bluuebunny/crossref_metadata_2025_split huggingface dataset:
THREE‐HOUR‐RANGE INDEX, K, AT DOMBÅS OBSERVATORY DURING 1939 TO 1942
Authors: Wasserfall K. F. 
Published: February 2008

Introduction—The following resolution was adopted [see 1 and 5 of “References” at end of paper] by the Washington Meeting of the International Association of Terrestrial Magnetism and Electricity in September 1939: “That cooperation of magnetic observatories be sought for a three‐year period (1940‐42) in an international trial‐scheme for provision of three‐hour‐range index K, to characterize the variation in degree of irregular magnetic activity throughout each day, especially in order to meet the request made by the International Union of Scientific Radio‐telegraphy and other bodies for information concerning the magnetic activity more detailed than the present daily magnetic character‐figure, and that this trial‐scheme should replace the scheme for a numerical character‐figure.”The so‐called “Potsdamer erdmagnetische Kenziffer,” which was introduced for Potsdam at the beginning of 1938 [2], served as a model for the index K. Bartels, Heck, and Johnston [3] have given a definition of K; here it will suffice to say that this definition agrees more or less with that for the quantity “storminess” (5) as defined by Krogness and Wasserfall [4]. For S, as well as for K, the range is the difference between the curve actually registered and an arbitrary curve showing quiet conditions. The curve for quiet conditions includes, for “absolute storminess” (AS), the mean daily and day‐to‐day quiet variations, Q and C, respectively, and for K the combined effect of Sq, L, and Dma, where Sq is the solar daily variation, L the lunar daily variation, and Dma the after‐effect of the disturbing‐field (the effect of the decay of the ring‐current), and the non‐cyclic variation on quiet as well as that on the disturbed days [3].
SOLAR AND MAGNETIC DATA, APRIL TO JUNE, 1943, MOUNT WILSON OBSERVATORY
Authors: Nicholson Seth B. , Mulders Elizabeth Sternberg 
Published: February 2008

No magnetic storms were recorded in the second quarter of 1943, although active sunspot‐groups (Mount Wilson Nos. 7571, 7573, 7578, and 7579) with bright chromospheric eruptions were present.Although sunspot‐groups of the new cycle have appeared, minimum sunspot‐activity will probably not be reached for some months. The high‐latitude groups Nos. 7579 and 7582 were certainly members of the new cycle.1 Group 7532, which crossed the central meridian on December1Pub. Astr. Soc. Pacific, 55, 182 (1943).20, 1942, probably belonged to the new cycle, although its polarities were like those of the waning cycle.22Pub. Astr. Soc. Pacific, 55, 43 (1943).
TUCSON MAGNETIC OBSERVATORY APRIL TO JUNE, 1943
Authors: Nelson J. H. 
Published: February 2008

(Latitude 32° 14′.8 N., longitude 110° 50′.1 or 7h 23m.3 W. of Gr.)April 2‐4—A moderate storm began suddenly at 23h10m GMT, April 2, with an increase of 23 gammas in Hduring the first five minutes. There was little outstanding activity and conditions were relatively quiet again by about 08h, April 4. Ranges: D, 11′; H, 80 gammas.
MAGNETIC OBSERVATORY, HERMANUS APRIL TO JUNE, 1943
Authors: Ogg A. 
Published: February 2008

(Latitude 34° 25′.2 S., longitude 19° 13′.5 or 1h 16m.9 E. of Gr.)April 2‐7—Disturbances began without conspicuous abruptness (H increased 14 gammas in ten minutes) at 21h 05m GMT, April 2. The disturbances continued until 21h, April 7. The largest K‐index value was 5 in the period 00h‐03h, April 3.
Huancayo Magnetic Observatory, October to December, 1943
Authors: Ledig Paul G. 
Published: February 2008

Latitude 12° 02′.7 S., longitude 76° 20′.4 or 5h 01m.4 W. of Gr.]November 19–27— Beginning gradually in the early hours of November 19, a magnetic disturbance was recorded which continued at approximately the same intensity for about nine days. The maximum range in horizontal intensity occurred on November 19 and was 225 gammas. The disturbance during the entire period was characterized by small but relatively rapid changes in H and by an almost complete absence of the usual large increase during the daylight hours. There was also a moderate decrease in the mean H‐values during the period and slight disturbance in D and Z.
Atmospheric‐Electric Observatories at Huancayo, Peru, during the Solar Eclipse, January 25, 1944
Authors: Jones M. W. , Giesecke A. A. 
Published: February 2008

IntroductionDuring the solar eclipse of January 25, 1944, (08h 04m to 10h 44m) which reached 88 per cent totality at Huancayo, Peru, at 09h 18m, it seemed desirable that the Huancayo Magnetic Observatory (latitude 12° 02′.7 south, longitude 75° 20′.4 west, altitude 3300 meters) of the Department of Terrestrial Magnetism of the Carnegie Institution of Washington, make special observations of several components of the geophysical program of the Observatory. These included observations of the potential‐gradient of the atmosphere, positive and negative conductivity, and nuclei‐count. A description of the method for measurement of the potential‐gradient and the conductivity can be found elsewhere [see 1 of “References” at end of paper]. Jones and Ledig [2] have shown that in the early morning hours at Huancayo there is a variation in potential‐gradient and conductivity which may be attributed to heating effects of the Sun. It appeared that during a solar eclipse interesting data would be obtained due to the variation in heating effect on the lower strata of the atmosphere. An increase in heating decreases the stability of this lower stratum and causes a mixing of this layer with higher strata, gradually bringing in more nuclei and consequently decreasing the conductivity of the air. The reverse would be expected during a solar eclipse.
Cheltenham Magnetic Observatory, January to March, 1944
Authors: Hershberger John 
Published: February 2008

(Latitude 38° 44′.0 N., longitude 76° 50′.5 or 5h 07m.4 W. of Gr.)January 10—A bay in H in the last three‐hour period of January 10, GMT, gave a K‐index of 6, and was followed by minor activity for a week or more.
Huancayo Magnetic Observatory, January to March, 1944
Authors: Ledig Paul G. 
Published: February 2008

(Latitude 12° 02′.7 S., longitude 75° 20′.4 or 5h 01m.4 W. of Gr.)February 7—A short magnetic disturbance was recorded beginning at 12h GMT, February 7. It was ushered in by a decrease of about 150 gammas in H during the first hour and followed by a number of sharp peaks and bays till after 18h, and then continued for about two hours more in a mild form. D and Z were also noticeably disturbed during the period of activity in H. H was somewhat below normal for the next day. The total range in H was 180 gammas during the disturbed period.
Watheroo Magnetic Observatory, October to December, 1944
Authors: Parkinson W. C. 
Published: February 2008

(Latitude 30° 19′.1 S., longitude 115° 52′.6 or 7h 43m.5 E. of Gr.)December 15–18—A disturbance of moderately severe intensity began with a “sudden commencement” in all three elements at 18h 52m GMT, December 15. Small rapid fluctuations began at 23h 35m on the same day and continued intermittently until 10h 20m December 16, these fluctuations being particularly active between 06h 50m and 08h 00m, December 16. At 13h 30m, December 16, large sweeping movements began in all three elements, H decreasing to a minimum value at 15h 57m and the Z‐trace going beyond the limits of registration between 13h 52m and 15h 38m. After 20h 30m, December 16, the traces steadied somewhat although still slightly disturbed, with H still considerably below its normal value. At 08h 54m, December 17, the traces again became more disturbed with fairly large sweeping movements taking place in all three elements, and with H increasing in mean value. At 23h 00m, December 17, these leisurely movements gave place to small fluctuations which persisted until 08h 30m, December 18, after which the traces resumed their normal character. A faint aurora was observed between 15h and 18h, December 16. Ranges: D, 32′.2; H, 263 gammas; Z, greater than 197 gammas.
On the relation between geomagnetism and the circulatory motions of the air in the atmosphere
Authors: Wulf Oliver Reynolds 
Published: February 2008

General considerationsThe dynamo‐theory of the diurnal variation of the Earth's magnetic field offers an explanation of this phenomenon that is expressed in terms of diurnal motions of the air in the high atmosphere. These motions must be related, even if very indirectly, to the air‐flow below through the changes of horizontal pressure‐distribution, shear, and the vertical movements of the air that in some degree must accompany all of these motions. The altitudes in which occur the air‐motions that generate the electromotive forces and the atmospheric‐electric currents of the dynamo‐theory are not surely known, but that they lie far above those accessible to sounding‐balloons seems certain. Perhaps the best estimate of the altitudes at which these atmospheric‐electric currents flow may be had from the requirement that, at these altitudes there be sufficient molecular collisions and at the same time sufficient ionization that the direct‐current conductivity of the air be relatively large. As an approximate estimate of this it seems that an altitude at the base of or somewhat below theE‐layer of the ionosphere may be taken, which, as an abbreviation to aid in discussion, will be spoken of in the present work as the 60‐ to 80‐km region. How far below this a relation can still be perceived between the air‐motions occurring there and those below remains to be discovered.
American magnetic character‐figure, CA, three‐hour‐range indices, K, and mean K‐indices, KA, for April to June, 1945
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 April to June, 1945, are given in Table 1.
Tucson Magnetic Observatory October to December, 1945
Authors: Westerman C. Edward 
Published: February 2008

(Latitude 32° 14′.8 N., longitude 110° 50′.1 or 7h 23m.3 W. of Gr.)December 13–14—A sudden increase in H of 10 gammas in less than a minute, commencing at 12h 39m GMT, December 13, marked the beginning of a moderate storm. During the first seven hours of the storm the activity was of fairly short period and small amplitude in both D and H. At 16h the H started decreasing at an irregular rate and, after reaching a minimum at 05h, December 14, began to increase and at 15h, December 14, although H was still approximately 100 gammas below normal, the disturbance apparently ended. The increase in declination from 20h, December 13, until 09h, December 14 was followed by a bay lasting an hour, during which D had a range of 21′. Z was relatively undisturbed during the storm. Ranges: D, 21′; H, 203 gammas.
American magnetic character‐figure, CA, three‐hour‐range indices, K, and mean K‐indices, KA, for January to March, 1946
Authors: Scott W. E. 
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 January to March 1946, are given in Table 1.
Alibag Magnetic Observatory April to June, 1946
Authors: Rao M. P. 
Published: February 2008

(Latitude 18° 38′.3 N., longiude 72° 52′.3 E. or 4h 51m.5 E. of Gr.)April 14–15—A disturbance with a very gradual commencement near 08h 30m GMT, April 14, continued till about 20h, April 15, resulting in two K‐indices of 5.
Dual laws of the course of magnetic disturbances and the nature of mean regular variations
Authors: Nikolsky A. P. 
Published: February 2008

The investigation of magnetic storms by the data of the observatories located in high latitudes has revealed at a number of stations the presence of two maxima in the diurnal variation of magnetic disturbance. The study of a vast material, in particular the magnetic observations at Tikhaya Bay for nine years, has shown the changes of magnetic disturbance in the morning and the night hours to depend on different laws. This, in its turn, gave reasons to suggest that the magnetic disturbances in the morning and the night are of different nature. The above conclusion has proved to be of great importance for the further investigation of the diurnal variations of the disturbed magnetic field in high latitudes.Moreover, one has scrutinized in detail the connection between the intensity of accidental irregular fluctuations of the magnetic field (Di), during magnetic storms and the corresponding absolute values of the horizontal component. According to the data at Tikhaya Bay, the correlation‐coefficient between these phenomena was found to be high, r = − 0.70 ± 0.04.The further investigation of the disturbed magnetic field in the same direction, from data at Tikhaya Bay, has shown that the absolute values of the horizontal component for individual quiet hours, selected from the disturbed days, are exactly the same as those on the quietest days. The reduction of the magnetic data for Dickson and Wellen has confirmed the results obtained above. This result cannot be explained from the point of view of our notions on the nature of the phenomena of Sd and Dst in the field of magnetic storms.The result of the present investigation permits the suggestion that during magnetic storms there are only accidental discrete and short‐period disturbed magnetic fields caused directly by the corpuscular streams coming from the Sun. The mean, regular variations Sd and Dst in the disturbed magnetic field do not correspond to any real, prolonged phenomena in the field of magnetic storms and are fictitious, that is, merely statistical results.
Electric current as a probably cause of daily magnetic variation
Authors: Terada K. 
Published: February 2008

Summary—This paper was read, as early as 1941, at the meeting of the Physico‐Mathematical Society of Japan held at Hiroshima University. The Japanese text of this paper (with English abstract) with some of the details was published in the Journal of Meteorological Society [Ser. II, 20, 353–369 (1942) and 21, 171–178 (1943)]. The complete paper has not yet been published because of the War.The paper is restricted to some physical points only and detailed mathematical treatments and the numerical data are omitted.
Revised form of solar and magnetic data from Mount Wilson Observatory
Authors: Nicholson Seth B. 
Published: February 2008

Mrs. Mulders, who for many years has been estimating the solar character‐figures from K2 and Hα spectroheliograms, is leaving the Observatory this month. She is moving to San Francisco where her husband has accepted a position with the United States Navy.It seems to me that this is a good time to terminate the publication [in Terr. Mag. since 1930] of these character‐figures, which have not proved very useful and whose publication at Zurich was terminated some years ago. Since several magnetic observatories estimate the magnetic character‐figure and since other more quantitative measures are superseding it, I question the advisability of continuing its publication also. It is probably worth while to continue the table of magnetic storms and the remarks about the solar activity contemporary with them.
Hermanus Magnetic Observatory January to March, 1947
Authors: van Wijk A. M. 
Published: February 2008

(Latitude 34° 25′.2 S., longitude 19° 13′.5 or 1h 16m.9 E. of Gr.)January 4–6—A storm of moderate intensity began with a sudden commencement at 11h 17m GMT, January 4 (H, 39 gammas in seven minutes), and continued until about 16h, January 6. Five K‐indices of 5 were recorded during that period.
The ionosphere as a measure of solar activity
Authors: Phillips M. Lindeman 
Published: February 2008

Critical frequencies of all regular ionospheric layers vary diurnally, seasonally, with geographic latitude and longitude, and with solar activity so that, for any location and any season

urn:x-wiley:00968013:media:tma33214:tma33214-math-0001
where f0 is the critical frequency, G and H are functions of (t), the time of day, and S is the sunspot‐number. For locations where such ionospheric trends are well established, observations of critical frequency may be used to determine an ionospheric “sunspot‐number”. If values of F2‐layer critical frequency for hours near local noon are used, since these generally have the most pronounced variation with solar activity, the ionospheric “sunspot‐number” obtained is considerably closer to its running‐average value than are ordinary sunspot‐numbers to their running averages. In addition, this measure is practically independent of varying atmospheric conditions and personal variation among observers, and therefore probably presents a more precise index of solar activity.
Discussion of data for magnetic declination at Oslo, 1843–1930, and before 1843
Authors: Wasserfall K. F. 
Published: February 2008

The Magnetic Observatory at Oslo (latitude 59° 54′.7 north, longitude 10° 43′.4 east) was founded by Professor Christopher Hansteen. The author has compiled the resulting data as regards horizontal intensity and magnetic activity in this Journal [see 1, 3, 5 of “References” at end of paper]. The daily values at 09h and 14h of magnetic declination are given in reference [2] for 1843–1930; the present communication summarizes the general discussion of the material for declination with some remarks on correlation with sunspot‐activity and observations made prior to the series begun by Hansteen in 1842.There were naturally many difficulties encountered in compiling reduction constants because of changes in azimuth of mark, alterations and repairs of buildings, changes of scale‐values and of base‐lines, and magnetic station‐differences for the several piers used in so long a period. Figure 1 gives a plan of the Observatory and environs as at present; originally the area was a rural one but it is now surrounded by a modern city. The hut for observations of declination, which was removed in 1908, was at point marked U.L. (now the University Library). The plan shows also the situation of the four piers I–IV, the pier where the unifilar magnetometer was mounted, and the one where the bifilar magnetometer was installed. It is of interest to note the isogonic lines at the Oslo Observatory Park and in the general region surrounding Oslo, as shown by Figures 2 and 2A for the epoch 1929.5.
On minute, rapid, periodic changes of the Earth's magnetism
Authors: Eschenhagen Max 
Published: February 2008

In a previous communication to the Academy, a curve was exhibited which had been obtained at the Potsdam Magnetic Observatory by automatic photographic registration of the horizontal component of the earth's magnetic force. The striking feature of this curve was the fact that, in addition to the usual larger perturbations, there was a series of very small waves having nearly the same constant period, so that these waves could, in a certain way, be regarded as constituting the elementary pulsations of the earth's magnetism.Since then it has been possible to obtain about sixty such curves. The sensitiveness of the intensity variometer was, as before, a very high one (1 mm. of ordinate=0.00004 cm−½ g½ sec−1), and for the time‐scale a length of abscissa of 24 cm. was taken to represent one hour, hence about twelve to sixteen times that of the usual registration.
International Magnetic Conference.—Welcoming Address
Authors: Ayrton W. E. 
Published: February 2008

Section A this year is very fortunate in having its meetings associated with those of an “International Conference on Terrestrial Magnetism and Atmospheric Electricity,” which is attended by the members of the “Permanent Committee for Terrestrial Magnetism and Atmospheric Electricity” of the “International Meteorological Conference.” It has been arranged that this Permanent Committee, of which Professor Rücker is the president, shall form part of the General Committee of Section A, and shall also act as the Committee of the International Conference, which will itself constitute a separate department of Section A. For the purpose, however, of preparing a Report to the International Meteorological Conference, and for similar business, this Permanent Committee will act independently of the British Association.My first duty to‐day, therefore, consists in expressing the honor and the very great pleasure which I feel in bidding you, members of the International Conference, most heartily welcome.
On the establishment of temporary magnetic observatoriés in certain localities, especially in tropical countries
Authors: von Bezold  , Rykatschew  
Published: February 2008

Die nachstehenden Vorschläge stützen sich wesentlich auf eine Abhandlung, welche der eine der Unterzeichneten im Jahre 1897 veröffentlicht hat. In dieser Arbeit wurde versucht, durch Vergleichung mit den Beobachtungen die Hypothese zu prüfen, dass die Kräfte, welche die erdmagnetischen Erscheinungen hervorrufen, in der Erdoberfläche selbst ein Potential besitzen; auf Grund von Werthen, die ihm Herr A. Schmidt für je 72 um je 5 Längengrade von einander abstehende Punkte auf 4 Parallelkreisen mitgetheilt hatte, gelang der Verfasser zum Schluss, dass die in Procenten der Amplitude des Potentials ausgedrückten Abweichungen von jener Hypothese um den 40—45 Grad nördlicher Breite am grössten ausfallen, d. h. also gerade in jenen Breiten, für welche die meisten und besten Beobachtungen vorliegen ; diese Abweichungen erreichen hier Werth bis zu 8% der Amplitude, während sie in niedrigen Breiten nur wenige Beobachtungen vorhanden sind, viel kleiner sind, theilweise sogar ganz verschwinden. Für die Theorie des Erdmagnetismus wäre es von höchster Wichtigkeit, darüber Gewissheit zu erlangen, ob dieses Resultat nicht vielleicht durch den Mangel an Beobachtungen, besonders aus dem Aequatorialgebiete, bedingt ist.In derselben Arbeit hat der Autor auf Grund der von A. Schuster mitgetheilten Werthe eine Karte entworfen, welche für den Sommer ein anschauliches Bild vom Verlaufe der Gleichgewichtslinien des Potentials der täglichen Variation giebt; die Darstellung der Karte bezieht sich auf den Mittag nach Greenwicher Zeit.