bluuebunny/crossref_metadata_2025_split huggingface dataset:
Tucson Magnetic Observatory July to September, 1937
Authors: Hershberger John 
Published: February 2008

(Latitude 32° 14′.8 N., longitude 110° 50′.1 or 7h 23m.3 W. of Gr.)July 19–26—A sudden increase of 42 gammas in H occurred at 12h 53m GMT, July 19, and was followed by a prolonged period of disturbance. For two days the disturbance consisted chiefly of short‐period oscillations of H and Z), the latter being of small amplitude. By 13h, July 21, the disturbance appeared to have ended. But about 18h the fluctuations began again very gradually, accompanied this time by a slowly decreasing value of H. At 07h, July 22, there began a series of irregular large movements, which continued with varying intensity for a little more than three days. The minimum of H for the storm occurred at 1h 51m, July 24. By 03h 28m H had increased 122 gammas, this being the largest change in an equivalent interval during the entire period. The disturbance died out very gradually, ending about the middle of July 26.
Relations between terrestrial magnetism and cosmic‐ray intensity
Authors: Hess Victor F. , Demmelmair A. , Steinmaurer R. 
Published: February 2008

Certain relations between the variations of the Earth's horizontal magnetic force H and of the observed cosmic‐ray ionization J have been found in the continuous registrations of the cosmic‐ray ionization on the Hafelekar, 2300 meters above sea‐level (near Innsbruck, Austria) during the year 1936–37 as follows:(1) A positive magnetic effect, ME1 is indicated during magnetic storms with increase of J associated with increase of H and vice versa. A similar effect has been noticed rather often also in the daily mean values of J and H during magnetically undisturbed days. ME1 amounts to +0.57 per mille of the cosmic‐ray ionization for an increase of the horizontal force by one γ (0.00001 gauss).(2) The analysis of the daily mean values for one year discloses a second effect, ME2, of opposite sign (increase of H accompanied by decrease of J) and smaller than ME1. ME2, for the average of the year 1936–37, is about −0.20 per mille per γ.(3) A similar negative magnetic effect, ME3, is found from the strong correlation between the diurnal variation of H and J; ME3= −0.2 per mille per γ.(4) Another negative effect, ME4, can be derived from the anti‐parallel variations of the monthly means of H and J (seasonal curves); ME4 = −1 per mille per γ.The three first‐mentioned effects can be explained qualitatively by adopting the hypothesis of the electronic ring‐currents in the outer space around the globe. The seasonal effect is not yet explained and it seems possible that its connection with terrestrial magnetism is accidental, in spite of the strong correlation.
Tucson Magnetic Observatory, October to December 1937
Authors: Hershberger John 
Published: February 2008

(Latitude 32° 14′.8 N., longitude 110° 50′.1 or 7h 23m.3 W. of Gr.)October 3–4—At 11h 18m GMT, October 3, H increased 25 gammas in three minutes. At the same time east declination decreased 2′. The elements continued moderately disturbed until 24h, when H began to decrease rapidly. This was soon followed by large oscillations in H and D, lasting until 08h, October 4. The larger oscillations also affected Z moderately. Except for minor disturbances of the saw‐tooth variety and a low value of H, the storm ended at 08h, but the elements were not entirely normal for about 19 hours later. The range of H for the storm was 233 gammas. The ranges of D and Z were scarcely larger than the normal diurnal ranges.
Discussion of S. Chapman's note on radio fade‐outs and the associated magnetic variations
Authors: Dellinger J. H. 
Published: February 2008

In response to Dr. Fleming's suggestion I am glad to comment on Dr. Chapman's Note above mentioned. Dr. Chapman showed that Dr. Birkeland had listed as a separate type of magnetic perturbation an occurrence in 1902 which is now seen to be one of the type associated with sudden disturbances of the ionosphere caused by solar eruptions. Dr. Birkeland's discernment is an interesting instance of partial recognition of this cosmic phenomenon as revealed by various early records and publications. Other instances, to which I have previously called attention, are the observation by T. L. Eckersley of a separate type of radio transmission interruption in 1928, and the simultaneous occurrences of magnetic perturbations and solar eruptions in 1859, 1872, etc.The outlines of the entire phenomenon emerged in 1935 and early 1936, when it was discovered that radio, magnetic, earth‐current, and solar effects occur simultaneously, that the three terrestrial effects have characteristics differentiating them from other vagaries (for example, magnetic storms), that are manifestations of a disturbance in the ionosphere, that this disturbance is a sudden increase in ionization below the E‐layer caused by ultra‐violet radiation from a solar eruption, and that the effects vary from a maximum in those latitudes and longitudes where the Sun's rays are vertical to zero in the night hemisphere.
Sitka Magnetic Observatory, January to March 1938
Authors: Gebhardt Robert E. 
Published: February 2008

(Latitude 57° 03′.0 N., longitude 135° 20′.1 or 9h 01m.3 W. of Gr.)January 4—A small disturbance began gradually at about 10h GMT and gradually increased in intensity to a maximum at 13h 30m. Thereafter the disturbance subsided; the trace had gradually returned to about normal values at 24h January 24. Ranges: D, 74′; H, 799 gammas; Z, 608 gammas.
The ionosphere at Huancayo, Peru, January, February, and March 1938
Authors: Wells H. W. , Stanton H. E. 
Published: February 2008

This report is in continuation of that published in this JOURNAL (43, 169–171, 1938) on ionospheric data from continuous multifrequency ionospheric recordings at the Huancayo Magnetic Observatory for January, February, and March, 1938.Table 1 contains mean hourly values of virtual height and critical frequency for the ionospheric regions for each hour during the first quarter of 1938. Also included are mean hourly values of the lowest frequency recorded (designated ƒmin) during the frequency‐sweep from 16.0 to 0.516 mc/second, which give a relative measure of absorption of radio signals in the lower ionosphere during the day. The data of Table 1 comprise recordings for each hour of the day and for every day of the month except for short intervals necessary for maintenance to the equipment.
The non‐magnetic R.R.S. Research
Authors: Edgell J. A. 
Published: February 2008

Readers of this JOURNAL have learned from brief notes published from time to time, that a non‐magnetic vessel, the Research, is being built by the British Admiralty to continue the magnetic survey of the oceans inaugurated by the Carnegie Institution of Washington through its Department of Terrestrial Magnetism and carried on by the non‐magnetic vessel, Carnegie, from 1909 until her destruction by explosion and fire in November 1929. It is especially fitting that Great Britain should assume the responsibility of continuing this important work in view of her great maritime interests. For many years the magnetic charts issued by the hydrographic services of the various countries have been based in increasing degree on data obtained by the Carnegie, but serious gaps in available data which would have been filled had she completed her last cruise, and the absence of information regarding the secular change in certain regions render imperative the resumption of the interrupted oceanic survey both from theoretical and practical considerations.To remedy this condition, the construction of the Research was authorized over three years ago but the keel was not laid until September 9, 1937. Since that time good progress has been made. In order to assist in designing the vessel and her instrumental equipment, the Carnegie Institution of Washington, upon invitation of the Admiralty, made arrangements that William J. Peters, first commander of the Carnegie and designer of many of the special and improved types of magnetic instruments used at sea, spend a year in London as consultant on the design of the new vessel and of her special instruments. In addition all information regarding the Carnegie was placed at the disposal of the British Admiralty, thus facilitating greatly the design of the new vessel.
The ionosphere at Huancayo, Peru, April, May, and June, 1938
Authors: Wells H. W. , Stanton H. E. 
Published: February 2008

This report on ionospheric conditions is in continuation of those published in preceding issues of this Journal (43, 169–171, 257–260, 1938) submitting results of continuous multifrequency ionospheric recordings at the Huancayo Magnetic Observatory. The current data for the months, April, May, and June, 1938, are obtained from recordings for each hour of the day and for every day of the month except for short intervals necessary for maintenance to the equipment.Table 1 contains mean hourly values of virtual height, critical frequency, and lowest frequency received for the second quarter of 1938. Figure 1 presents the data of Table 1 in graphical form. The following general discussion of characteristics seems pertinent:
A 27.3‐day period in the aurora borealis
Authors: Dixon F. E. 
Published: February 2008

In the course of a general study of the frequency of occurrences of aurora in Scotland during the years 1858–1938 a well‐marked period of length about 27.3 days was found to exist. Commander W.R. Priston has found a similar period in other meteorological elements, and it was his work (not yet published) which prompted the present investigation. The period is more than the well known 27‐day recurrence observed in many magnetic and associated phenomena, since that usually continues for only a few solar rotations, whereas this period has persisted for 80 years.The data used in this investigation were simply the dates on which aurora was seen from one or more of the meteorological stations in Scotland, including Orkney and Shetland. From 1858 to 1919 these are available in the Journal of the Scottish Meteorological Society and since 1924 they have been included in the Lerwick section of the Observatories' Year Book. For the intervening years the Reports of the Registrar General for Scotland were consulted, the required information being included in the meteorological notes appended thereto. In a few cases, chiefly in the earlier years, the original climatological returns have been referred to. This was necessary when the published information was indefinite, for example “Aurora was seen on nearly every night in October.” There were 5224 nights on which aurora was seen, an average of 66 nights per year and 5.1 per 27.3‐day period. The number of nights varied from 161 in the year July 1869 to June 1870 to five in 1912–1913.
Note on early fade‐out investigations
Authors: Braaten Arthur M. 
Published: February 2008

In communications by Chapman [see 1 of “References” at end of paper], Kirby [2], Dellinger [3], and Appleton [4] there have been pointed out several interesting instances of early observations of the various effects associated with visible eruptions in the Sun's chromosphere. I should like to add to the store of information on the subject by presenting some material which I believe has not been generally available heretofore. As a matter of historical interest, it may be noted that as early as 1928 there had been advanced an explanation relating the Sun, the ionosphere, and radio fade‐outs.On October 10, 1928, a catastrophic disturbance affecting short‐wave radio transmission occurred. The phenomenon, manifested by a sudden cessation of reception, was of such a nature as to immediately attract considerable interest. The salient features of the disturbance were: Suddenness and simultaneity of onset; completeness of effect; relative rapidity of recovery, absence of any associated magnetic perturbation. It may be stated here that a few fades of similar character had been observed previously, both in this country, by the Radio Corporation of America [5], and in England, by the Marconi Company [6]. These were presumably not as devastating or far‐reaching in effect as the later fade; at least they had apparently occasioned no more than ordinary interest.
The fourth centenary of William Gilbert of Colchester
Authors: Harradon H. D. 
Published: February 2008

In view of the important contribution to the science of terrestrial magnetism made by William Gilbert, it seems fitting to recall that 1940 marks the fourth centenary of his birth. We are indebted to the article by E. C. Smith, Nature of January 6, 1940, for some of the facts given below.He was born at Colchester, County Essex, England, in 1540. Little is known with certainty of his early days but at the age of twenty he graduated from St. John's College, Cambridge. He later spent several years in travel and study on the Continent and in 1569 obtained the degree of M.D. Four years later he settled in London to practice medicine, becoming ultimately physician to Queen Elizabeth. In due time he rose to be President of the Royal College of Physicians and to it he bequeathed his books, globes, and apparatus, which unfortunately were all destroyed in the great fire of London in 1666. Although he was thus a physician of no mean standing, the work which won him immortality had little to do with medicine, in which field, moreover, no important discovery is attributed to him. He died at Colchester, November 30, 1603, and was buried in Holy Trinity Church where a monument was erected by his brothers.
Note regarding resolution No. 4, Washington Assembly, International Association of Terrestrial Magnetism and Electricity
Authors: Fleming J. A. 
Published: February 2008

Resolution No. 4 adopted in September 1939 at the Washington Assembly of the International Union of Geodesy and Geophysics as published in the December 1939 number of the Journal (p. 478) is not complete. In its final form it is as follows:(4) Control of variometers and absolute instruments—(a) The Association reaffirms its Resolution 3 adopted at the Edinburgh Assembly of the great need of examination at regular intervals, at least every two years, of magnetic instruments, including the control of the direction of the magnetic axes of the magnets in variometers.
Annual variations of the critical frequencies of the ionized layers at Tromsö during 1939
Authors: Harang Leiv 
Published: February 2008

Regular determinations of the critical frequencies of the ionized layers, which were begun at the Auroral Observatory in April 1935,were continued during 1939. Regular observations were usually taken on six days during the week at 10h, 12h, and 14h, local time. At Tromsö, situated near the auroral zone, the conditions of the ionosphere are strongly influenced by magnetic storms and the echoes are often lacking during disturbed periods, or more‐or‐less irregular and scattered echoes appear which sometimes make a precise critical‐frequency determination difficult.
Note on scale‐value equation of the CIW induction‐variometer
Authors: McNish A. G. 
Published: February 2008

H. H. Howe of the United States Coast and Geodetic Survey has recently called attention to the fact that the equation of equilibrium for the CIW induction‐variometer [Terr. Mag., 41, 161–172 (1936)] should contain the term Z2 instead of Z. Including this modification in the equation introduces a factor of 1/2 in the theoretical scale‐value equation of the instrument, higher order terms being neglected. Fortunately this blunder occasioned no error in practice since the scale‐value has been determined empirically thus far.No important modifications of the theoretical operating‐characteristics of the instrument result from the inclusion of this correction provided the field‐changes are small as compared with the total value of vertical intensity. However, as Mr. Howe points out, serious effects may be encountered in regions where vertical intensity is extremely small, namely, close to the magnetic equator. In particular, the variometer would be unable to discriminate between positive and negative values of vertical intensity if the variations in that element pass through zero. This condition can be remedied by using an auxiliary magnet and thus increasing the value of vertical intensity so that at no time will the modified field reverse sign. If an auxiliary magnet is used no restrictions are imposed on the utility of the variometer by recognition of the correction in the equation of equilibrium.
Capetown Magnetic Observatory October to December, 1939
Authors: Ogg A. 
Published: February 2008

(Latitude 33° 57′ S., longitude 18° 28′ or 1h 13m.9 E. of Gr.)October 3–4—A storm began gradually at about 08h 55m GMT, October 3, and ended at 08h, October 4. Conditions, however, remained somewhat disturbed until October 8. Ranges: D, 28′.2; H, 159 gammas; Z, 133 gammas.
The ionosphere at Watheroo, Western Australia, January to June, 1940
Authors: Parkinson W. C. , Prior L. S. 
Published: February 2008

This report is a continuation of those already published in this Journal and gives monthly mean hourly values of the heights and penetration‐frequencies of the ionospheric regions as obtained from the automatic multifrequency ionospheric recording apparatus.Commencing with January, 1940, some desirable changes were made in the scaling of the heights of the layers. Besides the minimum virtual height, the actual heights of maximum electron‐density, uncorrected for presence of lower layers, are now scaled, using the method described by Booker and Seaton.
Solar and magnetic data, July to September, 1940, Mount Wilson Observatory
Authors: Nicholson Seth B. , Mulders Elizabeth Sternberg 
Published: February 2008

Many sunspots were observed in July, August, and September, nine of them large enough to be visible without a telescope. Nevertheless, the Earth's magnetic field showed little disturbance.When the magnetic storm of July 13 began, two large groups, Mount Wilson Nos. 6902 and 6905, were in longitude 78° west and 39° east, respectively.
Greenwich Frequency‐Statistics of Geomagnetic Disturbance
Authors: Chapman S. 
Published: February 2008

Summary—The sum of the hour‐to‐hour changes (regardless of sign) of the horizontal magnetic intensity, H, at Greenwich, from one Greenwich noon to the next, is denoted by νH; it has been determined for 21,323 days, covering a period of 62 years (1848–1913, less 1864–67). On quiet days νH is governed by the quiet‐day solar daily variation, Sq; on disturbed days the disturbance‐field D makes the main contribution to νH. Frequency‐tables are given, showing the proportion of days on which νH lies within assigned ranges, (i) for the mean of the year, (ii) for the mean of each calendar month, and (iii)—for each of three seasons—for five groups of years of different mean sunspot‐number, and (iv) for two groups of years of similar mean sunspot‐number, but taken from the ascending and descending parts of the sunspot‐cycle.Similar frequency‐tables, for the same years (plus 1914), and for the same sub‐divisions of the material, have previously been given, for 20,762 Greenwich lunar days, for RDD, the daily range of the variation of the Greenwich magnetic declination, D, after the monthly mean solar daily variation S has been removed; RDD thus depends on the D‐field, except that when this field is weak, RDD will partly measure the day‐to‐day variation of the Sq‐field.The frequency‐distributions for Vh and RDD, especially as regards their dependence on the season and the sunspot‐epoch (divisions ii, iii, and iv of the data) are rather similar. A method of correcting the νH‐statistics for the influence of Sq is devised, and applied to the annual mean frequency‐curve; the RDD‐statistics are more tentatively corrected for the influence of the Sq day‐to‐day variability on quiet days; the corrected frequency‐curves for H and D are in notably good agreement.The numerical measure νH, which except on quiet days is largely determined by the D‐field, is shown to be rather closely correlated with the international daily magnetic character‐figure C, for nearly all the months of a sample year (1901).
Radioactivity of Rocks and Ionization‐Balance of the Atmosphere
Authors: Hess Victor Francis 
Published: February 2008

It is shown that if one computes the ionization produced by gamma rays from radioactive substances in rocks and soil from figures given recently as average values for representative classes of rocks by Evans and Goodman the expected ionization turns out considerably smaller than the one actually observed by placing ionization‐vessels over land and over water.Two methods are developed theoretically which make it possible to determine simultaneously the residual ionization, the effect of cosmic rays and of the gamma rays from radioactive substances in the Earth, and to separate these components of the total ionization. Comparisons of ionizations determined by one of these methods with values computed from given figures of radioactive material in well‐defined rocks are planned.
The Ionosphere at Huancayo, Peru, July to September, 1941
Authors: Ledig P. G. , Coile R. C. , Jones M. W. 
Published: February 2008

This report is a continuation of those already published in this JOURNAL and gives monthly mean hourly values of the heights and penetration‐frequencies of the ionospheric.regions as obtained from the automatic multifrequency ionospheric recording apparatus located near Huancayo, Peru, South America, in latitude 12° 02′.7 south, longitude 75° 20′.4 west of Greenwich, which operates over a frequency‐range 0.516 to 16.0 Mc/sec. A complete discussion of these data will be made in an annual summary.Table 1 gives the monthly mean hourly values of the actual heights of maximum electron‐density (hmax), uncorrected for retardation in lower regions2, and the minimum virtual height (hmax) for both the F1‐ and F2‐Vregions, the penetration‐frequencies for the E‐, F1‐, and F2‐regions, and the lowest frequency at which echoes were observed when that frequency was greater than 0.516 Mc/sec.
The Distribution of the Ellipticity Statistic Le when the Hypothesis is False
Authors: Girshick M. A. 
Published: February 2008

In the June 1940 issue of this JOURNAL, John W. Mauchly has considered a statistic Le as a measure of ellipticity and obtained its distribution for the case of two varites under the assumption that the hypothesis of “sphericity”, is true.The object of this note is to find the distribution of Le when the hypothesis of sphericity is false. This distribution will be useful in determining the probability of accepting the hypothesis of sphericity when in fact it is false. More specifically, this distribution will permit the calculation of the probability of accepting the hypothesis that the true value λe of Le is unity when in fact it has some other value lying between zero and unity. Moreover, this distribution may be used to evaluate the size of the sample required such that the probability of accepting the hypothesis of sphericity (for any specified value of the population‐index of ellipticity λe) shall be of a given magnitude.
Huancayo Magnetic Observatory, July to September, 1941
Authors: Ledig Paul G. 
Published: February 2008

(Latitude 12° 02′.7 S., longitude 76° 20′.4 or 5h 01m.4 W. of Gr.)July 4–5—Beginning suddenly at 03h 45m GMT, July 4, with an increase of 45 gammas in H in three minutes and followed by almost twenty‐four hours of only very mild disturbance, a very severe magnetic storm was recorded on July 5. It began approximately at midnight and developed its maximum at about noon and then fell off again by the end of the day. It was marked by several peaks and bays with particularly large ones at about 12h and 13.5h. Both D and Z were also markedly effected.