bluuebunny/crossref_metadata_2025_split huggingface dataset:
AMERICAN URSI BROADCASTS OF COSMIC DATA
Authors: Ennis C. C. 
Published: February 2008

The data for terrestrial magnetism, sunspots, solar constant, and aurora are the same as given in previous tables.The first three columns of the Table give (1) the magnetic character according to the scale 0‐2 of the International Commission of TerrestrialMagnetism and 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 footnote to the Table. The next two columns give the data relating to sunspots: (1) the number of groups of spots and (2) the total number of spots. It is to be noted that sunspot‐numbers such as those from Zürich can be obtained from the number of groups and spots given in the Table by the formula N=k (10g+s), where k for Mount Wilson is about 0.7.
SITKA MAGNETIC OBSERVATORY JANUARY TO MARCH, 1934
Authors: Hershberger John 
Published: February 2008

(Latitude 57° 03′.0 N.; longitude, 135° 20′.1 or 9h 01m.3 W. of Gr.)The only storm of importance occurred on March 5. The storm was preceded by a gentle but gradually increasing disturbance beginning about 13h, March 4, Greenwich mean time. On March 5, D and H increased very suddenly at 7h 45m and Z began to increase about 7h 52m. All reached their maximum values within a few minutes and their minimum values about an hour later. The values were about normal again by 13h but the record continued disturbed for several days. The ranges were: D, 118′; H, 660γ; Z, 466γ.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, January, February, and March, 1937
Authors: Nicholson Seth B. , Mulders Elizabeth E. S. 
Published: February 2008

On January 27 from 19h 04m to 19h 45m, the magnetometer recorded a disturbance in the Earth's magnetic field, which occurred simultaneously with a complete fade‐out in short‐wave radio transmission on the Pacific Coast. H first decreased 41 gammas in 11 minutes, recovering 37 gammas in the next 30 minutes. Cloudy weather prevented solar observations at that time, although observations earlier in the day showed considerable activity on the Sun.The February storm occurred when a very large active sunspot‐group was three days past the central meridian. Dr. Hubble reported seeing an aurora during this magnetic storm at 8h, GMT, February 3. He described the aurora as reddish in color with a few typical streamers.
Observations at secular‐variation stations in Mexico during 1936
Authors: Gallo Joaquín 
Published: February 2008

During November and December 1936, R. O. Sandoval of the Magnetic Section of the National Astronomical Observatory of Mexico made observations of the absolute values of the magnetic elements at Mérida, Campeche, and Veracruz. The results of these observations are shown in Table 1. Mr. Sandoval's instrument was C.I.W.‐type magnetometer‐inductor No. 107 manufactured by the Precise Instrument Company, and the values shown in the Table are corrected to International Magnetic Standards.The station at Mérida was at the airport 6.5 km southwest of the City, while at Campeche the station was also at the airport 1.5 km south of the Cathedral. At both of these stations observations could be made only at certain times of the day. At each station a small cement platform was constructed at ground‐level, the precise point being marked by a cross. An iron pole 800 meters to the north of each station marks the astronomical meridian. The station at Veracruz was 1.5 km north of the Plaza and without interference from buildings or ships.
Summary of the year's work, Department of Terrestrial Magnetism, Carnegie Institution of Washington
Authors: Fleming J. A. 
Published: February 2008

Terrestrial magnetism—During the year ended June 30, 1937, the program of the Department was devoted not only to experimental investigation, but also to the coordination and integration of isolated researches that the inferences of each may be more broadly interpreted. Such a program cannot be consummated within a limited period so that reports of successive years must bear similarities outlining the general progress and application of experimental fact as it is revealed. During the year the common goal and unity of the several branches of research have been admirably demonstrated.Thus the association of a special type of magnetic disturbance and sharp fade‐outs of high‐frequency radio‐wave reflections with bright eruptions in the solar chromosphere, first pointed out by J. H. Dellinger, was conclusively proved by work of the Department in cooperation with Mount Wilson Observatory and other organizations. These effects are propagated from the Sun with the velocity of light. The active agent is believed to be ultra‐violet light originating in the solar eruption which produces sudden and intense electrification of the Earth's upper atmosphere. These new effects serve to discriminate between various theories of terrestrial‐magnetic changes and supply evidence on the electrical processes taking place in the ionosphere. The evidence yielded by the automatic recorders at the Huancayo and Watheroo observatories concerning the nature of the radio “fade‐out” effect indicates that this phenomenon is predominantly due to an intense ionization between heights of about 60 and 100 km. The high ionization produced below the lower E‐region of the ionosphere by bright chromospheric eruptions apparently causes radio‐echo disappearance through absorption in this region of high collisional frequency. A definite magnetic effect is observed during the fade‐out. Analysis of this effect shows it to be an augmentation of the magnetic diurnal variation as contrasted with other types of magnetic disturbance. The association of a magnetic effect of the diurnal‐variation type with a definite region of the ionosphere through experimental observations forms a contribution of first importance to the science of terrestrial magnetism. The simultaneity of the fade‐out, magnetic, and earth‐current effects with solar outbursts in the region of sunspot‐areas was confirmed by direct observation at the Huancayo Magnetic Observatory.
Lunar diurnal variation in Earth‐currents at Huancayo and Tucson
Authors: Rooney W. J. 
Published: February 2008

The lunar diurnal variation in earth‐current flow at Huancayo and Tucson has been determined from the records for the year 1932, near the sunspot‐minimum. Using the method employed by Chapman for the magnetic elements, a definite lunar diurnal variation of markedly double period is found in both components of the potential‐gradient at both stations. Harmonic analyses of the mean curves show that at Huancayo the amplitude of the second harmonic is about one‐sixth that of the solar diurnal variation for the same year, while the amplitudes of the first, third, and fourth harmonics are negligibly small. At Tucson the amplitude of the second harmonic is about one‐fifth that of the solar diurnal variation for the northward component which is the principal component at that station.The manner in which the lunar diurnal variation changes with the phase of the Moon was also examined. For both components at Huancayo, curves constructed for the four main phases of the Moon show a marked increase in activity during daylight hours and a corresponding diminution during the night so that the individual curves are no longer semi‐diurnal. For Tucson the curves for the individual phases of the Moon, as determined from this single year's record are too irregular to show the changes definitely, but do indicate that they are less pronounced at this higher‐latitude station. As a check on this point the lunar diurnal variation at Tucson was redetermined by the method applied by Egedal to the data from Ebro. In this method the lunar diurnal variation is obtained from the records for the individual hours of the solar day. Using the hours from 12 to 24 the lunar diurnal variation found is in good agreement with that obtained by the usual method. Comparing the lunar diurnal variation obtained separately by this method during daylight, 12h to 18h, with that obtained during the night, 18h to 24h, there is found only a slight decrease in amplitude from day to night and very little change in phase. These results are in agreement with those obtained by the first method and also with the revised conclusions reached by Egedal from his studies of the Ebro records.
Watheroo Magnetic Observatory, January to March 1938
Authors: Green J. W. 
Published: February 2008

(Latitude 30° 19′.1 S., longitude 115° 52′.6 or 7h 43m.5 E. of Gr.)January 16–17—This storm, beginning at 22h 30m GMT, January 16, reached its greatest intensity on January 17. Ranges: D, 38′; H, 246 gammas; Z, 254 gammas.
Magnetic Observatory, Capetown January to March, 1939
Authors: Ogg A. 
Published: February 2008

January 4—There was a small disturbance at 23h 05m GMT, January 4. The changes were: H, −12 gammas in six minutes; Z, −14 gammas in ten minutes.January 5—There was a small disturbance at 04h 08m GMT, January 5. The changes were: D, −4″.0 in six minutes; H, −21 gammas in six minutes; Z −32 gammas in thirty minutes.
Wide‐range magnetograph at Washington, D.C.
Authors: Fleming J. A. 
Published: February 2008

An experimental installation has been set up in the Standardizing Magnetic Observatory of the Department of Terrestrial Magnetism of the Carnegie Institution of Washington intended primarily for the experimental development of geomagnetic equipment and appliances. Further, it will serve for the general training of observers assigned to duty at observatories. As in the past, standardization of instruments, tests of sensitive apparatus, and final instruction of observers will be done at the Cheltenham Magnetic Observatory of the United States Coast and Geodetic Survey with the close cooperation of that Bureau and the Department of Terrestrial Magnetism.This includes a wide‐range magnetograph, which will also provide complete records of such violent magnetic storms as those of March 24–25 and 29–30, 1940. La Cour variometers for declination, D, and horizontal intensity, H, and the CIW induction‐variometer for vertical intensity, Z, with scale‐values adjusted to about 30 gammas per mm, record on the drum of a la Cour magnetograph, with a time‐scale of one hour=15 mm, and automatic time‐marks every ten minutes. The photographic sheets are 300 mm wide, and the quiet traces are kept near the center of the sheet so that deflections up to 3500 gammas may be recorded.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, January to March, 1940
Authors: Nicholson Seth B. , Mulders Elizabeth Sternberg 
Published: February 2008

The magnetic disturbances beginning on January 3, 10, 30, and February 24 were probably all associated with the very large group of sunspots whose successive central meridian passages occurred on January 5.5 (Mount Wilson No. 6725), February 1.8 (No. 6741), and February 28.5 (No. 6756).The same group crossed the central meridian for the fourth time on March 27.0 (No. 6784). On the previous appearances it had been a typical bipolar group, but now all that remained was the principal preceding member—a round stable unipolar spot.
Ionospheric changes associated with the magnetic storm of March 24, 1940
Authors: Berkner L. V. , Seaton S. L. 
Published: February 2008

Observations of the ionosphere at the Huancayo and Watheroo magnetic observatories during the great magnetic disturbance of March 24, 1940, are shown and discussed. At Huancayo, the ionospheric disturbance began about 40 minutes before the first really large magnetic change, though coinciding with increasing magnetic activity. During the first great magnetic changes, the F2‐layer was swept upward and disappeared in about 30 minutes. At the same time, ion‐density of the E‐layer rose about 40 per cent.Growth of a “new” F2‐layer began after disappearance of the old, proceeding in an apparently normal manner for the next hour. Because the original ion‐density had been reduced to a low value, the F2‐region is regarded as a nearly un‐ionized atmosphere, suddenly exposed to solar radiation. Effective recombination‐coefficient and rate of ion‐production at level of maximum density of F2‐region are estimated from this growth. This yields approximate values of α = 1.8 × 10−10 and q0 = 230. These values must be somewhat larger, and must increase downward, if height‐change during growth of the layer is to be explained without electron‐transport during the interval.Steady growth of the new F2‐layer was followed by a succession of abnormal increases and decreases of ion‐density of diminishing amplitude at an almost regular period of three hours for three and one‐half or four periods. Abnormal rate of decrease and subsequent increase of abnormal electron‐production at level of maximum is computed for the first period. This varies between −1000 and +1700 electrons per cc per second.At Watheroo Magnetic Observatory ionospheric changes followed the general pattern usually experienced during magnetic disturbances in temperate zones. Evidence indicates large spatial tilts of iso‐ionic surfaces near Watheroo about 40 minutes after beginning of great magnetic changes. These spatial tilts were followed by rapid rise of height and increase of scattering.Abnormal decrease of ion‐density of the F2‐layer at both observatories began simultaneously, within observational limits, less than 15 minutes after the first great geomagnetic change. The great rise in height at Watheroo lagged behind that at Huancayo by nearly an hour. A chronology of radio fade‐outs and bright chromospheric eruptions before and during the storm is given.
American URSI broadcasts of cosmic data, with American magnetic character‐figure CA, July to September, 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.
Notes on Isomagnetic Charts: III—The Isogonic and X‐, Y‐Charts for the Centered Dipole Field
Authors: Chapman S. 
Published: February 2008

Summary—Various forms of the equations of the isogonic lines are derived, for the field of the centered magnetic dipole. The isogonic chart for this field is shown to have two singular points in addition to the four uniform ray‐poles (one at each magnetic or geographic pole); these singular points, which are situated at the intersections of the magnetic and geographic equators are rectangular nodes. The equation and form of the nodal curves are discussed. The area over which the magnetic declination exceeds the obliquity of the magnetic axis is also considered; it is shown to cover more than a third of the whole area of the sphere, however small the obliquity may be.The Y‐ and X‐isomagnetic charts are also briefly considered; the former has only two singular points, namely non‐uniform ray‐poles at the geographic poles; these are also (non‐uniform) ray‐poles of the X‐chart, which in addition has two nodes at the same points as those of the D‐chart; but in the case of X these nodes are not rectangular.
The Lunar Diurnal Variation of the Horizontal and Vertical Magnetic Forces at the Polar‐Year Station Mogadiscio
Authors: Egedal J. , Bossolasco M. 
Published: February 2008

An article on the lunar diurnal variation of the magnetic declination at Mogadiscio has already been published in this Journal.1The main results of a derivation of the lunar diurnal variation of the horizontal and vertical forces at the same place are given below. A more detailed account in Italian has been published in “Geofisica pura e applicata.”
The Ionosphere at Huancayo, Peru, July to September, 1940
Authors: Wells H. W. , Coile R. C. 
Published: February 2008

This report is a continuation of those already published in this Journal1 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 Huancayo, Peru, South America, in latitude 12° 02′.7 south, longitude 75° 20′.4 west of Greenwich, which operates over the 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 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 0.516 Mc/sec.
Magnetic Character, January to June, 1940
Authors: van Dijk G. 
Published: February 2008

I have pleasure in giving below the lists of the selected five calm and five disturbed days and the days, recommended for reproduction for the period January to June 1940 and should feel much obliged to you if these data could be inserted in one of the next numbers of the Journal.The following days are recommended for reproduction:Very greatly disturbed, March 24, March, 29, 1940; greatly disturbed, January 3, April 2, April 25, June 25, 1940.
Huancayo Magnetic Observatory, December, 1940, to March, 1941
Authors: Ledig Paul G. 
Published: February 2008

December 20–25—A moderate disturbance in H accompanied also by definite disturbances in D and Z began gradually about 13h GMT, December 20, and was marked by a series of sharp peaks and bays lasting until about 20h. The disturbance was followed by subnormal values and mild disturbances in H until December 25.December 31—A sharp disturbance in H of short duration was recorded on December 31. It began at 13h 25m GMT, with a rapid rise followed by a rapid fall to a narrow bay, then about an hour later at 14h 30m a rise of 170 gammas occurred in ten minutes to reach a high peak followed by a fall of 300 gammas to a sharp bay in twenty minutes. The next three hours was a period of moderate disturbance, followed by several hours of subnormal values in H and with a return to practically normal conditions at 22h. Both D and Z were somewhat disturbed from the beginning of the storm until after 17h.
American Magnetic Character‐Figure, CA, Three‐Hour‐Range Indices, K, and Mean K‐Indices, KA, for April to June, 1944
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, 1944, are given in Table 1.
Sitka Magnetic Observatory, April to June, 1944
Authors: Pinckney Harold W. 
Published: February 2008

(Latitude 57° 03′.0 N., longitude 135° 20′.1 or 9h 01m.3 W. of Gr.)April 2–6—Beginning about 06h 26m GMT, April 2, a disturbance was severe until about 13h with K‐indices of 9, 9, 8 being recorded. With the exception of the period between 07h and 11h, April 6, when a K‐index of 8 was reached, activity was moderate.
On Contributions to the Early History of Geomagnetism
Authors: Espenschied L. 
Published: February 2008

Here are a couple of related observations that may be of interest to the JOURNAL in case they have thus far escaped attention:It appears that one of the earliest of the electrical experimenters, one Otto von Guericke, of the mid 1600's, was led to make his experiments in generating electricity by means of a rotating sulphur globe by having entertained an electrical theory in lieu of the then magnetic conception of the gravity of the Earth. This is brought out in what to me was a charming article upon the subject of von Guericke, by Thomas Coulson, which appeared in the September and October issues of 1943 of the Journal of the Franklin Institute. I myself am an appreciative owner of von Guericke's book. ... I have been hoping that some scholar might eventually find enough interest in the Experimenta Nova to render it into English. Not only would it be interesting to know what von Guericke's ideas really were in this respect, but it is conceivable that since they were not subject to the limiting influence of our subsequent findings and mode of thought, there might be in them some refreshing novelty and suggestiveness.
Geophysical Work in the Union of Soviet Socialist Republics
Authors: Pushkov N. 
Published: February 2008

For a better understanding of geophysical operations in the U.S.S.R. I should like to give some details concerning our work during the last few years.The Institute of Terrestrial Magnetism was established in 1940. At first we had only two sections, namely, (1) a group for magnetic survey on land in Leningrad and (2) a magnetic observatory at Pavlovsk (Slutsk). A short time afterward, several new groups were organized as follows: for magnetic survey at sea; magnetic cartography; theoretical investigations; superintendence of magnetic observatories; and some others. The Slutsk Ionospheric Station and the Magnetic Observatory were incorporated into the Institute.
Apia Observatory October to December, 1945
Authors: Beagley J. W. 
Published: February 2008

(Latitude 13° 48′.4 S., longitude 171° 46′.5 or 11h 27m.1 W. of Gr.)October 11–13—A period of minor disturbance commenced with a small positive bay at 22h GMT, October 11, and lasted until 11h, October 13. The principal features were bays in H during the fourth three‐hour period of October 12 and the third three‐hour period of October 13, giving K‐indices of 5 and 4, respectively. There were only slight fluctuations on the Z‐trace, and D\ was undisturbed.