bluuebunny/crossref_metadata_2025_split huggingface dataset:
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, April, May, and June 1932
Authors: Nicholson Seth B. , Sternberg Elizabeth E. 
Published: February 2008

The only magnetic storms during the second quarter of 1932 in which the total range in H exceeded 100γ were on April 7 and May 29. The storm of April 7 was reported in the last number of this publication.On May 29 only one spot was visible. No observations were made with the spectrohelioscope on that date. On May 28 the activity of the bright hydrogen near this group had increased slightly over that observed on May 27.
Remarks on Dr. Kennelly's notes
Authors: Bartels J. 
Published: February 2008

The readers of this JOURNAL will be grateful to Dr. Kennelly for his clear summary. He stresses the usefulness of the international conventions for a uniform adoption of units—a usefulness which is rather independent from theoretical considerations about which there is no unanimity.As to terrestrial magnetism it is a question whether the new conventions, especially the rather vague recognition of a physical dimension of the magnetic permeability, make a change in the usual practice necessary. I should like to support the unchanged use of the gauss (and of the γ as its 100000th part) as a unit even more strongly than Dr. Kennelly, for the following reasons: Practically all writers of text‐books or papers on terrestrial magnetism neglected from the outset the susceptibility of air, a procedure fully justified by the negligible numerical difference between B and H, as Dr. Kennelly also points out. Thus, if we speak of the magnetic field of the Earth and of its intensity, we need not state definitely whether we mean the quantity which the convention calls magnetic field‐strength H, or that which it calls flux‐density B. (Furthermore, it is usual in terrestrial magnetism—and sanctioned by the International Meteorological Conference at Paris in 1896—to reserve the letter H for horizontal force. We therefore may as well talk of the total force or total intensity of the north component, etc., and express them in the unit gauss, as heretofore. A physicist adhering to the conventions is at liberty to take the values as expressing “flux‐density”.) As Dr. Kennelly states, with the electric magnetometers —for instance, the Schuster‐Smith magnetometer—measurements are in fact made in the unit gauss as defined by the new international conventions.
Progress in the photography of the aurora borealis
Authors: Störmer Carl 
Published: February 2008

In pursuance of the collaboration of German and Norwegian scientists in the Aurora‐Borealis investigations initiated by Dr. Brüiche, the Notgemeinschaft der deutschen Wissenschaft, Heinrich Hertz Institute, and the AEG furnished the means for carrying out exhaustive research during the past winter on the instantaneous photography of the Aurora Borealis.In this research work, reduction of the exposure‐time is not only of profound importance from the standpoint of recording rapidly‐moving phenomena, but is also the hypothesis for the employment of the cinematographic principle for recording the behaviour of the Aurora Borealis as a function of time, as used for establishing any possible correlation with other phenomena (fluctuations of ionized‐region layers, rapid magnetic disturbances, etc.). In order to carry out the research work, Dipl. Ing. Bauer, assistant at the photophysical laboratory of the Danzig Technical University, worked as guest in the Aurora‐Borealis Observatory at Tromsö from December 1931 to April 1932 with apparatus from the AEG Research Institute.
American URSI broadcasts of cosmic data
Authors: Clarke Katharine B. 
Published: February 2008

The data for terrestrial magnetism, sunspots, 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 Terrestrial Magnetism and Electricity, (2) the type featuring the day other than normal by 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 0.77.
Graphical aids in the reduction of magnetic observations
Authors: Ennis C. C. 
Published: February 2008

In view of the voluminous computational work involved in the ordinary reductions of magnetic observations resulting from the photographic registrations at observatories, it is important to have in mind the development of methods for simplifying and expediting the computational work, and especially to devise methods of checking which are independent of the original computations. To this end the graphs presented herein were developed in the Department of Terrestrial Magnetism of the Carnegie Institution of Washington, primarily as aids in checking the diurnal‐variation values as determined from the differential expressionsΔX = cos D ΔH − H sin D sin 1′ ΔDΔY = sin D ΔH + H cos D sin 1′ ΔDΔF = cos I ΔH + sin I ΔZΔI = (1/F sin 1′) (cos I ΔZ − sin I ΔHUsing as an example the magnetic elements at Watheroo Magnetic Observatory for all days for 1929, where D = 4° 12′.1 west, I = 64° 15′.5 south, H = 24646γ, Z = − 51116γ, west declination and south inclination being reckoned minus, the above expressions reduce to
Provisional solar and magnetic character‐figures, Mount Wilson Observatory, July, August, and September, 1933, and note on values December, 1929, and January, 1930
Authors: Nicholson Seth B. , Sternberg Elizabeth E. 
Published: February 2008

In the third quarter of 1933 there were two magnetic storms in which the total range in H exceeded 100γ. No spots were visible at the time of the storm which began on August 5 nor was any exceptional activity recorded with the spectroheliograph.On September 6 an active group appeared and developed rapidly. Exceptionally bright hydrogen clouds were present over this group until it disappeared at the west limb on September 10. The magnetic storm which began September 8 was probably due to this activity, although it may have been caused by a less active region in which no spots were visible but which was near the central meridian on September 8.
Auroral observations and magnetic conditions at the Sitka Magnetic Observatory, July 1932 to June 1933
Authors: Ulrich Franklin P. 
Published: February 2008

This paper is a continuation of the reports,2 begun in 1923, of the investigation concerning the relation between aurora and the Earth's magnetic field. The investigation of the Earth's magnetic field and its relation to radio reception was discontinued with the report for 1928–29 because of the lack of proper sensitive instruments and because this investigation is being taken up elsewhere in a more detailed manner than was possible at this Observatory.Instruments and methods—The instruments and methods as outlined in the report for 1923–24 were used during these observations.
Summary of the year's work, Department of Terrestrial Magnetism, Carnegie Institution of Washington
Authors: Fleming J. A. 
Published: February 2008

The work of the Department during the report‐year, July 1, 1933, to June 30,1934, may be generally grouped under four divisions of endeavor. These were: (1) Reduction and study of the observational material already gathered; (2) development of methods and technique to obtain continuous records of the electrical conditions and their variations in the ionosphere ; (3) continued attack in the laboratory on basic phenomena of magnetism through experimental work in nuclear physics; (4) maintenance of field‐operations to preserve continuity of secular‐variation material and of records at observatories for seasonal, diurnal, and irregular fluctuations of the Earth's magnetic and electric field.Perhaps a most significant immediate advance is that in the ionosphere‐research which was initiated by the Department in 1925. In its latest development, it appears the most promising of recent methods of approach and one greatly enhanced by the rapid progress in nuclear physics and in wave‐propagation. It is not at the stage where continuous photographic records may be secured, manual observational methods meanwhile having shown fundamental results. This method appears also a sure means to obtain definite information not only of the conditions of the, as yet, otherwise inaccessible regions above the Earth's surface but of cosmical phenomena and of their relations to terrestrial ones. An understanding of the mechanism connecting the ionosphere and the external portion of the Earth's surface must improve knowledge of the relation of cosmical radiations in the ionosphere to their images represented by magnetic and electric phenomena at the Earth's surface and below the Earth's surface.
Final relative sunspot‐numbers for 1934
Authors: Brunner W. 
Published: February 2008

The following Tables contain the final sunspot‐numbers for 1934, 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 1 gives the yearly means of the relative numbers, R, since the last minimum 1923 and the number of days without spots.
Watheroo Magnetic Observatory October, 1934, to March, 1935
Authors: Parkinson W. C. 
Published: February 2008

(Latitude 30° 18′.1 S., longitude, 115° 52′.6 or 7h 43m.5 E. of Gr.)October 24, 1934—This small disturbance began with a sudden commencement at 1h 02m, G. M. T., the horizontal intensity showing a decrease of 5 gammas in two minutes. The declination changed 0′.7 westerly, while the commencement was not well marked in vertical intensity.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory April, May, and June, 1935
Authors: Nicholson Seth B. , Sternberg Elizabeth E. 
Published: February 2008

The storm of May 1 began with a sudden commencement in which the horizontal intensity increased 23 gammas. No observations with the spectroheliograph were made at Mount Wilson from April 27 to May 3. A group of spots, which in four days developed into a large group, was first seen on May 2 in latitude 32° south, 22° east of the central meridian.An active group which reached its maximum area on June 10 was first seen on June 8 in latitude 32° south, 19° east of the central meridian. On June 9 at 18h, G. M. T., very bright hydrogen‐clouds were observed over this group.
Measures of terrestrial‐magnetic activity
Authors: van Dijk G. 
Published: February 2008

In the abstract of his paper1, “Terrestrial‐magnetic activity and its relation to solar phenomena,” Professor Bartels states, “A break in the homogeneity of the international character‐figures in recent years is discovered.” From the contents of the paper it appears that by “recent years” especially the year 1930 is meant.Bartels bases his conclusion principally on the fact that while the international character‐number C shows a considerable increase from 1929 to 1930 (from 0.672 to 0.826) the u‐ and u1‐measures of magnetic activity indicate a small decrease (u from 1.05 to 1.00, u1 from 67 to 63).
The magnetic character of the year 1934 and the numerical magnetic character of days 1934
Authors: van Dijk G. 
Published: February 2008

The annual review of the “Caractère magnétique de chaque jour” for 1934 has been drawn up in the same manner as for preceding years. Fifty‐two observatories contributed to the quarterly tables, forty‐seven of them sent complete data.Table II (reproduced as Table 1 below) of the annual review, contains the mean character of each day for each month. The lists of calm days and disturbed days, and the days recommended for reproduction are also reprinted here as Table 2.
Mitteilung über erdmagnetische und elektrische Arbeiten in der U. d. S. S. R. in den jahren 1931–35
Authors: Puschkow N. W. 
Published: February 2008

Der Umfang der erdmagnetischen und elektrischen Arbeiten in der Sowjetunion wächst von Jahr zu Jahr. Diese Arbeiten werden jetzt von einer grossen Anzahl verschiedener Organisationen geleitet und durchgeführt: Geomagnetischen, hydrographischen, geologischen Instituten, Universitäten, und Hochschulen.Das Netz der magnetischen Observatorien—Die Sowjetunion verfügt zur Zeit über 18 magnetische Observatorien, von denen sechs sich in der Polarzone befinden. Wir halten diese Zahl aber für ungenügend: es wird beabsichtigt in der nächsten Zeit noch fünf bis sechs Observatorien in der Arktis und im asiatischen Teil der Union zu stiften. Nebst dieser Ausbreitung des Netzes wird auch beabsichtigt seine Ausrüstung bis zu einem Niveau zu heben, das unseren Observatorien gestatten wird eine allseitige Erforschung der magnetischen Erscheinungen mit allen zur Zeit zugänglichen Mitteln zu führen. Die Polarobservatorien werden mit je drei Serien von Magnetographen versehen, inklusive Magnétographe grosser Geschwindigkeit. Auch elektrische Messungsmethoden werden eingeführt.
Sitka Magnetic Observatory October to December, 1935
Authors: Hershberger John 
Published: February 2008

(Latitude 57° 03′.0 N., longitude 135° 20′.1 or 9h 0lm.3 W. of Gr.)October 20—The storm began about 10h.6, G. M. T., with a large increase in east declination and corresponding decreases in the two intensity‐components. The three elements immediately went into oscillations of large amplitudes and relatively short periods, which reached their maximum intensity about 11h.6. These continued until about 15h, when the amplitudes began to diminish and the elements gradually returned to their normal values. By 17h the storm had practically ended.
Cheltenham Magnetic Observatory October to December, 1935
Authors: Ludy Albert K. 
Published: February 2008

(Latitude 38° 44′.0 N., longitude 76° 50′.5 or 5h 07m.4 W. of Gr.)October 20–22—A disturbance of moderate intensity began October 20 at about 9h. The ranges were not great, the disturbance being chiefly short‐period fluctuations. At about 11h 20m there began a bay in horizontal intensity, lasting about 45 minutes, followed immediately by another bay in the opposite direction of about the same duration. Beginning at about 5h 45m October 21, there occurred a bay in all three elements of about one‐hour duration. Other bays in declination occurred at 22h 30m October 21 and 2h 20m October 22. The disturbance ended about 22h October 22.
Cheltenham Magnetic Observatory January to March, 1936
Authors: Ludy Albert K. 
Published: February 2008

(Latitude 38° 44′.0 N., longitude 76° 50′.5 or 5h07m.4 W. of Gr.)January 24–28—A moderate disturbance began at about 16h.5, January 24 and continued for several days, gradually diminishing until about 21h January 28. The greatest intensity of the disturbance occurred between 20h, January 24, and 5h, January 25. The ranges were: Declination, 21′; horizontal intensity, 100 gammas; vertical intensity, 87 gammas.
Publications relating to the polar year 1932–1933
Authors: la Cour D. 
Published: February 2008

During the last few years many publications pertaining to the Polar Year 1932–1933 have appeared in the different countries. Nevertheless, a large number of these publications have not yet been supplied for the archives of the International Commission for the Polar Year despite the resolution on this point adopted by the International Meteorological Committee at its meeting at De Bilt in 1933, and again emphasized by the Conference of Directors at Warsaw in 1935.In view of these facts, it is requested that there be sent to the Commission, if possible, five copies of all publications (small or large) relating directly or indirectly to the Polar Year which have not already been sent for its archives.
Watheroo Magnetic Observatory July to September, 1936
Authors: Green J. W. 
Published: February 2008

(Latitude 30° 19′.1 S., longitude 115° 52′.6 or 7h 43m.5 E. of Gr.)July 2—The disturbance recorded July 2 was of moderate intensity with definitely marked beginning at 1h 24m 40s GMT, as shown by record of the Crichton‐Mitchell vertical‐intensity inductometer. The elements were at their greatest divergence from normal between 12h and 13h. The disturbance ended at about 20h Ranges: Declination, 14′; horizontal intensity, 197 gammas; vertical intensity, 135 gammas.
Hansteen's magnetic instrument
Authors: Wasserfall K. F. 
Published: February 2008

Hansteen's historic magnetic instrument was, according to old documents, used on but one occasion after his death in 1873. This observation was made by the well‐known meteorologist H. Mohn in July 1882. As shortly afterwards a new unifilar magnetometer, Elliott No. 38, was provided, no further attention appears to have been given it.In 1922 it was decided to undertake the study of the long series of observations with a bifilar at the Oslo Observatory, begun by Hansteen in 1843 and which has continued without interruption until the present time. When the author began the reduction of the series, he found the oscillation‐box among some other equipment left by Hansteen but the magnet belonging to the box could not be found. This absolute instrument was very primitive, but the exactness of Hansteen's observations with it is none the less astonishing.
American URSI broadcasts of cosmic data October to December, 1936
Authors: Ennis C. C. 
Published: February 2008

The data for terrestrial magnetism, sunspots, and solar constant 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 Terrestrial Magnetism and Atmospheric Electricty, (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 the mean value of k for Mount Wilson was 0.53 during 1936.
Provisional solar and magnetic character‐figures, Mount Wilson Observatory October, November, and December, 1936
Authors: Nicholson Seth B. , Sternberg Elizabeth E. 
Published: February 2008

The magnetic storm of October 16–18 occurred during cloudy weather at Mount Wilson. An active group which crossed the central meridian on October 17.1 was 25° south of the center of the solar disc when the storm began, while another much smaller group, which crossed the central meridian on October 16.8, was 7° north of the center.At the time of the November storm two large active spot‐groups were nearly at the central meridian, one crossing it on November 29.4,16° north, the other on November 29.4,11° south of the center of the solar disc.
Principal magnetic storms Sitka Magnetic Observatory October to December 1936
Authors: Hershberger John 
Published: February 2008

(Latitude 57° 03′.0 N., longitude 135° 20′.1 or 9h 01m.3 W. of Gr.)October 9–10—A moderate disturbance began about 7h.5 GMT, October 9, and continued with gradually‐increasing intensity until at about 8h 21m, October 10, the amplitudes suddenly became very large and the periods short, continuing so for about an hour, After this the elements gradually quieted down, and by 17h, October 10, the disturbance was practically over.
Apia Observatory October to December, 1936
Authors: Baird H. F. 
Published: February 2008

(Latitude 13° 48′.4 S., longitude 171° 46′.5 or 11h 27m.1 W. of Gr.)October 9–10—A moderate disturbance was introduced at 7h 28m GMT, October 9, by a slight sudden rise in horizontal intensity. The H‐trace showed undue fluctuations and gradually fell to reach a minimum of 34921 gammas at 7h 41m, October 10, thereafter gradually returning to normal.
Observations at secular‐variation stations in Mexico during April and May, 1937
Authors: Gallo Joaquín 
Published: February 2008

During April and May 1937, 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 Oaxaca and Puebla. The results of these observations are shown in Table 1. Mr. Sandoval's instrument was CIW‐type magnetometer‐inductor No. 107 manufactured by the Precise Instrument Company, and the values shown in the Table are corrected to International Magnetic Standards.At Oaxaca the station is at the airport 2.5 km from the Cathedral, ISO meters northwest of the north end of the hangar and four meters east of road to farm. It is marked by a wooden peg. True azimuths from south through west are: Cross, Merced Church, 34° 11′.2; cross Santo Domingo Church, 52° 18′3.
Auroral observations on August 1, 1937, at Malcolm Island, Canada
Authors: McNish A. G. 
Published: February 2008

An interesting report of an auroral observation made at Pultney Point, Malcolm Island, near Vancouver Island, Canada, on August 1, 1937, has been received from Dr. T. G. Thompson of the Oceanographic Laboratories, University of Washington. The report states:“About 23h 30m (probably 120° west meridian time) we noted a great beam of greenish light to the southeast. The beam shifted and moved from southeast toward the west and eventually took the form of an enormous shaft of light extending across the sky. It was considerably above the clouds and we got a very beautiful cloud‐effect. The light was reflected in the waters of Johnstone Strait much the same as moonlight.
Tucson Magnetic Observatory April to June, 1937
Authors: Hershberger John 
Published: February 2008

(Latitude 32° 14′.8 N., longitude 110° 50′.1 or 7h 23m.3 W. of Gr.)April 2–3—A disturbance began at 05h 02m GMT, April 2, the chief movement being an increase of 13 gammas in H. This was followed by several long, shallow bays, and at 12h the disturbance seemed to have ended. But at 16h there were a few shorter‐period oscillations in H and D, of small amplitude. These were followed by a marked depression in the average value of H, which lasted until about 07h, April 4. During this period the traces were relatively quiet except for a few bays between 02h and 07h, April 3.
The magnetic character of the year 1936 and the numerical magnetic character of days 1936
Authors: van Dijk G. 
Published: February 2008

The annual review of the “Caractère magnétique de chaque jour” for 1936 has been drawn up in the same manner as for the preceding years. Fifty‐four observatories contributed to the quarterly tables; fifty‐two of them sent complete data.Table 1 (reproduced from Table II of the annual review) contains the mean character of each day for each month. The lists of calm days and disturbed days, and the days recommended for reproduction are also reprinted here as Table 2.
Note on auroras seen on July 22, August 3 and 4, 1937, in southwestern New Hampshire
Authors: McNish A. G. 
Published: February 2008

A report of auroras seen from a place about eight miles south‐southwest of Keene, New Hampshire, has been received from E. M. Brooks. The report is briefly summarized as follows:July 22—A few isolated beams were seen running upwards from a faint band extending from the north to the northwest at 3h 45m GMT. No indication of the aurora remained after 4h 15m.