal intensity, 90 gammas; vertical intensity, 59 gammas; declination, 12′.
Apia Observatory April to June, 1937
Authors: Wadsworth J. 
Published: February 2008

(Latitude 13° 48′.4 S., longitude 171° 46′.5 or 11h 27m.1 W. of Gr.)April 12—A disturbance commenced suddenly at 08h 50m GMT, April 12, with an instantaneous increase in H equal to 12 gammas. The maximum value of H was attained between 11h and 12h and the minimum at 18h 25m. The range in H was 46 gammas.
Natural residual magnetism of eruptive rocks
Authors: Koenigsberger J. G. 
Published: February 2008

PART I—GeneralThe study of the magnetic behavior of rocks under the influence of the Earth's magnetic field and of time, and the study of the history of terrestrial magnetism by aid of the rocks and minerals is facilitated by a knowledge of some new facts connected with physics, physical chemistry, mineralogy, and petrography. As the literature is scattered through many periodicals in various languages, the facts, which are not generally known, are summarized here. Some of these appear of interest in connection with the general theory of ferromagnetism.
Apia Observatory, January to March 1938
Authors: Wadsworth J. 
Published: February 2008

(Latitude 13° 48′.4 S., longitude 171° 46′.5 or 11h 27m.1 W. of Gr.)January 16‐18—A sudden commencement occurred at 00h 44m GMT, January 16, when H increased 56 gammas. After this the traces were only slightly disturbed until 22h 37m when rapid oscillations in H and Z were recorded. H fell gradually through a range of 281 gammas until 18h 52m, January 17, when it returned to normal values though it continued to show slight disturbances. Ranges: Z, 32 gammas; D, 9′.
Cheltenham Magnetic Observatory October to December, 1938
Authors: Ludy Albert K. 
Published: February 2008

October 7–9—A storm occurred between 06h 15m GMT, October 7, and 02 h October 9. The oscillations were irregular and the larger ranges took place between 22 h, October 7, and 08h, October 8. Ranges: D, 47′; H, 225 gammas; Z, 238 gammas.October 23–28—After a period of slight disturbance beginning October 23, there gradually developed a mild storm which lasted several days until October 28. Although the ranges were not great there was continmd activity during this time.
Cheltenham Magnetic Observatory July to September, 1939
Authors: Ludy Albert K. 
Published: February 2008

July 3–4—A sudden commencement occurred at 00 h 39 m GMT, July 3, and was followed by a period of moderate disturbance lasting until 06 h, July 4. Ranges: D, 28′; H, 298 gammas; Z, 150 gammas.July 4–6—After an interval of about eight hours of quiet conditions a storm began at 14 h 07 m GMT, July 4. All three elements were active until 05 h, July 6. Ranges: D, 61′; H, 424 gammas; Z, 426 gammas.
Huancayo Magnetic Observatory October to December, 1939
Authors: Wells H. W. 
Published: February 2008

October 1–2—Abnormally large diurnal bays in H occurred on both October 1 and 2 with respective ranges of 326 and 314 gammas.October 3–4—A magnetic storm featuring large fluctuations in H began at 12h GMT, October 3, and ended at 05h, October 4. Ranges: D, 13′.7; H, 465 gammas; Z, 67 gammas.
Apia Observatory January to March, 1940
Authors: Sapsford H. Bruce 
Published: February 2008

(Latitude 13° 48′.4 S., longitude 171° 46′.5 or 11h 27m.1 W. of Gr.)March 23—A minor disturbance began at 06h 15m GMT, March 23 with a sudden increase in H of 21 gammas and in Z of 6 gammas. The H‐trace then fell to a minimum at 09h 22m through a range of 81 gammas. The corresponding range of Z was 16 gammas. D was only slightly affected. The trace returned to normal level shortly after 10h but small rapid oscillations continued.
Secular Change at Cheltenham, Maryland
Authors: Howe H. Herbert 
Published: February 2008

It will be remembered that about 1933 a phenomenal change took place in the rate of secular change of declination at Cheltenham, Maryland. Within about a year the rate changed from an increase of 4 minutes per year to zero. This change of rate has persisted, the present rate being a few tenths of a minute per year, decreasing. (4′ per year means about 21γ per year)Recently a larger and nearly as abrupt decrease has taken place in the rate of secular change of horizontal intensity. Determination of a rate of secular change for short periods is complicated by the annual variation, which has an amplitude of some 20γ. Plotting monthly means and drawing a smooth curve, the following were obtained as approximate rates of secular change (in gammas per year, decreasing) for the middles of consecutive years from 1933 to 1940: 54, 50, 47, 44, 41, 32, 21,3.
American magnetic character‐figure, CA, three‐hour‐range indices, K, and mean K‐indices, KA, for October to December, 1942, and summary for year 1942
Authors: Johnston H. F. 
Published: February 2008

Summaries of American URSI broadcasts have appeared regularly in this JOURNAL since the issue for December, 1930.As set forth in this JOURNAL for June, 1937, “The Department of Terrestrial Magnetism and the United States Coast and Geodetic Survey with the cooperation of the United States Army and the United States Navy communication‐services and several amateur radio stations have undertaken to supply the American character‐figure based upon the reports of the seven American‐operated observatories—those of the Department of Terrestrial Magnetism at Huancayo in Peru and at Watheroo in Western Australia, and those of the United States Coast and Geodetic Survey at Cheltenham (Maryland), Honolulu (Hawaii), San Juan (Puerto Rico), Sitka (Alaska), and Tucson (Arizona).” This character‐figure is being designated CA, and its values for the first twelve, the second twelve, and all twenty‐four hours of each Greenwich day for October to December, 1942, are given in Table 1.
Magnetic activity at Dombås based on absolute storminess for the horizontal component
Authors: Wasserfall K. F. 
Published: February 2008

Introduction—Absolute storminess, AS, means the diurnal sum of positive and negative storminess, and is one of the best expressions for magnetic activity. Since 1916 daily values for AS, for D, H, and V, have been published in our year‐books, but so far no attempt has been made to make further use of these valuable data, except that AS for D has been regularly used as the basis for our contribution to the international character‐number, C.For various reasons it has been considered desirable to devise a new international measure for magnetic activity in addition to the character‐number, C. There is no doubt that AS would be a good basis for this new international measure except that few observatories compute data for AS. For this reason the Assembly at Washington in September 1939 decided to base the international cooperation, not on AS, but on the so‐called three‐hour‐range index K. As the work required for deriving the K‐index is much less than that connected with working out data for AS, this scheme for international cooperation seems to have been generally accepted, and—judging from results already published—there is every reason to believe that the K‐index more or less covers what is required for the new measure for magnetic activity.
Magnetic Observatory, Hermanus, October to December, 1942
Authors: Ogg A. 
Published: February 2008

(Latitude 34° 25′.2 S., longitude 19° 13′.5 or 1h 16m.9 E. of Gr.)October 2–5—A sudden‐commencement storm began at 02h 46m GMT, October 2. H increased 21 gammas in five minutes. At first the disturbances were small and were characterized by pulsations and oscillations on all traces from 08h to 19h, October 2. The intensity of the storm gradually increased until bays of K‐index 6 were formed on all traces at 20h to 21h, October 2. On October 3 at 01h and 04h, bays of K‐index 4 were formed on all traces. Disturbances continued until 01h, October 5.
Brief Compendium on the Sphere and Art of Navigating
Authors: Cortes Martin 
Published: February 2008

Chapter 3—On the virtue and property of the lodestoneThe lodestone according to the Cardinal Cusanus has essence, virtue, and operation. The virtue is engendered by the essence; from the essence and virtue is born the operation, so that the stone communicating its virtue to the iron for this reason causes the iron to move although between them there be a silver dish or plate or something similar. The attractive force of the lodestone causes the nature of the iron to join with it and at rest so much that although heavy and weighty it does not fall because the nature of the iron does not remain in it but joins with the nature of the stone which seems to extend whence we see that by this union it happens that it not only attracts this iron but this to another, and another to another and thus is formed a chain* as experience has shown. St. Augustine was surprised as he has written in the books of “De Civitate Dei”1 because on a plate he saw a bit of iron agitated when the lodestone was moved about under the plate.
Sitka Magnetic Observatory, October to December, 1943
Authors: Pinckney Harold W. 
Published: February 2008

Latitude 57° 03′.0 N., longitude 135° 20′.1 or 9h 01m.3 W. of Gr.]October 1–4—The disturbance in progress at the end of September continued with diminishing intensity through the night of October 4.
Final Relative Sunspot‐Numbers for 1943
Authors: Brunner W. 
Published: February 2008

Table 1 contains the final sunspot‐numbers for 1943, for the whole disk 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.
Magnetic Data, Cape Town and Hermanus Magnetic Observatories, 1940–1942
Authors: Ogg A. 
Published: February 2008

The Cape Town Magnetic Observatory, which was established for the Polar Year 1932–1933, was unsuitable as a permanent observatory owing to magnetic disturbances caused by the electric railways. The observatory, however, continued in operation until the end of 1940, when a new observatory at Hermanus was ready for work.Table 1 gives the mean yearly values of the magnetic elements at the Magnetic Observatory, Hermanus, for the years 1941 and 1942, and also gives the relation between these and the Cape Town values for the years 1933–1940, which were published in this JOURNAL September 1941, p. 364.