bluuebunny/crossref_metadata_2025_split huggingface dataset:
Conversion of Berlin Earth‐current data to millivolts per kilometer
Authors: Gish O. H. 
Published: February 2008

Doubtless others than the writer have at times desired to know the equivalent, say in millivolts per kilometer, of the arbitrary units used for expressing the valuable earth‐current data obtained at Berlin.Recently an estimate of such an equivalent in millivolts per kilometer has been made on the basis of information given in an article entitled “Die Erdstrom‐Aufzeichnungen in den deutschen Telegraphen‐Leitungen” transmitted by Dr. von Stephan, Staats‐Secretär des Reichs‐Postamts1. Here (p. 558) one finds the statement (referring to Plate IX) : “In den Declinations‐Schwankungen bedeutet 1 mm nahezu 0.8 Bogenminuten, bei den Erdströmen dagegen die Hälfte der elektromotorischen Kraft eines Daniell‐ (Zink‐Kupfer) Elements (letztere von l Volt wohl nicht stark verschieden).” From this it appears that for the earth‐current graphs on Plate IX, one millimeter is at least roughly equivalent to 0.5 volt. The same scale is apparently also used for the earth‐current graph on Plate X. The range on that graph (in the case of the Berlin‐Dresden span) is 80 mm which is then equivalent to 40 volts or, since this line is 120 kilometers long, to 333 millivolts per kilometer, which is a reasonable value for a moderate storm.
Huancayo Magnetic Observatory October to December, 1935
Authors: Torreson O. W. 
Published: February 2008

(Latitude 12° 02′.7 S., longitude 75° 20′.4 or 5h 01m.4 W. of Gr.)October 20–21—A mild disturbance, beginning inconspicuously at about 9h 10m with very small perturbations in all three elements, the perturbations gradually increasing in magnitude and period up to 13h and thereafter H, particularly, showing several large peaks and bays of 50‐ to 100‐gamma range, with periods of about one hour from crest to crest, until 20h. D and Z were considerably disturbed also during the period from 13h to 20h. On October 21, large bays and peaks occurred in H during the daylight hours (12h to 21h, G. M. T.), while D and Z were little disturbed. The end of the disturbance was not well defined. The ranges recorded were: Declination, 9′; horizontal intensity, 208 gammas; vertical intensity, 54 gammas.
Harvard University
Authors: Stetson Harlan T. 
Published: February 2008

A communication just received at the Institute of Geographical Exploration from Dr. Carl Störmer (Norway) states that thus far no authenticated observations of the long delayed echoes such as were widely observed during the sunspot maximum of 1929 have yet been reported.The recent rapid rise in sunspot‐numbers should indicate an early return of conditions favorable to reception of these echoes of long delay. Since the conditions most favorable for the phenomenon occur, as Dr. Störmer has pointed out (Nature, January 5, 1929), when the Sun is near the magnetic equator, we shall next be approaching these favorable conditions in February.
Apia Observatory January to March, 1936
Authors: Baird H. F. 
Published: February 2008

(Latitude 13° 48′.4 S., longitude 171° 46′.5 or 11h27m.1 W. of Gr.)Sudden rises in the value of horizontal intensity, followed by only slightly disturbed traces, occurred at 3h 32m, January 8; 9h 21m, February 14; and 10h 55m, February 16, The maximum rise, that on February 16, was of 23 gammas.
American URSI broadcasts of cosmic data, April to June, 1936
Authors: Ennis C. C. 
Published: February 2008

The data for terrestrial magnetism, sunspots, solar constant, and auroræ 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 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.
Huancayo Magnetic Observatory April to June, 1936
Authors: Torreson O. W. 
Published: February 2008

(Latitude 12° 02′.7 S., longitude 75° 20′.4 or 5h 01m.4 W. of Gr.)April 17–23—A prolonged but mild disturbance, interesting chiefly because it occurred 27 days after a mild disturbance in March of similar character. This disturbance may be said to have begun with an inconspicuous sudden commencement at 18h 30m GMT, in all three elements. H increased 17 gammas in four minutes, while D and Z just perceptibly increased. Following this, H decreased steadily to a very low value by 3h on April 18. A similar decrease on several successive days, occurring between 0h and 5h, was the most conspicuous feature of the disturbance. On all days there were superposed on the H‐trace, numerous quite large bays and peaks which, while causing much irregularity, did not prevent the appearance of the usual diurnal character. Both D and Z showed numerous small perturbations throughout the disturbance, which did not affect the general diurnal trend. The end of the disturbance is very indefinite, the trace for April 23 being quite irregular while that for April 24 was comparatively smooth and quiet.
Watheroo Magnetic Observatory April to June, 1936
Authors: Green J. W. 
Published: February 2008

(Latitude 30° 19′.1 S., longitude 115° 52′.6 or 7h 43m.5 E. of Gr.)May 29—There was a sudden commencement on May 29. Its time of beginning as recorded by the vertical‐intensity inductometer 8h 48m 00s GMT. H increased 12 gammas in three minutes; 7 gammas of the increase took place in the first half‐minute. H then decreased 77 gammas to minimum at 13h 32m and then increased 81 gammas to maximum at 21h 50m. Z increased 2 gammas abruptly, then 5 gammas in 12 minutes followed by disturbance in which Z had a range of 65 gammas with minimum at 13h 40m and maximum at 21h 50m.
Dr. Nanabhai Ardesher Framji Moos, 1859–1936
Authors: Unakar Mukund V. 
Published: February 2008

The death, on March 12, 1936, of Dr. N. A. F. Moos removed from the field of terrestrial magnetism one of its well‐known representatives during the last four decades. His scientific activities were intimately associated with the development of the magnetic work of the Bombay Observatory of which he was director from 1896 to 1919.The selection of the present site of the Observatory at Colaba dates from 1823. It was inaugurated as an astronomical observatory and not until 1841 were magnetic and meteorological observations added to its activities. Only from 1846, however, was the Observatory properly equipped to take regular observations in magnetism and meteorology. In 1865 Mr. Charles Chambers was appointed its first full‐time superintendent and in a short time the Observatory was provided with autographic instruments for continuously recording the magnetic and meteorological elements and soon entered upon an era of real scientific activity both in regard to the collection of accurate data and to their discussion.
American URSI broadcasts of cosmic data July to September, 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 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.
Cheltenham Magnetic Observatory July to September, 1936
Authors: Ludy Albert K. 
Published: February 2008

(Latitude 38° 44′.0 N., longitude 76° 50′.5 or 5h 07m.4 W. of Gr.)July 1–3—A moderate disturbance began about 20h GMT, July 1, and ended just two days later. The beginning and ending were gradual. The disturbance was marked by rapid decrease in horizontal intensity of 27 gammas in 6 minutes at 4h 14m, July 2, and a decrease in vertical intensity of 39 gammas in 30 minutes at 7h42m, July 2. Ranges: Declination, 17′; horizontal intensity, 146 gammas; and vertical intensity, 113 gammas.
Huancayo Magnetic Observatory January to April, 1937
Authors: Davies Frank T. 
Published: February 2008

(Latitude 12° 02′.7 S., longitude 75° 20′.4 or 5h 01m.4 W. of Gr.)January 27—A sudden commencement occurred at 03h 37m GMT, January 27. In four minutes H increased 28 gammas, Z increased 7 gammas, and D decreased 1′. The records were moderately disturbed from 07h to 14h.
The geophysical observatory of Chambon‐la‐Forêt
Authors: Harradon H. D. 
Published: February 2008

The development of electric‐railway lines, particularly in the vicinity of large cities, has made necessary in recent years the transfer of several magnetic observatories to more isolated and magnetically undisturbed sites. Thus in the last decade it has been found necessary to move the principal magnetic observatory of Germany from Seddin to a new site at Niemegk and the Sverdlovsk (formerly Ekaterinburg) Observatory, where for nearly 100 years magnetic observations had been in progress, to Vyssokaja Dubrava, some 30 km from the old location.We now learn from a booklet kindly furnished us by Professor Ch. Maurain, that the central magnetic observatory of France, previously located at Val‐Joyeux, about 25 km from Paris, owing to the encroachment of industrial electric currents, has been moved to a clearing in the Forest of Orléans, Commune de Chambon‐la‐Forêt (Département du Loiret), 87 km south of Paris. The geographical coordinates of the new observatory are latitude 48° 01′ 26″ north, longitude 2° 15′ 36′′ east of Greenwich, or 0° 04′ 38″ west of Paris; the elevation above sea‐level of the pier where the magnetic observations are made is about 133 meters. The greater part of the site lies in a clearing in the forest, the remainder being wooded. A determination of the magnetic susceptibility of several samples of the soil gave a mean value of 2×10−6, so that the soil may be regarded as practically non‐magnetic.
MacGregor Arctic Expedition, 1937–38
Authors: Johnston H. F. 
Published: February 2008

This Expedition, under the command of C. J. MacGregor, Meteorologist of the United States Weather Bureau, left Port Newark, New Jersey, for the Far North on July 1, 1937. The Expedition hopes to arrive in Grinnell Land late in August and will establish its base at Fort Conger, Lady Franklin Bay, a station which was previously occupied by General A. W. Greely during the First International Polar Year in 1882–83. On August 17 the Expedition reported by radio being in latitude approximately 73° north near Thule, Greenland.Commander MacGregor with eleven assistants sailed on the three‐masted schooner, General A. W. Greely. This schooner of 200 tons net registry was built for trading in the arctic regions. Her frame is extra strong and the massive knees to withstand ice‐pressure are all of natural wood. In addition her hull is encased by two extra sheaths of two‐inch planking of oak. Sails will be depended upon during the greater part of the voyage to the north, occasional assistance being given by two 40‐horse‐power Sterling marine engines. The twin propellers are protected from small pieces of ice by heavy oak‐casings.
American URSI broadcasts of cosmic data, April to June, 1937, with American Magnetic character‐figure CA, June to August, 1937
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 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 the mean value of k for Mount Wilson was 0.53 during 1936.
Sitka Magnetic Observatory April to June, 1937
Authors: Gebhardt Robert E. 
Published: February 2008

(Latitude 57° 03′.0 N., longitude 135° 20′.1 or 9h 01m.3 W. of Gr.)April 24–25—A slight disturbance beginning abruptly at 12h 02m GMT, April 24, marked the beginning of several days of severe storms. This disturbance continued with increasing activity until it had reached its maximum intensity at 00h 10m, April 25. After about two hours the disturbance stopped quite sharply and in another five hours the three elements were normal. Ranges were: D, 69′; H, 545 gammas; Z, 298 gammas.
Sitka Magnetic Observatory July to September, 1937
Authors: Gebhardt Robert E. 
Published: February 2008

(Latitude 57° 03′.0 N., longitude 135° 20′.1 or 9h 01m.3 W. of Gr.)July 6–7—A slight disturbance occurred on July 6, characterized by a sharp movement in D and H (76 gammas decrease in H) at 0h 52m GMT. The elements remained calm until 11h at which time they began to decrease gradually until 14h 30m GMT, then started a slow but steady return to normal values. The trace was at its normal value about 03h GMT, July 7. The disturbance was marked by its uniform motion; sudden rapid oscillations were noticeably absent. Ranges: D, 31′; H, 211 gammas; Z, 331 gammas.
Ionospheric observations: Eclipse of June 8, 1937
Authors: Wells H. W. , Stanton H. E. , Seaton S. L. 
Published: February 2008

Special ionospheric observations conducted at Huancayo (Peru) and Watheroo (Western Australia) for the eclipse of June 8, 1937 show:(1) The day of the eclipse was normal, ionospherically.(2) No eclipse‐effect for F‐region critical frequencies at Huancayo.(3) The eclipse caused merging of the F1‐ and F2‐regions, followed by normal conditions at sunset, more than an hour earlier than usual.The absence of any eclipse‐effect in the F‐region critical frequencies may be real or may be attributed to the fact that the eclipse did not occur at Huancayo until late afternoon. It is suggested that for such conditions ionizing radiation from the Sun would be greatly reduced by absorption in the Earth's atmosphere before the beginning of the eclipse due to the large zenith‐angle of the Sun.
American URSI broadcasts of cosmic data, October to December 1937, with American magnetic character‐figure CA, January to March 1937, and November 1937 to January 1938
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 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 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 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; during 1937 this value varied from 0.47 to 0.66, with an average value of 0.53.
Coil‐magnetometer and Earth‐inductor—A comparison of results obtained at the Abinger magnetic station of the Greenwich Royal Observatory
Authors: Greaves W. M. H. , Witchell W. M. 
Published: February 2008

Dr. J. Egedal, Danish Meteorological Institution, Copenhagen, has recently made an examination of the results obtained at a number of magnetic observatories in the northwest of Europe, with special reference to the magnetic vertical intensity, Z, as derived from observations with earth‐inductors. In the course of his investigation the values obtained in 1934 at Abinger, both with the inductor and with the Dye coilmagnetometer for directly determining Z, were compared, and it seemed to Dr. Egedal that discordances could most easily be explained as due to an effect of temperature in the magnetometer. He communicated this opinion to the Royal Observatory, Greenwich, and it was felt there that the matter deserved a closer investigation than would have been possible to anyone not having full details of the observing conditions.Accordingly the differences at Abinger in Z base‐line value as given by inductor and magnetometer have been analyzed, taking all days in the years 1934–37 on which determinations were made by both instruments.
The electric characterization of days at the Huancayo Magnetic Observatory for the 12 years 1925–1936
Authors: Torreson O. W. 
Published: February 2008

Observations of the atmospheric potential‐gradient were begun by the Carnegie Institution of Washington at the Huancayo Magnetic Observatory, in Peru, in 1924. A photographically‐recording apparatus was installed at that time and has been in practically continuous operation up to the present. The data thus accumulated are now being tabulated for publication and will appear shortly, together with complete descriptions of the apparatus, its location, and particulars of the surrounding countryside.At the inauguration of the observing‐program it was decided that the electric characterization of days as used by the British Meteorological Office at Kew Observatory should be adopted. This system has recently been described in detail by F. J. W. Whipple1 and need be mentioned only briefly here. There are three character‐figures, 0, 1, and 2. “0” denotes the absence of negative potential in any 24‐hour period beginning at midnight, “1” indicates the existence of negative potential at one or more times during the 24‐hour period but with a total duration of less than three hours, and “2” indicates the existence of negative potential for a total duration of three hours or more.
Huancayo Magnetic Observatory, January to March 1938
Authors: Davies Frank T. 
Published: February 2008

(Latitude 12° 02′.7 S., longitude 75° 20′.4 or 5h 01m.4 W. of Gr.)January 16–17—A marked sudden commencement occurred at 22h 37m GMT, January 16. In one minute, H increased 250 gammas, Z increased 24 gammas and then decreased 13 gammas, and D moved 2′.3 west and then 4′,4 east. Rapid oscillatory motions of the H‐spot continued until about 02h, January 17. Milder activity prevailed until 12h when severe and rapid changes began in horizontal intensity lasting until 18h. Between 14h and 15h there was a 355‐gamma bay in H. The minimal value in H was 29320 gammas at 16h 25m. There was another period from 21h 20m to 24h during which H was quite disturbed. The storm ended about 24h, January 17. Ranges: D, 12′.8; H, 505 gammas; Z, 62 gammas.
Final relative sunspot‐numbers for 1937 and monthly means of prominence‐areas for 1931–1937
Authors: Brunner W. 
Published: February 2008

Table 1 contains the final sunspot‐numbers for 1937, 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.
Watheroo Magnetic Observatory, April to June 1938
Authors: Green J. W. 
Published: February 2008

(Latitude 30° 19′.1 S., longitude 115° 52′.6 or 7h 43m.5 E. of Gr.)April 13–14—Following a sudden commencement at 11h 43m GMT, April 13, D moved westerly 0′.5 suddenly, then 1′.5 in forty seconds and 5′ during the next three minutes. H increased 27 gammas in three minutes followed by an abrupt decrease of 10 gammas and a further increase of 15 gammas. The numerical value of Z after an initial increase of 2 gammas decreased 8 gammas abruptly followed by an increase of 20 gammas in three minutes. Disturbed conditions prevailed for 24 hours.
International Union of Geodesy and Geophysics, Meeting in Washington, September 4–15, 1939 International Association of Terrestrial Magnetism and Electricity
Authors: Goldie A. H. R. 
Published: February 2008

Provisional outline of the discussionsI—Address of President: Trends of Research in Terrestrial Magnetism and Electricity (Friday, September 8, at 14.30)II—Report of Secretary and Director of Central BureauIII—Report of Dr. van Dijk on the publication of numerical magnetic character of daysIV—FinancesV—Election of officers of the AssociationVI—National reportsVII—Reports of Committees and Reporters appointed at the Edinburgh AssemblyVIII—Polar Year 1932–33—(1) Report on the activity of the Polar Year Commission of the International Meteorological Organization; (2) Discussion of International Polar Year resultsIX—Communications on miscellaneous subjectsX—Subjects for discussion during the AssemblyXI—Subjects for joint discussion with the Association of MeteorologyXII—Subjects for deliberation by Committees (subjects requiring world‐wide cooperation in work being done or planned)XIII—Appointment of Committees and ReportersXIV—Resolutions
The magnetic character of the year 1937 and the numerical magnetic character of the 1937
Authors: van Dijk G. 
Published: February 2008

The annual review of the “Caractère magnétique de chaque jour” for 1937 has been drawn up in the same manner as for the preceding years.1 Sixty‐two observatories contributed to the quarterly tables; fifty‐six 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.
The ionosphere at Huancayo, Peru, July, August, and September, 1938
Authors: Wells H. W. , Stanton H. E. 
Published: February 2008

This report on ionospheric conditions is in continuation of those published in preceding issues of this JOURNAL submitting results of continuous multifrequency ionospheric recordings at the Huancayo Magnetic Observatory. The current data for the quarter July to September, 1938, are obtained from recordings for each hour of the day and for every day of the month except for short intervals necessary for maintenance to the equipment.Table 1 contains mean hourly values of virtual height, critical frequency, and lowest frequency received. Figure 1 presents the data of Table 1 in graphical form. The following general discussion of characteristics is pertinent: