bluuebunny/crossref_metadata_2025_split huggingface dataset:
Total and uncharged nuclei at Washington, D.C.
Authors: Sherman K. L. 
Published: February 2008

Observations of the concentration of both uncharged and total condensation‐nuclei were made at different times and places near Washington, using an Aitken nuclei‐counter in conjunction with a cylindrical, electrical condenser through which air was drawn at a desired rate by a spring‐driven turbine. The ratio (S) of the concentration of uncharged to that of all nuclei, serves as a measure of the relative magnitude of the coefficients of combination and those of attachment between small ions and charged and uncharged nuclei, respectively, provided the assumptions usually made in this connection are valid. Diverse values of S have been found heretofore when these were determined from the same data but by different methods. It is shown in the theory of least squares that the method of determining the best estimate of a quantity of this character depends upon the manner in which weights should be assigned to the data. It is shown here that the weight assigned to the observed number of particles falling on a square of the counter, should vary inversely as that number. The proper method of determining the best estimate of S, when weights are assigned in this manner, and also two other simpler methods were applied to these data. The surprisingly small differences in the three results, indicates these data are homogeneous.From 620 individual samples of both uncharged and total nuclei, S was found to be 0.75 with a standard error of 0.02. This value of S is distinctly greater than that reported for other places but it is in close agreement with values previously determined at Washington with other equipment. No significant evidence of a dependence of S, upon time, upon place, or upon concentration of nuclei, such as some observers report, is provided by these data. An examination of the standard deviation of S for a single sample indicates that the variations which do appear are no greater than those which are to be expected from random errors. Systematic errors in all measurements of this sort may arise from the adsorption of nuclei on the walls of the apparatus. The differences in the values of S found at the different places may in part be attributed to this source. Four hundred individual samples taken, both before and after the air passed through the condenser with no field applied, indicate that 0.85 of the nuclei which enter this condenser get through. The procedure followed here was such that errors in the calculated value of S from this source are eliminated provided charged and uncharged nuclei are adsorbed with equal facility.
Tucson Magnetic Observatory January to March, 1940
Authors: Hershberger John 
Published: February 2008

(Latitude 32° 14′.8 N., longitude 110° 50′.1 or 7h 23m.3 W. of Gr.)January 3—A moderately severe but short‐lived storm began at 14h 40m GMT, January 3, and ended about three hours later. The principal feature was a drop in H of 198 gammas, followed by a return to its normal value in an hour and a half. D fluctuated through a range of 12′ and Z was slightly disturbed.
General meteorological aspects of thunderstorm electricity
Authors: Byers Horace R. 
Published: February 2008

Physicists studying the details of lightning‐discharges have in recent years progressed quite satisfactorily in analyzing the observed electrical phenomena. On the meteorological side, where the mechanism of the thunderstorm as a cloud in relation to the development of the strong potential‐gradients which have been observed is to be investigated, the progress is, by comparison, relatively slight. It is the purpose of this paper to discuss some of these meteorological factors, particularly to bring them to the attention of the physicists as well as of the meteorologists who must work side by side in this field.Measurements have shown that the potential‐gradient, at least near the ground, is usually positive in fine weather or in the absence of thunderstorms and that this gradient is generally greatest at those times when the air is thermodynamically in a stable state of equilibrium and therefore not subject to the formation of thunder‐showers. In the relatively weak gradients of convection‐weather, however, as soon as a convection‐cloud develops, the electrical field suddenly becomes very intense until, as the convection‐cloud forms into a mature cumulo‐nimbus,the phenomenal thunder‐storm potentials appear.
American URSI broadcasts of cosmic data with American magnetic character‐figure CA, April to June, 1940
Authors: Johnston H. F. 
Published: February 2008

The data for terrestrial magnetism, sunspots, and solar constant are the same as given in previous tables.The three columns for each month in Table 1 give (1) the magnetic character according to the scale 0–2 of the International Commission of Terrestrial Magnetism and Atmospheric Electricity, (2) the type featuring the day other than normal by the letters b, p, o, and i for days marked by bay, rapid pulsations, long‐period oscillations, and irregular oscillations, respectively, and (3) the hour and minute of Greenwich mean time marking the beginning of a storm, the end of the storm being indicated in the foot‐note to the Table.
F‐region critical frequencies at Deal, New Jersey, during partial solar eclipse of April 7, 1940
Authors: Schafer J. P. 
Published: February 2008

F‐region critical frequencies were obtained at Deal, New Jersey (latitude .30° 01′ north, longitude 75° 15′ west), on the day of the solar eclipse of April 7, 1940. The eclipse was partial in the vicinity of Deal with a magnitude of approximately 0.70 (60 per cent area).The results obtained are given in Figure 1 which shows the variation in F‐region critical frequency throughout the day of the eclipse as well as similar curves for the two days preceding and one day following. The solid‐line curve for the day of the eclipse shows the actual variations measured, while the dashed line for the same day indicates the possible trend in the absence of eclipse.
Huancayo Magnetic Observatory, October to December, 1940
Authors: Ledig Paul G. 
Published: February 2008

October 7–8—A mild disturbance in H accompanied by subnormal values occurred on October 7, beginning rather gradually at 00 h GMT, and lasting until about 21 h on the same day. Other low values in H were observed on the following day.October 26—There was a mild disturbance in H which began with a sharp rise and fall at 13 h 22 m GMT, October 26, and was followed by a single “bay” between 14 h 40 m and 15 h 00 m. The disturbance was followed by several hours of subnormal H‐values.
AmericanURSI Broadcasts of Cosmic Data, with American Magnetic Character‐Figure CA, October to December, 1940, and Summary of CA for Year 1940
Authors: Johnston H. F. 
Published: February 2008

The data for terrestrial magnetism, sunspots, and solar constant are the same as given in previous tables.The three columns for each month in Table 1 give (1) the magnetic character according to the scale 0–2 of the International Commission of Terrestrial Magnetism and Atmospheric Electricity, (2) the type featuring the day other than normal by the letters b, p, o, and i for days marked by bay, rapid pulsations, long‐period oscillations, and irregular oscillations, respectively, and (3) the hour and minute of Greenwich mean time marking the beginning of a storm, the end of the storm being indicated in the foot‐note to the Table.
The Daily Variation of Irregular Disturbances of the Earths's Magnetic Field at Bombay
Authors: Narayanaswami R. 
Published: February 2008

Besides the quiet‐day solar diurnal variation and the variations associated with magnetic storms, the intensity of the Earth's magnetic field at any place is subject to many irregular, short‐period fluctuations. The paper contains an analysis of the diurnal variation of these irregular disturbances during the eleven‐year period 1923–33. As a measure of the disturbance, the departures of the hourly ranges of the horizontal forces from the mean hourly range on the five international quiet days in that particular month were used. In calculating the disturbance, due regard was paid to the sign of the change of the element during the hour. The diurnal variations of the irregular disturbances depend on the season of the year and on the sunspot‐activity. These variations are analyzed and compared with the results of disturbance diurnal variation in higher latitudes. The main conclusions that emerge from the analysis are:(i) The hour of minimum disturbance occurs early in the morning usually between 04h to 05h or 05h to 06h local time and that of the maximum near about noon.(ii) There are two secondary maxima, one at 16h to 18h and another at about 22h to 23h local time.(iii) Analyzing the results according to month, the day maximum is most pronounced in the months April to August. In the winter months, there is a tendency for the variation to approach the European type (as shown by the analysis of the data of Eskdalemuir (magnetic latitude Φ=59°.5) and of Wilhelmshaven (Φ = 54°.5) in which there is one minimum in the morning at about 09h local time and a maximum in the evening at about 22 h.(iv) If days of magnetic character 2 are excluded, the diurnal variations are similar, but the late evening maximum is suppressed, leaving the noon maximum more pronounced.It is generally believed that “in the latitudes between the two auroral zones, that is, up to at least 65° magnetic latitude, Di has a simple diurnal variation with its maximum in the evening; as the auroral zone is approached the hour of maximum gets later, from about 21h at 55° to midnight at 70°. Up to this latitude the form of the daily variation of Di does not vary much either with season or with the general intensity of magnetic disturbance” [Chapman]. The present analysis of the Bombay data shows that in low magnetic latitudes, the main variation is a maximum near noon with a minimum a little before sunrise. The evening maximum of temperate latitudes is superposed on this simple variation.It is suggested that the maxima of disturbance‐variation at Bombay at about noon and in the afternoon are associated with the maxima of ion‐density in the E‐ and F1‐layers and in the F2‐layer, respectively. The late evening maximum is presumably due to fluctuations in F2‐layer caused by electrified particles from the Sun concentrating on the night side of the Earth on account of the deflecting action of its magnetic field.
Magnetic Horizontal Intensity at Oslo, 1843–1930
Authors: Wasserfall K. F. 
Published: February 2008

The Oslo Magnetic Observatory was founded by Professor Christopher Hansteen. The geographical coordinates of the station are ϕ = 59° 54′.7 north, λ = 10° 43′.4 east.The results published in this paper are based on magnetic data left by Hansteen and on the work done by his successors. The large bifilar magnet was mounted in May, 1841. This magnet is 1.2 meters long and weighs 13 kg. The suspension, which is nine meters long with 35 mm between the two threads, is solidly fixed to the vault of the central hall of the building. The two‐story hall has a gallery on the second floor—the vault carrying the astronomical equatorial tower of the building.
American URSI Broadcasts of Cosmic Data, Giving American Magnetic Character‐Figure, CA Three‐Hour‐Range Indices, K and Mean K‐Indices, KA, for January to March, 1941
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 January to March, 1941, are given in Table 1.
American URSI Broadcasts of Cosmic Data, Giving American Magnetic Character‐Figure, CA, Three‐Hour‐Range Indices, K, and Mean K‐Indices, KA, for April to June, 1941
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, 1941, are given in Table 1.
Huancayo Magnetic Observatory, April to June, 1941
Authors: Ledig Paul G. 
Published: February 2008

April 7—Small disturbances began at about 09h GMT, April 7. Large bays developed on all traces from 23h to 24h. Ranges: D, 14′; H, 60 gammas; Z, 62 gammas.April 9–11—This period was moderately disturbed.
The Ionosphere at Watheroo, Western Australia, July to September, 1941
Authors: Parkinson W. C. 
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 ionosphere as obtained by means of automatic multifrequency ionospheric recording apparatus located near Watheroo, Western Australia, in latitude 30° 19′.1 south, longitude 115° 52′.6 east of Greenwich, which operates over the frequency‐range 0.516 to 16.0 Mc/sec.Table 1 gives the monthly mean hourly values of the height of maximum electron‐density (hmax), uncorrected for retardation in lower regions2, and the minimum virtual height (hmin) for both the F1‐ and F2‐regions, the penetration‐frequencies for the E‐, F1‐, and F2‐regions, and the lowest frequency at which echoes were observed when that frequency was higher than 0.5.16 Mc/sec.
Hermanus Magnetic Observatory, July to September, 1941
Authors: Ogg A. 
Published: February 2008

(Latitude 33° 57′ S., longitude 18° 28′. or 1h 13m.9 E. of Gr.)July 3–10—There was a small sudden commencement at 12h 16m GMT, July 3, which was followed by a disturbed period of about three hours. There was a larger disturbance beginning with a sudden commencement at 03h 43m, July 4. The changes were: D moved 3′ easterly in five minutes; H increased 17 gammas in three minutes; Z decreased numerically 19 gammas in five minutes. The disturbances continued for about five hours. At 15h the storm increased, forming considerable bays on all traces until on July 5, from 06h to 07h, there were large changes leading to a large storm. Ranges: D, 57′.9; H, 456 gammas; Z, 293 gammas. The disturbances continued until July 10. The ranges in horizontal intensity were 100 gammas on July 6 and 59 gammas on July 7.
Auroras Observed at the Blue Hill Observatory, 1885–1940
Authors: Stetson H. T. , Brooks C. F. 
Published: February 2008

Two recent articles have appeared in this JOURNAL based on studies of a list of auroral occurrences observed at the Blue Hill Observatory since its founding in 1885 [see 1, 2 of “References” at end of paper]. It has been suggested that because of the importance of the relationships existing between solar activity, auroras, and other geophysical phenomena, so comprehensive a list of observations as has accumulated at Blue Hill should be made generally available.The list accordingly has been prepared to include well‐established auroras seen from Blue Hill or the adjacent territory and found on the records of the Observatory at Milton, Massachusetts. A few doubtful entries of suspected auroras have been deleted. Because of the large number of those who have participated in the meteorological observations since the establishment of the Observatory, it does not appear possible to list all the observers.
American URSI Broadcasts of Cosmic Data, Giving American Magnetic Character‐Figure, CA, Three‐Hour‐Range Indices, K, and Mean K‐Indices, KA, for October to December, 1941, and Summary for Year 1941
Authors: Johnston H. F. 
Published: February 2008

Summaries of American URSI broadcasts have appeared regularly in this JOURNAL since the issue for December, 1930.As set forth in this JOURNAL for June, 1937, “The Department of Terrestrial Magnetism and the United States Coast and Geodetic Survey with the cooperation of the United States Army and the United States Navy communication‐services and several amateur radio stations have undertaken to supply the American character‐figure based upon the reports of the seven American‐operated observatories—those of the Department of Terrestrial Magnetism at Huancayo in Peru and at Watheroo in Western Australia, and those of the United States Coast and Geodetic Survey at Cheltenham (Maryland), Honolulu (Hawaii), San Juan (Puerto Rico), Sitka (Alaska), and Tucson (Arizona).” This character‐figure is being designated CA, and its values for the first twelve, the second twelve, and all twenty‐four hours of each Greenwich day for October to December, 1941, are given in Table 1.
Cheltenham Magnetic Observatory, October to December, 1941
Authors: Ludy Albert K. 
Published: February 2008

(Latitude 38° 44′.0 N., longitude 76° 50′5 or 5h 07m.4 W. of Gr.)October 10–13—A disturbance occurred from 14h 48mGMT, October 10, to 01h, October 13. The highest K‐index was 6 which occurred but once. Ranges: D, 41′ H, 156 gammas; Z, 91 gammas.
Tucson Magnetic Observatory, October to December, 1941
Authors: Nelson J. H. 
Published: February 2008

(Latitude 32° 14′.8 N., longitude 110° 50′1 or 7h 23m.3 W. of Gr.)October 11–12—A very moderate storm began about 06h GMT, October 11, and continued for approximately twenty‐seven hours. A considerable amount of short‐period activity was superimposed on a few long‐period variations in both D and H. Very little disturbance in Z was noted. Approximate ranges: D, 11′; H, 139 gammas; Z, 30 gammas.
Huancayo Magnetic Observatory, October to December, 1941
Authors: Ledig Paul G. 
Published: February 2008

(Latitude 12° 02′.7 S., longitude 75° 20′4 or 5h 01m.4 W. of Gr.)October 22—There was a moderate disturbance characterized by small and relatively rapid movements resulting in a number of peaks and bays in H between 13h and 21h GMT, October 22. D and Z were only mildly disturbed.
Final Relative Sunspot‐Numbers for 1941
Authors: Brunner W. 
Published: February 2008

Table 1 contains the final sunspot‐numbers for 1941, for the whole disk of the Sun, based on observations made at the Zurich Observatory, supplemented by series furnished by other cooperating observatories for days (indicated by asterisks) on which no observations were possible at Zurich.Table 2 gives the yearly means of the relative numbers, R, since the last minimum 1933 and the number of days without spots.
American URSI Broadcasts of Cosmic Data, Giving American Magnetic Character‐Figure, CA, for January to March, 1942, Three‐Hour‐Range Indices, K, and Mean K‐Indices, KA, for October, 1941, to March, 1942
Authors: Johnston H. F. 
Published: February 2008

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

The Committee, which was appointed by the International Association of Terrestrial Magnetism and Electricity at the Stockholm Meeting in 1930 to consider existing and desirable distribution of magnetic and electric observatories, in its report invited attention to a subject which is as important as the establishment of additional observatories. It is that of the maintenance of proper adjustment of instruments, in particular, of variometers.The magnetic observatory at Hermanus, which was built in 1940, to meet the needs of the African Continent, came into full operation in January, 1941. The variometer‐equipment consists of one set of Askania D‐, H‐, and Z‐variometers and two sets of la Cour D‐, H‐, and Z‐variometers (15 mm/hr and 180 mm/hr).
Cheltenham Magnetic Observatory, January to March, 1942
Authors: Ludy Albert K. 
Published: February 2008

(Latitude 38° 44′.0 N., longitude 76° 50′.5 or 5h 07m.4 W. of Gr.)February 23–24—A moderate disturbance lasting about twenty‐one hours began at 13h 28m GMT, February 23, with a sudden small drop in H, followed by a gradual decrease during the following seventy‐five minutes, the total change being about 110 gammas. Thereafter irregular fluctuations continued until the end of the storm. Between 01h and 03h, February 24, there occurred a bay in west declination, which temporarily decreased about 24′. Another bay of about 20′ in the opposite direction occurred between 07h and 10h, just before the storm ended.
Magnetic Observatory, Hermanus, January to March, 1942
Authors: Ogg A. 
Published: February 2008

(Latitude 23° 25′.2 S., longitude 19° 13′.5 or 1h 16m.9 E. of Gr.)January 2–5—There were disturbances from 12h GMT, January 2, to 06h, January 3. The largest K‐number was 4, for the periods 12h–15h and 15h–18h, January 2 and 00h–03h, January 3. The disturbances began again at 10h, January 3 and continued until 24h, January 5. The greatest K‐number was 4 for the period 18h–21h, January 5.
Oscillations and pulsations recorded during the year 1941, at the magnetic observatory, Hermanus, South Africa
Authors: Ogg A. 
Published: February 2008

The oscillations and pulsations, which are discussed in this report, are those which occur on days which are otherwise quiet. The small movements seen on quiet days have been termed “pulsations” by Dr. van Bemmelen [see 1 of “References” at end of paper].Eschenhagen [2] was the first to investigate the smallest magnetic perturbations seen on magnetic records. These were fairly regular sinusoidal oscillations, which he called elementary waves.