bluuebunny/crossref_metadata_2025 huggingface dataset:
ATMOSPHERIC ELECTRICITY AT THE COLLEGE‐FAIRBANKS POLAR YEAR STATION
Authors: Sherman K. L.
Published: February 2008

The atmospheric‐electric program at College, Alaska, during the second International Polar Year extended from October 1, 1932, to August 31, 1933. (1) Continuous registration was made of air‐potential with a recording quadrant‐electrometer and a radioactive collector on a horizontal rod at the variation‐observatory and during most of the time also with a recording bifilar‐electrometer with radioactive collectors exposed by the stretched‐wire method for control at a standardization‐station. (2) Continuous registration was made of air‐conductivity due to both positive and negative ions, using semi‐portable apparatus in which the deflection is nearly proportional to the conductivity; in this apparatus the charge collected by the Gerdien condenser flows to earth through a resistance of about one electrostatic unit and the resulting voltage‐drop through this unit is recorded by a single‐fiber electrometer. (3) Determinations of the number of positive and negative small ions, usually made once each day, using a modified Ebert ion‐counter. (4) Determinations of the number of condensation‐nuclei, once daily from late in March through August, using an Aitken counter; during the cold weather the counter did not function satisfactorily.

These data conform with those obtained in lower latitudes at stations on land that are relatively free from variable sources of pollution. The average gradient for all complete days for the eleven‐month period is 104 volts per meter with a maximum in January and a minimum in August. Harmonic analyses of the hourly values show that a 24‐hour component exists in gradient, in substantial agreement with Mauchly's findings. All complete days of positive and negative conductivity yield average values of 179 and 131 × 10−6 electrostatic unit, respectively. The variations are approximately the inverse of those in the gradient although their product—the electrical conduction current—shows regular daily and seasonal variations. The average number of positive small ions by months varied from a minimum of 620 per cc in July to a maximum of 980 in November. The number of negative small ions varied from 520 per cc in July to 660 in November and February. From the ion‐count and the corresponding values of conductivity a mean value of 1.56 cm2 volt−1 sec−1 for the mobility of both the positive and negative small ions was found, although different mobility‐groups are indicated by frequency‐curves. The average of 112 determinations of nuclei is 3760 per cc.

The electrode‐effect appears to be quite important at this station. The ratio of positive to negative conductivity varies directly as the gradient, both in long‐period and short‐period changes. This and other features of the results are explicable on the basis of conditions as they would exist in quiet air. At times turbulence is effective in complicating the relations between the elements and so for a complete explanation of these results the effect of mixing must be considered in addition to conditions as they would exist in quiet air.
Final relative sunspot‐numbers for 1936 and monthly means of prominence‐areas for 1909‐1936
Authors: Brunner W.
Published: February 2008

Table 1 contains the final sunspot‐numbers for 1936, for the whole disc of the Sun, based on observations made at the Zürich Observatory, supplemented by series furnished by other cooperating observatories for days (indicated by asterisks) on which no observations were possible at Zürich.

Table 2 gives the yearly means of the relative numbers, R, since the last minimum 1933 and the number of days without spots.
Cheltenham Magnetic Observatory, October to December 1937
Authors: Ludy Albert K.
Published: February 2008

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

October 3–4—A storm began abruptly at 11h 19m GMT, October 3, with an increase of 12 gammas in H. It progressed mildly with short‐period oscillations until midnight of October 3. The storm then entered into a severe phase lasting about ten hours. During this time there were rapid changes of great amplitude and the extreme values of all three elements occurred about 06h. Ranges: D, 77′; H, 370 gammas; Z, 350 gammas.
Huancayo Magnetic Observatory, October to December 1937
Authors: Davies Frank T.
Published: February 2008

(Latitude 12° 02′.7 S., longitude 75° 20′.4 or 5h 01m.4 W. of Gr.)

October 3–4—A sudden commencement of relatively small amplitude occurred in all three elements at 11h 22m GMT, October 3. H decreased 2 gammas and then increased 17 gammas in two minutes. In the same interval D moved westerly 1′ and Z increased 5 gammas. The traces were very disturbed from this time until the end of October 4, a marked feature of the storm being a minimum bay in H from 00h to 12h, October 4.
Request for information about the giant pulsation on April 22, 1938
Authors: La Cour D.
Published: February 2008

During the Polar Year Dr. Thorkelsson, head of the Meteorological Service of Iceland, arranged for registrations, using a quick‐run magnetograph placed at his disposal by the International Commission for the Polar Year 1932–1933. As generally known, the records obtained from Iceland were remarkably interesting because they showed a greater frequency of giant pulsations than ever reported from other regions of the world. In view of this fact it was proposed by Professor S. Chapman and the writer at the Edinburgh Assembly of the International Association of Terrestrial Magnetism and Electricity that a thorough investigation of the giant pulsations should be carried out through international collaboration under the auspices of the Association. A committee on the subject was set up and the Association budgeted for £400 for those researches.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, April, May, and June 1938
Authors: Nicholson Seth B. , Mulders Elizabeth E. S.
Published: February 2008

Three active sunspot‐groups were all within 30° of the Sun's central meridian when the storm of April 13 began. During the very great storm of April 16 these groups were still visible, and in addition two more active groupsd had appeared at the Sun' east limb. A bright aurora was visible at Mount Wilson near midnight of April 16 (8h, GMT). The motion of the H‐element was so voilent that the maximium was off the sheet and the minimium was indistinguishable, making it impossible to measure its range.
Cheltenham Magnetic Observatory, April to June 1938
Authors: Ludy Albert K.
Published: February 2008

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

April 13–15—A moderate disturbance began at 08h 40m GMT, April 13, and continued until 02h, April 15. The storm was characterized by great short‐period activity of not very large range. Ranges: H, 188 gammas; Z, 178 gammas; D, 30′.
Remarks Dr. Chapman's note on radio fade‐outs and the associated magnetic disturbances
Authors: Appleton E. V.
Published: February 2008

This letter is by way of an addendum to the communication of Professor S. Chapman1 and the further communication by S.S. Kirby2 which it prompted.

Mr. Kirby has given a useful analysis of the steps by which the relations between radio fade‐outs and their associated solar and magnetic disturbances have been gradually elucidated during the last two and a half years by American workers, but the story seems to me to be incomplete, since no mention is made of the work of Mögel, the pioneer investigator of such matters.
Sitka Magnetic Observatory July to September, 1938
Authors: Gebhardt Robert E.
Published: February 2008

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

July 4–5—A slight magnetic disturbance began gradually at about 03h GMT, July 4, and increased slowly to maximum intensity between 12h and 14h. Thereafter the elements gradually returned to normal values at about 07h GMT, July 5. Ranges: D, 79′; H, 553 gammas; Z, 488 gammas.
A primary standard for measuring the Earth's magnetic vector i—theory
Authors: Johnson E. A.
Published: February 2008

The theory of a new primary standard for measuring any component of the Earth's magnetic field is developed. The magnetometer consists of a Helmholtz‐Gaugain coil which provides a standard field opposed to that component of the Earth's magnetic field which is to be measured, and a rotating coil used as a null detector. The voltage generated in the rotating coil is detected by an alternating‐current amplifier. The constant of the Helmholtz‐Gaugain coil is computed from the formulas developed by C. Snow from the mutual inductance between two concentric cylinders. Corrections are computed for the fact that the Helmholtz‐Gaugain coils are helices, for the axial components of current, for the effect of the lead‐in wires, and for non‐uniformities in winding. The finite size of the detector is not a limitation on the accuracy since it is taken into account in the computation. Consequently, the accuracy of the coil‐constant of the new standard depends only upon constructional accuracy. Inhomogeneity in the field of the Helmholtz‐Gaugain coil necessitates the use of small correction‐terms to the voltage of fundamental frequency generated in the detector and produces odd harmonics of the fundamental frequency in the detector. The errors in orientating the Helmholtz‐Gaugain coil are also examined. The limiting sensitivity of the detector is calculated from the thermal agitation of electricty in the coil of the detector.
Harmonic analysis of diurnal variations for single days
Authors: Bartels J.
Published: February 2008

The forthcoming volume of results at the Watheroo and Huancayo magnetic observatories will contain an extensive table of about 40,000 harmonic coefficients for the diurnal variations in the horizontal magnetic intensity H at Huancayo Magnetic Observatory (Peru) for every individual day of the years 1922 to 1936. This collection of coefficients, a new feature in observatory compilations, represents an advanced stage of reduction of the original magnetic records beyond the usual hourly means, and will be used as material for discussions on the variability of the solar and lunar diurnal variations. H at Huancayo has been selected for the first table of this kind because of the unusual features of its large diurnal variation. A new scheme for numerical harmonic analysis of diurnal variations for this mass‐reduction had to be developed yielding, in the most economical way, the coefficients of the periods 24, 12, 8, and 6 hours. This scheme and allied topics are described in detail in this paper, because they may be useful in similar geophysical work. The scheme itself may be found in section 8.
Midday F2‐region critical frequencies for Deal, New Jersey
Authors: Goodall W. M.
Published: February 2008

Midday F2‐region critical frequencies as obtained at Deal, New Jersey, are given in Table 1. The values are given in mc/sec and are for the O‐component. The period covered by these readings is from June 1938 to April 1939. Most of the readings were obtained near noon and all, except those marked with an asterisk, were obtained between 11h 30m and 13h 30m EST.
Sitka Magnetic Observatory January to March, 1939
Authors: Gebhardt Robert E.
Published: February 2008

February 5–7—A moderate magnetic storm began at 19h 49m GMT, February 5, with a sudden decrease of 7′.0 in east declination during the first minute. During the next five minutes there was an increase of 21′.0 in east declination. Changes occurred also in the other components. The traces remained relatively quiet until 10h, February 6, when the activity increased gradually until 12h.
Tucson Magnetic Observatory January to March, 1939
Authors: Hershberger John
Published: February 2008

February 5–7—A storm of very moderate intensity began sharply at 19h 50 m GMT, February 5, and lasted until about 14h, February 7. The beginning was marked by a sudden drop of 6 gammas in H, followed immediately by an increase of 32 gammas. The average value of H gradually decreased until it was about 100 gammas below normal at 03h, February 7. Range in H was 126 gammas.
Auroral work in southern Norway in the year 1938
Authors: Störmer Carl
Published: February 2008

(1) Introduction—Since 1911 I have had in operation a series of permanent stations in southern Norway to photograph the polar aurora and to measure its height by simultaneous exposures from different stations connected by telephone‐lines. A report of the work from 1911 to 1922 has been issued but only a small part of the extensive material obtained since 1922 has as yet been published.

In recent years I have examined this material which consists of more than 25,000 negatives and have prepared an auroral log for the years 1923 to 1937. In this log, which is perhaps too extended for publication, each picture has been examined carefully and the following data have been noted: Number of exposure, station, time, exposure, auroral form, stars, number of points measured, and general remarks. This log contains 11,338 successful pictures and among these about 6,484 sets of simultaneous photographs for determination of height. Of these 6,484 sets only a few have been measured and calculated, but these have furnished 4,683 heights of which only selected ones have been published.
Final relative sunspot‐numbers for 1938 and monthly means of prominence‐areas for 1931–1938
Authors: Brunner W.
Published: February 2008

Table 1 contains the final sunspot‐numbers for 1938, 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.
An unusual magnetic disturbance
Authors: Howe H. Herbert
Published: February 2008

A rather unusual magnetic disturbance occurred on June 26, 1939. Figure 1 is reduced from actual tracings of the curves registered at the five magnetic observatories of the United States Coast and Geodetic Survey during the interval 20h to 22h GMT, June 26, 1939. Unfortunately, there was a slight artificial disturbance at Tucson just before the beginning of the natural disturbance, caused by a truck used in connection with the construction of the new variation‐building.

All five observatories show sudden commencements at about 20h 20m GMT, marked chiefly in four cases by an increase in horizontal intensity. After about an hour, the curves returned to normal, in two abrupt steps separated by about seven minutes. The duration of this disturbance was about the same as that of a bay, but it is different from an ordinary bay because of the abrupt increase and decrease.
Cheltenham Magnetic Observatory April to June, 1939
Authors: Ludy Albert K.
Published: February 2008

April 4–5—A mild disturbance of short duration took place between 18h 35m GMT, April 4, and 8h, April 5. Ranges: D, 23″; H, 78 gammas; Z, 43 gammas.

April 16–22—An abrupt commencement of a storm occurred at 21h 29m GMT, April 16. In the first few hours the storm was very moderate but at 0lh 58m, April 17, it suddenly became very severe. The greatest ranges of the storm occurred between 06h and 08h, April 17. During this interval the range of H was 664 gammas. The interval between 08h and 20h, April 17, was marked by great short‐period activity of moderate range in all three elements. From 20h to 22h the ranges again became relatively large. The main phase of the storm ended at 21h 35m, April 17, but the field continued to be moderately disturbed until 03h, April 22. Ranges: D, 47″; H, 664 gammas; Z, 515 gammas.
Auroras and sunspots
Authors: Clayton H. Helm
Published: February 2008

In the hope of advancing our knowledge of the relationship between sunspots and auroral displays the author has undertaken a study of the 55‐year record of auroras observed at the Blue Hill Meteorological Observatory near Boston, Massachusetts. These data cover the period from from 1885 to 1939 and were kindly furnished by Dr. C. F. Brooks, the present director. In handling these data all doubtful cases were eliminated. Also, one date was assigned to all cases where the aurora was observed until after midnight.
On the existence of a biannual component in the F2‐layer ionization
Authors: Eckersley T. L.
Published: February 2008

§1. Introduction—The problem of the mode of ionization of the ionosphere is of great physical interest. It is known that the ionosphere consists of three well‐defined regions, the E‐, F1‐, and F2‐layers, and that whereas the main features of the mechanism of the ionization of the E‐ and F1‐layers are known, there are many problems associated with the mode of ionization of the F2‐layer which remain as yet unsolved.

From the general nature of the diurnaI variations in the ionic density in the E‐ and F1‐layers, as deduced from critical escape‐frequencies measured at vertical incidence, it is obvious that the ionization is at least in part related to the Sun's radiation. It is now generally accepted that the E‐ and F1‐layers are mainly ionized by ultraviolet radiation from the Sun. There is some abnormal sporadic ionization which does not appear to be of solar origin, for instance, the ionization which is reponsible for the reflection of 7‐ to 10‐meter waves to distances of 1000 km or so, and which does not apparently vary with the sunspot‐cycle, and the sporadic ionization which persists throughout the long polar winter night. But the main E‐ and F1‐ionizations have been shown to obey the law deduced theoretically by Chapman for a region of the atmosphere ionized by a monochromatic radiation from the Sun, namely that the midday critical frequency should vary as cos¼θ, where θ is the zenithal angle of the Sun. The wave‐lengths of the ionizing radiations and the precise molecular or atomic reactions involved are as yet unknown, as it would need a complete spectroscopic analysis in the ultraviolet region of O, N, O2, and N2 in their various excited and ionized states to determine them. Eclipse experiments on the accompanying changes of density during the optical eclipse also confirm the idea that the ionization of the E‐ and F1‐layers is mainly due to ultraviolet light from the Sun.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory October to December, 1939
Authors: Nicholson Seth B. , Mulders Elizabeth Sternberg
Published: February 2008

The disturbance of October 3 to 4 was not like that of a typical magnetic storm, although the range in H was large. The largest spot‐group on the Sun was Mount Wilson No. 6623, which crossed the central meridian on October 4.2, 14° north of the center of the disk.

The magnetic storm of October 13 to 15 was probably associated with the active group No. 6633, which crossed the central meridian on October 12.3, 12° south of the center of the disk.
The magnetic observatory at Toolangi
Authors: Baldwin J. M.
Published: February 2008

The magnetic observatory at Toolangi is now in full operation again, the recording having started in January 1940. Careful consideration was given to the question of underground construction and its adoption resulted from the decision that it was better to run the risk of dampness than the local risk of loss through forest fire.

The new building is of concrete with three feet of earth over the roof. The building is entirely covered with waterproof coating outside and below which there is adequate provision for efficient drainage, all drainage water being discharged some distance down the hillside. All material used in the building was tested and is non‐magnetic.
Sitka Magnetic Observatory January to March, 1940
Authors: Gebhardt Robert E.
Published: February 2008

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

January 3–4—A small storm began abruptly at 14h 41m GMT, January 3, with a sharp decrease in the horizontal intensity. The field was very disturbed from 15h to 17h. Thereafter the trace began a gradual return to normal values. The disturbance ended about 24h, January 4. At times during the stormiest period the spots moved so rapidly, it was not possible to separate the three components. Ranges: D, 170′; H, 1172 gammas; Z, 1135 gammas.
Cheltenham Magnetic Observatory January to March, 1940
Authors: Ludy Albert K.
Published: February 2008

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

January 3–4—A mild storm, which was very active during the first two hours, began at 14h 41m GMT, January 3, when H decreased 158 gammas in 23 minutes. The storm ended at 05h, January 4. Ranges: D, 26′; H, 265 gammas; Z, 54 gammas.
Directional and Diurnal Characteristics of Auroras at Some Places in Canada
Authors: Currie B. W. , Jones C. K.
Published: February 2008

Introduction—Observations of auroras at almost all places on the Earth's surface indicate that displays extend along some predominating horizontal direction and that the maximum diurnal activity occurs at a particular time, both of which are typical of the locality in question. Vegard [see 1 of “References” at end of paper] has shown that the average directions of arcs and bands at a number of the places in the Northern Hemisphere are systematized and assume added significance if they are referred to the geomagnetic rather than to the astronomical meridians. In most cases the average angle between the westward‐directed end of the arcs and bands observed at a particular place and the geomagnetic meridian through the place is several degrees greater than 90°. Vegard [1, 2] has examined also the diurnal frequency of auroras for a number of northern stations, and has expressed the opinion that within the limit of error the principal maximum occurs at about one hour before geomagnetic midnight. On the other hand Hulburt [3] from the data of many arctic and antarctic expeditions suggests that the diurnal course of an auroral display is dependent upon the meteorology of the upper atmosphere at a station.
A New Laboratory for Cosmic‐Terrestrial Research
Authors: Stetson Harlan True
Published: February 2008

An initial grant from the American Philosophical Society1 in 1935 for investigations in cosmic‐terrestrial relationships together with additional funds from anonymous sources has made possible the inauguration of a program of needed observations in geophysical phenomena that has recently resulted in the establishment of a new laboratory for cosmic‐terrestrial research at Needham, Massachusetts.

The site of the new Laboratory (Fig. 1) was selected after about a year of careful study of the environs of Boston from the point of view of suitability as to appropriate conditions for atmospheric‐electric observations, together with accessibility to the Massachusetts Institute of Technology with which the work at the Laboratory is associated.
Internationale Erdmagnetische Charakterzahlen im Jahre 1940
Authors: Bartels Von J.
Published: February 2008

Zur Reproduktion werden vorgeschlagan:

**1940—März 24 u. 29; September 26, 15 Uhr bis September 27, 9 Uhr.

*1940—Januar 3; April 2 u. 25; Juni 25; Juli 13; August 3; Oktober 7 u. 8; November 25.

Zahl der Observatorien, deren Charakter‐Schätzungen verwendet werden konnten: 53 im Januar und Februar; 54 im März; 56 im April, Mai, Juni; 58 im Juli; 57 im August bis November; 58 im Dezember.
In Memoriam Doctor Garmt van Dijk, 1877–1940
Authors: Cannegieter H. G.
Published: February 2008

In the last days of the year 1940 the Netherlands Meteorological Institute has suffered a sad bereavement in the death of the member of its scientific staff, Dr. G. van Dijk. After a short illness he died suddenly and quite unexpectedly in the night of December 19, 1940, at the age of 63 years. Thirty‐four years of a busy life had been devoted to the organization and direction of the Magnetic and Seismological Section of the De Bilt Meteorological Institute.

Van Dijk was born June 22, 1877. He studied at the University of Groningen and was given the degree of Doctor of Physics March 4, 1905. On February 1, 1907, he was appointed by the Institute at De Bilt as Assistant Director in charge of the Section of Magnetism and Seismology. After his plans new pavilions were constructed for the magnetic and seismological instruments. The seismological pavilion was finished in 1911 and the magnetic pavilion in 1913.
Erdmagnetisch ruhige und gestörte Tage im zweiten Halbjahr 1940
Authors: Bartels J.
Published: February 2008

An die Herren Direktoren der erdmagnetischen Observatorien:

Dr. G. van Dijk ist am 19. Dezember 1940 gestorben; H. G. Cannegeiter hat ihm in Hemel en Dampkring [39, 1–3 (1941)] einen Nachruf gewidmet.
Sitka Magnetic Observatory, April to June, 1941
Authors: Gebhardt Robert E.
Published: February 2008

April 19—A short period of increased activity began gradually at 05h GMT, April 19. Maximum storminess occurred between 08h and 09h with decreased values of all elements. After 09h conditions slowly returned to normal.

April 24–25—A small magnetic storm began abruptly at 08h 39m GMT, April 24. The activity increased gradually until about 15h and then began a gradual decrease. The disturbance consisted of large bays. After 15h a short‐period vibration was superimposed on the long‐period motion. After 08h, April 25, there was a slow return to normal. Ranges : D, 126′; H, 884 gammas; Z, 804 gammas.
Notes on Isomagnetic Charts: VIII—The Mutual Consistency of the Declination and Horizontal‐Intensity Isoporic Charts
Authors: Chapman Sydney
Published: February 2008

Summary—The rate of change of the vertical component of the earth‐air electric current‐density i is expressed in terms of the surface‐gradients of the rates of change of the horizontal magnetic elements X and Y or D and H: the formulas enable (di/dt) to be calculated from the distribution of the isomagnetic and isoporic lines for these elements. It is shown that if the directions and spacing of the isoporic lines are seriously uncertain, (di/dt) should be found, from the magnetic charts, to have a value of order five milliamperes per km2 per year; this is confirmed by calculations based on the Admiralty charts for 1922, the Fisk isoporic charts for the same epoch, and the Swedish magnetic surveys of epochs 1929.5 and 1936.5. The actual value of (di/dt) is inferred, from atmospheric‐electric observations, to be at most 10−4, so that these much larger calculated values of (di/dt) indicate errors in the isoporic charts.
Note on the Effect on Cosmic‐Ray Intensity of the Magnetic Storm of March 1, 1942
Authors: Lange Isabelle , Forbush S. E.
Published: February 2008

Figure 1 shows the decrease in cosmic‐ray intensity (corrected for barometric pressure) recorded at Cheltenham (Maryland) and Huancayo (Peru) during the magnetic storm of March 1, 1942, which began with an abrupt sudden commencement at 02h 30m (75° west meridian mean time). It will be noted that the decrease in cosmic‐ray intensity occurred immediately after the sudden commencement and was followed by large changes in cosmic‐ray intensity.

The change of cosmic‐ray intensity in Figure 1 is remarkably similar to that recorded during the five days following the sudden commencement of the magnetic storm of January 16, 1938 [see Fig. 2 of paper by S. E. Forbush, Terr. Mag., 43, 203–218 (1938)]. These curves are much like those for the average storm‐time variations in magnetic horizontal intensity [see paper by S. Chapman, Terr. Mag., 40, 349–370 (1935) and also E. H. Vestine, Terr. Mag., 47, 97–113 (1942)], which is strong indication that the changes in cosmic‐ray intensity are due to the magnetic field of the storm.
William John Peters, 1863–1942
Authors: Harradon H. D.
Published: February 2008

During the first two decades of the existence of the Department of Terrestrial Magnetism of the Carnegie Institution of Washington, emphasis was placed on the acquisition of observational data in order that a firm foundation for future theoretical studies of the Earth's magnetism might be laid. To this end numerous expeditions were sent to all parts of the world to determine the magnetic elements at stations on land and a large amount of observational material was thus accumulated. At the same time the cruises of the Galilee and Carnegie were furnishing the magnetic data at sea to supplement the results on land. Aside from important theoretical considerations, the contribution of these data over the oceans to the correction of errors in existing magnetic charts was of inestimable value to navigation as was attested by the keen interest manifested by the maritime nations to whose hydrographic bureaus the results were promptly supplied.
Study of cosmic rays between New York and Chile
Authors: Berry Edward B. , Hess Victor F.
Published: February 2008

A Compton Model‐C cosmic‐ray meter aboard the S.S. Santa Ana measured cosmic‐ray intensities between New York and Valparaiso from September, 1940, to February, 1942. The hourly deflections of the electrometer‐needle, recorded photographically, were measured and the computed cosmic‐ray intensities corrected for barometric pressure with a coefficient K = −1.74 per cent per cm mercury. After reduction to 30 inches of mercury, they were grouped into 2°.5 intervals of geomagnetic latitude with the corresponding mean temperatures and temperature‐coefficients for the various latitudes determined. The variation of intensity of ionization with geomagnetic latitude was then plotted, showing a latitude‐effect of 8.3 per cent. A longitude‐effect of 1.5 per cent between geographic longitudes 75° west and 145° west was also found.

The curve of temperature‐coefficients was found to be symmetrical about 23° north geomagnetic latitude in contrast to a similar curve of P. S. Gill for the Pacific, which is symmetrical about the geomagnetic equator.

Variations of cosmic radiation during the magnetic storm of March 1, 1942, are plotted and show the same characteristics and order of magnitude as those reported by other observers.
Sitka Magnetic Observatory, January to March, 1943
Authors: Pinckney Harold W.
Published: February 2008

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

January 20–21—Commencing with an increasing bay in D at 21h 05m GMT, January 20, a moderate disturbance continued through 07h, January 21. Ranges: D, 71′; H, 565 gammas; Z, 577 gammas.
Magnetic Observatory, Hermanus, January to March, 1943
Authors: Ogg A.
Published: February 2008

(Latitude 34° 25′.2 S., longitude 19° 13′.5 or 1h 16m.9 E. of Gr.)

January 1–5—There was a small sudden‐commencement disturbance at 15h 30m GMT, January 1. At the beginning of the disturbances, which continued until 21h, January 5, the ranges were very small, but after 08h 30m, January 4, the magnetic activity increased. The greatest .K‐index was 5 for the periods 12h to 15h and 18h to 21h, January 4, and 09h to 15h and 18h to 21h, January 5. There were micropulsations on all traces from 01h 45m to 02h 00m, January 3.
CHELTENHAM MAGNETIC OBSERVATORY JULY TO SEPTEMBER, 1943
Authors: Hershbebger John
Published: February 2008

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

July 4‐6—A moderate disturbance yielding two K‐indices of 6 began at about 12h GMT, July 4, and lasted approximately forty‐eight hours. Intermittent minor activity continued for more than a week.
Cheltenham Magnetic Observatory, October to December, 1943
Authors: Hershberger John
Published: February 2008

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

October 24–31—A period of minor disturbance began in the fourth three‐hour period of October 24 (GMT), and continued to the end of the month. Four K‐indices of 6, and sixteen of 5, were scattered throughout the period.
Tucson Magnetic Observatory, October to December, 1943
Authors: Wilson R. M.
Published: February 2008

Latitude 32° 14′.8 N., longitude 110° 50′.1 or 7h 23m.3 W. of Gr.]

September 27–October 4—The September part of this storm was described in the last report. The moderate storm or series of storms that began at about 00h GMT, September 27, continued until about 11h, October 4. Moderately severe storm‐conditions prevailed from 00h, September 30, to 05h, October 1, also from 23h, October 1, to 03h, October 2, and from 23h, October 2; to 11h, October 3. The other periods of the storm were characterized by irregular variations of D and H without unusually prominent maxima and minima. Ranges: D, 22′,5; H, 166 gammas; Z, 36 gammas.
Watheroo Magnetic Observatory, January to March, 1944
Authors: Parkinson W. C.
Published: February 2008

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

February 7–8—This small disturbance began at about 05h GMT, February 7. There was no sudden commencement, but the traces gradually became more disturbed, reaching their greatest activity at 12h 50m when there were large peaks in D and Z and a considerable bay in H until 13h 26m. During this interval the range in H was 103 gammas, in D 11′.5, and in Z 99 gammas. There was a smaller series of peaks and bays between 15h and 16h 30m; however apart from this feature the disturbance gradually subsided until normal conditions again prevailed at 24h February 8. Ranges: D, 20′.0; H, 113 gammas; Z, 147 gammas.
Hermanus Magnetic Observatory, October to December, 1943
Authors: Ogg A.
Published: February 2008

(Latitude 34° 25′.2 S., longitude 19° 13′.5 or 1h 16m.9 E. of Gr.)

October 1–5—The disturbances which began at midday of Greenwich date September 26 continued until midday October 5. During the period from October 1 to October 5 the maximum K‐index was 5 for each of the three‐hour periods 12h–15h, October 1, and 12h–5h and 18h–21h, October 2.
C. Coleridge Farr, 1866–1943
Authors: Macleod D. B.
Published: February 2008

Dr. C. Coleridge Farr, F.R.S., for 30 years a member of the Canterbury Branch of the Royal Society of New Zealand, and an original Fellow of the Society, died on January 27, 1943.

Farr was born in Adelaide on May 22,1866. His father, the Venerable Archdeacon Farr, LL.D. (Cantab.), was, at the time, headmaster of St. Peter's College, the leading Boys' College in Adelaide. After receiving his early education at his father's school, Dr. Farr proceeded to Adelaide University. It was his good fortune that Sir William Bragg was Professor of Mathematics and Physics. Farr remained a lifelong friend of Sir William and his family, and he was fond of recalling that he had often nursed on his knee Professor W. H. Bragg, at present the Cavendish Professor of Physics at Cambridge.
Sitka Magnetic Observatory, July to September, 1944
Authors: Pinckney Harold W.
Published: February 2008

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

August 2–3—Climaxing a three‐month period of unusual calm a fairly severe storm began gradually about 21h GMT, August 2, accelerated at 24h, and diminished sharply in intensity after 11h, August 3. A maximum positive departure from normal of 625 gammas occurred in horizontal intensity at 03h 32m and K‐indices of 7 were recorded for the first three periods of August 3. Most of the action on D took the form of rather long‐period oscillations.
Five International Quiet and Disturbed Days for July to September, 1944
Authors: Johnston H. F.
Published: February 2008

Reports of geomagnetic activity for the third quarter of 1944 have been received from a sufficient number of magnetic observatories so that the international quiet and disturbed days may be selected in accordance with the method outlined on pages 219–227 in the December 1943 issue of this JOURNAL. The selection is based on the reports of magnetic character on a scale of 0, 1, and 2 from 30 observatories in July, 20 in August, and 17 in September, and of K‐indices from 23 in July and 18 in August and September.
Huancayo Magnetic Observatory, January to March, 1945
Authors: Jones Mark Wallon
Published: February 2008

(Latitude 12° 02′.7 S., longitude 75° 20′.4 or 5h 01m.4 W. of Gr.)

January 15— There was a short disturbance characterized by a sharp beginning at 18h 00m GMT, January 15. There was a high peak in H at 18h 07m, which was followed by numerous peaks and bays with a deep bay at 18h 47m. The disturbance was over by 19h 40m, D and Z showing only mild variations. The K‐index of 6 covered the variation. Range: H, 307 gammas.
Tucson Magnetic Observatory April to June, 1945
Authors: Nelson J. H.
Published: February 2008

(Latitude 32° 14′.8 N., longitude 110° 50′.1 or 7h 23m.3 W. of Gr.)

April 1–2—A moderate magnetic storm of only twenty‐four hours' duration began at 05h GMT, April 1. There was marked activity of fairly short period during the first ten hours, which were followed by a period of mild disturbance until the end of the storm. Ranges: D, 15′; H, 110 gammas.
Hermanus Magnetic Observatory April to June, 1945
Authors: Ogg A.
Published: February 2008

(Latitude 34° 25′.2 S., longitude 19° 13′.5 or 1h 16m.9 E. of Gr.)

April 1—A small sudden‐commencement storm began at 04h 59m GMT, April 1, and continued for about twenty‐four hours. The range of H was 136 gammas and the maximum K‐index was 5, period 15h‐18h.
Annual variation of the values at noon of the critical frequencies of the ionized layers at Tromsö during 1940, 1941, 1942, 1943, and 1944
Authors: Harang Leiv
Published: February 2008

In previous notes the monthly mean values of the critical frequencies of the ionized layers have been given beginning with 1935. In the following the mean monthly values of the critical frequencies determined at local noon will be given. As the station Tromsö is situated near the auroral zone, the conditions of the ionosphere are strongly influenced by the frequent geomagnetic storms, and the echoes are often lacking during disturbed periods due to increased absorption, or more or less irregular echoes appear, which sometimes make a precise critical‐frequency determination difficult.

Because of the war it has not been possible to take the observations so regularly as previously, and for some months the number of daily observations are not sufficient to give reliable monthly means. In 1940 the observations had to be stopped on April 10, as the antennas had to be removed due to bombing in the vicinity. The observations could not be resumed until July, 1940. In December, 1944, the antennas had again to be removed.
Geophysical Observatory Sodankylä
Authors: Keränen J.
Published: February 2008

The scientific work of the Geophysical Observatory at Sodankylä, which had begun on January 1, 1914, continued without interruption until the final stages of the second world war, despite the fact that military operations sometimes came uncomfortably close to the Observatory, particularly during the winter war 1939–40. In September, 1944, however, it became necessary to leave the Observatory when the entire population of Finnish Lapland was evacuated, and one month later the German military forces razed the Observatory to the ground prior to their retreat from northern Finland. Nothing but ruins was left of a single one of the ten buildings composing the Observatory and the greater part of the recording instruments and the whole library were destroyed. Fortunately, the photographic records, the unpublished and half‐finished manuscripts, the greater portion of the absolute instruments, and one magnetic recording set were brought to safety before the German occupation.
Noise during radio fade‐outs
Authors: Ferrell Oliver Perry
Published: February 2008

The interesting communication from J. M. Watts [Terr. Mag., 51, 122–125 (1946)] regarding a form of solar hiss or noise during radio wave, fade‐outs has been brought to my attention. In preparing a bibliography of the effects of radio‐wave propagation above 30.0 Mc/sec, I have found the following previous references of this noise which may prove of interest or value to other investigators.

Some casual mention is made of the noise accompanying radio fade‐outs by Dr. J. H. Dellinger who coordinated many of the random radio fade‐out observations. D. Arakawa [Abnormal attenuation in short‐wave propagation, Reports of Radio Research in Japan 6, No. 1 (1936)] appears to have made the first concise investigations and mentions the noise on the point‐to‐point communication circuits from Manila to Tokyo during radio fadeouts. It also seems worthy of mention that a lone British radio amateur observed this type of hiss during fade‐outs between 40.0 and 60.0 Mc/sec, in 1937.
Five international quiet and disturbed days for October to December, 1945
Authors: Scott W. E.
Published: February 2008

Reports of geomagnetic activity for the last quarter of 1945 have been received from a sufficient number of observatories so that the International quiet and disturbed days can be selected in accordance with the method outlined on pages 219–227 in the December, 1943, issue of this Journal. The selection is based on the reports of magnetic character on a scale of 0, 1, and 2 from 37 observatories and of K‐indices from 28 observatories.
Tucson Magnetic Observatory April to June, 1946
Authors: Nelson James H.
Published: February 2008

(Latitude 32° 14′.8 N., longiude 110° 50′.1 or 7h 23m.3 W. of Gr.)

April 14–15—A moderate disturbance began about the middle of the Greenwich day April 14, with small activity of fairly short period. Activity increased slightly about 01h GMT, April 15. The period of disturbance ended about 20h, April 15. Ranges: D, 15′; H, 94 gammas.
Summary of the year's work, to June 30, 1946, Department of Terrestrial Magnetism, Carnegie Institution of Washington
Authors: Fleming J. A.
Published: February 2008

The surrender of Germany in 1945 and of Japan early in the report‐year (July 1, 1945, to June 30, 1946) brought to an end the long struggle since 1939, which has diverted almost all scientific investigators and organizations into paths bearing on the grim business of war. This Department's personnel and program, as briefly summarized below, have assisted the Government of the United States by taking over the development of many problems whose solutions have involved fields of its research and the worldwide data it has acquired since 1904. Happily most of the developments for defense have involved the results not only of old lines of approach to theoretical and experimental studies, but also of new lines in the Department's fields of research. Naturally the work required to complete contractural commitments—some undertaken only a few months before cessation of hostilities—with various war agencies, although in large measure done before June 30, 1946, will make some demands on administrative resources and scientific personnel of the Department for the remaining months of the calendar year 1946.
Five International quiet and disturbed days for April to June, 1946
Authors: Scott W. E.
Published: February 2008

Reports of geomagnetic activity for the second quarter of 1946 have been received from a sufficient number of observatories so that the International quiet and disturbed days can be selected in accordance with the method outlined on pages 219–227 in the December, 1943, issue of this Journal. The selection is based on the reports of magnetic character on a scale of 0, 1, and 2 from 37 observatories and of K‐indices from 29 observatories.
Suggestions for reprinting articles of historic interest in geomagnetism
Authors: Mitchell A. Crichton
Published: February 2008

I have two suggestions for the continuation of reprints of articles of historic interest in geomagnetism in the Journal, as follows:

(1) Fr. Timoteo Bertelli did a great deal to clear up a number of obscure points in the history of terrestrial magnetism. Whatever he undertook, he carried out thoroughly, and, for the greater part, accurately. He made one or two mistakes—but we all do that. But I think his work, although widely mentioned, has not been properly appreciated, and I would suggest that the Journal publish some account of his writings of which I do not know of a complete list.
Henry Fawsit Skey, 1877–1947
Authors: Baird H. F.
Published: February 2008

0n January 16, 1947, at his home in Christchurch, New Zealand, Henry Fawsit Skey, a former Director of the Christchurch Magnetic Observatory, died suddenly from a heart attack which overcame him just before noon whilst he was having a cup of tea with his wife.

He was born in April, 1877, at Dunedin, New Zealand, where he attended the Otago Boys' High School, and later the Otago University. There he gained a senior scholarship, and next year graduated with honors in Physics.
Sitka Magnetic Observatory January to March, 1947
Authors: Campbell Joel B.
Published: February 2008

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

January 2–6—An extended period of moderately disturbed conditions was recorded during the first few days of January. The disturbance began gradually at about 08h 30m GMT, January 2, and continued until about 16h 00m, January 6. Activity consisted chiefly of variations of rather large amplitude and long period forming small bays throughout the storm. One K‐index of 6 was recorded near the beginning of the disturbance and four K‐indices of 5 were recorded just before the end.
Report of temporary Sub‐Commission on liquidation of agenda of the International Commission for the Polar Year 1932–1933
Authors: Fleming J. A. , Keränen J. , Stagg J. M. , Thomson A.
Published: February 2008

Introduction

The realization of the Second Polar Year in 1932–1933, as a truly international project, is a monument to the enthusiasm and indefatigability of the late Dr. D. la Cour and to the support generously provided by the Danish Meteorological Institute. From it have already resulted many valuable contributions to knowledge of polar geophysics in numerous publications and in completed or partially completed manuscripts. There remains much material not yet fully compiled or discussed. It would be peculiarly unfortunate if the potentialities for increased understanding of polar geophysics resulting from this great project, in which so many nations and men took selfless part at great cost, were not fully analysed and published. The past ten years have demonstrated that progress and future human welfare depend upon more solid knowledge of natural phenomena in the Arctic and Antarctic.
Alibag Magnetic Observatory July to September, 1947
Authors: Rao M. P.
Published: February 2008

(Latitude 18° 38′.3 N., longitude 72° 52′.3 or 4h 51m.5 E. of Gr.)

July 17–18—A storm of great intensity commenced suddenly at 17h 48m GMT, July 17, with an unusually large increase of 109 γ in H, a decrease of 27 γ in Z, and an increase of 1′.3 in westerly declination. After a period of intense activity lasting for about three hours, all three elements became fairly steady until about 03h 15m, July 18, when rapid fluctuations began to be recorded continuously until about 11h 15m. A crochet of the type usually associated with a solar flare was also recorded on all the magnetograms at 10h 37m, July 17. The storm ended at about 20h, July 18, giving K‐indices one each of 8, 7, and 6 and two of 5. Ranges: D, 8′.5; H, 298 γ; Z, 62 γ.
K‐indices and sudden commencements, January to March, 1948, at Abinger
Authors: Jones H. Spencer
Published: February 2008

I enclose the list of K‐indices of geomagnetic activity at Abinger for January to March, 1948, in Table 1.
Geomagnetic and geoelectric literature in two new German periodicals
Authors: Macht Hans G.
Published: February 2008

(a) Zeitschrift für Meteorologie, Jahrgang 1, Berlin 1946/47 (Deutscher Zentralverlag G.m.b.H.)—The well‐known Meteorologische Zeitschrift ceased in 1944 on account of war‐emergencies, with the July issue (No. 7) of Volume 61 (1944) as the last. In October, 1946, a new meteorological journal was founded under the name Zeitschrift für Meteorologie, also edited by Prof. Dr. R. Suring, Director of the Potsdam Meteorologisches Zentral‐observatorium. This periodical continues the task of the former Meteorologische Zeitschrift in the publication of papers and notes dealing as well with meteorology as with geophysical topics included with geomagnetism. Short reports concerning sunspot‐numbers, magnetic storms, and polar lights are also given.