bluuebunny/crossref_metadata_2025_split huggingface dataset:
Study of cosmic rays between New York and Chile
Authors: Berry Edward B. , Hess Victor F. 
Published: February 2008

A Compton Model‐C cosmic‐ray meter aboard the S.S. Santa Ana measured cosmic‐ray intensities between New York and Valparaiso from September, 1940, to February, 1942. The hourly deflections of the electrometer‐needle, recorded photographically, were measured and the computed cosmic‐ray intensities corrected for barometric pressure with a coefficient K = −1.74 per cent per cm mercury. After reduction to 30 inches of mercury, they were grouped into 2°.5 intervals of geomagnetic latitude with the corresponding mean temperatures and temperature‐coefficients for the various latitudes determined. The variation of intensity of ionization with geomagnetic latitude was then plotted, showing a latitude‐effect of 8.3 per cent. A longitude‐effect of 1.5 per cent between geographic longitudes 75° west and 145° west was also found.The curve of temperature‐coefficients was found to be symmetrical about 23° north geomagnetic latitude in contrast to a similar curve of P. S. Gill for the Pacific, which is symmetrical about the geomagnetic equator.Variations of cosmic radiation during the magnetic storm of March 1, 1942, are plotted and show the same characteristics and order of magnitude as those reported by other observers.
Sitka Magnetic Observatory, January to March, 1943
Authors: Pinckney Harold W. 
Published: February 2008

(Latitude 57° 03′.0 N., longitude 135° 20′.1 or 9h 01m.3 W. of Gr.)January 20–21—Commencing with an increasing bay in D at 21h 05m GMT, January 20, a moderate disturbance continued through 07h, January 21. Ranges: D, 71′; H, 565 gammas; Z, 577 gammas.
Magnetic Observatory, Hermanus, January to March, 1943
Authors: Ogg A. 
Published: February 2008

(Latitude 34° 25′.2 S., longitude 19° 13′.5 or 1h 16m.9 E. of Gr.)January 1–5—There was a small sudden‐commencement disturbance at 15h 30m GMT, January 1. At the beginning of the disturbances, which continued until 21h, January 5, the ranges were very small, but after 08h 30m, January 4, the magnetic activity increased. The greatest .K‐index was 5 for the periods 12h to 15h and 18h to 21h, January 4, and 09h to 15h and 18h to 21h, January 5. There were micropulsations on all traces from 01h 45m to 02h 00m, January 3.
CHELTENHAM MAGNETIC OBSERVATORY JULY TO SEPTEMBER, 1943
Authors: Hershbebger John 
Published: February 2008

(Latitude 38° 44′.0 N., longitude 76° 50′.5 or 5h 07m.4 W. of Gr.)July 4‐6—A moderate disturbance yielding two K‐indices of 6 began at about 12h GMT, July 4, and lasted approximately forty‐eight hours. Intermittent minor activity continued for more than a week.
Cheltenham Magnetic Observatory, October to December, 1943
Authors: Hershberger John 
Published: February 2008

Latitude 38° 44′.0 N., longitude 76° 50′.5 or 5h 07m.4 W. of Gr.]October 24–31—A period of minor disturbance began in the fourth three‐hour period of October 24 (GMT), and continued to the end of the month. Four K‐indices of 6, and sixteen of 5, were scattered throughout the period.
Tucson Magnetic Observatory, October to December, 1943
Authors: Wilson R. M. 
Published: February 2008

Latitude 32° 14′.8 N., longitude 110° 50′.1 or 7h 23m.3 W. of Gr.]September 27–October 4—The September part of this storm was described in the last report. The moderate storm or series of storms that began at about 00h GMT, September 27, continued until about 11h, October 4. Moderately severe storm‐conditions prevailed from 00h, September 30, to 05h, October 1, also from 23h, October 1, to 03h, October 2, and from 23h, October 2; to 11h, October 3. The other periods of the storm were characterized by irregular variations of D and H without unusually prominent maxima and minima. Ranges: D, 22′,5; H, 166 gammas; Z, 36 gammas.
Watheroo Magnetic Observatory, January to March, 1944
Authors: Parkinson W. C. 
Published: February 2008

(Latitude 30° 19′.1 S., longitude 115° 52′.6 or 7h 43m.5 E. of Gr.)February 7–8—This small disturbance began at about 05h GMT, February 7. There was no sudden commencement, but the traces gradually became more disturbed, reaching their greatest activity at 12h 50m when there were large peaks in D and Z and a considerable bay in H until 13h 26m. During this interval the range in H was 103 gammas, in D 11′.5, and in Z 99 gammas. There was a smaller series of peaks and bays between 15h and 16h 30m; however apart from this feature the disturbance gradually subsided until normal conditions again prevailed at 24h February 8. Ranges: D, 20′.0; H, 113 gammas; Z, 147 gammas.
Hermanus Magnetic Observatory, October to December, 1943
Authors: Ogg A. 
Published: February 2008

(Latitude 34° 25′.2 S., longitude 19° 13′.5 or 1h 16m.9 E. of Gr.)October 1–5—The disturbances which began at midday of Greenwich date September 26 continued until midday October 5. During the period from October 1 to October 5 the maximum K‐index was 5 for each of the three‐hour periods 12h–15h, October 1, and 12h–5h and 18h–21h, October 2.
C. Coleridge Farr, 1866–1943
Authors: Macleod D. B. 
Published: February 2008

Dr. C. Coleridge Farr, F.R.S., for 30 years a member of the Canterbury Branch of the Royal Society of New Zealand, and an original Fellow of the Society, died on January 27, 1943.Farr was born in Adelaide on May 22,1866. His father, the Venerable Archdeacon Farr, LL.D. (Cantab.), was, at the time, headmaster of St. Peter's College, the leading Boys' College in Adelaide. After receiving his early education at his father's school, Dr. Farr proceeded to Adelaide University. It was his good fortune that Sir William Bragg was Professor of Mathematics and Physics. Farr remained a lifelong friend of Sir William and his family, and he was fond of recalling that he had often nursed on his knee Professor W. H. Bragg, at present the Cavendish Professor of Physics at Cambridge.
Sitka Magnetic Observatory, July to September, 1944
Authors: Pinckney Harold W. 
Published: February 2008

(Latitude 57° 03′.0 N., longitude 135° 20′.1 or 9h 01m.3 W. of Gr.)August 2–3—Climaxing a three‐month period of unusual calm a fairly severe storm began gradually about 21h GMT, August 2, accelerated at 24h, and diminished sharply in intensity after 11h, August 3. A maximum positive departure from normal of 625 gammas occurred in horizontal intensity at 03h 32m and K‐indices of 7 were recorded for the first three periods of August 3. Most of the action on D took the form of rather long‐period oscillations.
Huancayo Magnetic Observatory, January to March, 1945
Authors: Jones Mark Wallon 
Published: February 2008

(Latitude 12° 02′.7 S., longitude 75° 20′.4 or 5h 01m.4 W. of Gr.)January 15— There was a short disturbance characterized by a sharp beginning at 18h 00m GMT, January 15. There was a high peak in H at 18h 07m, which was followed by numerous peaks and bays with a deep bay at 18h 47m. The disturbance was over by 19h 40m, D and Z showing only mild variations. The K‐index of 6 covered the variation. Range: H, 307 gammas.
Tucson Magnetic Observatory April to June, 1945
Authors: Nelson J. H. 
Published: February 2008

(Latitude 32° 14′.8 N., longitude 110° 50′.1 or 7h 23m.3 W. of Gr.)April 1–2—A moderate magnetic storm of only twenty‐four hours' duration began at 05h GMT, April 1. There was marked activity of fairly short period during the first ten hours, which were followed by a period of mild disturbance until the end of the storm. Ranges: D, 15′; H, 110 gammas.
Hermanus Magnetic Observatory April to June, 1945
Authors: Ogg A. 
Published: February 2008

(Latitude 34° 25′.2 S., longitude 19° 13′.5 or 1h 16m.9 E. of Gr.)April 1—A small sudden‐commencement storm began at 04h 59m GMT, April 1, and continued for about twenty‐four hours. The range of H was 136 gammas and the maximum K‐index was 5, period 15h‐18h.
Annual variation of the values at noon of the critical frequencies of the ionized layers at Tromsö during 1940, 1941, 1942, 1943, and 1944
Authors: Harang Leiv 
Published: February 2008

In previous notes the monthly mean values of the critical frequencies of the ionized layers have been given beginning with 1935. In the following the mean monthly values of the critical frequencies determined at local noon will be given. As the station Tromsö is situated near the auroral zone, the conditions of the ionosphere are strongly influenced by the frequent geomagnetic storms, and the echoes are often lacking during disturbed periods due to increased absorption, or more or less irregular echoes appear, which sometimes make a precise critical‐frequency determination difficult.Because of the war it has not been possible to take the observations so regularly as previously, and for some months the number of daily observations are not sufficient to give reliable monthly means. In 1940 the observations had to be stopped on April 10, as the antennas had to be removed due to bombing in the vicinity. The observations could not be resumed until July, 1940. In December, 1944, the antennas had again to be removed.
Noise during radio fade‐outs
Authors: Ferrell Oliver Perry 
Published: February 2008

The interesting communication from J. M. Watts [Terr. Mag., 51, 122–125 (1946)] regarding a form of solar hiss or noise during radio wave, fade‐outs has been brought to my attention. In preparing a bibliography of the effects of radio‐wave propagation above 30.0 Mc/sec, I have found the following previous references of this noise which may prove of interest or value to other investigators.Some casual mention is made of the noise accompanying radio fade‐outs by Dr. J. H. Dellinger who coordinated many of the random radio fade‐out observations. D. Arakawa [Abnormal attenuation in short‐wave propagation, Reports of Radio Research in Japan 6, No. 1 (1936)] appears to have made the first concise investigations and mentions the noise on the point‐to‐point communication circuits from Manila to Tokyo during radio fadeouts. It also seems worthy of mention that a lone British radio amateur observed this type of hiss during fade‐outs between 40.0 and 60.0 Mc/sec, in 1937.
Tucson Magnetic Observatory April to June, 1946
Authors: Nelson James H. 
Published: February 2008

(Latitude 32° 14′.8 N., longiude 110° 50′.1 or 7h 23m.3 W. of Gr.)April 14–15—A moderate disturbance began about the middle of the Greenwich day April 14, with small activity of fairly short period. Activity increased slightly about 01h GMT, April 15. The period of disturbance ended about 20h, April 15. Ranges: D, 15′; H, 94 gammas.
Suggestions for reprinting articles of historic interest in geomagnetism
Authors: Mitchell A. Crichton 
Published: February 2008

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

0n January 16, 1947, at his home in Christchurch, New Zealand, Henry Fawsit Skey, a former Director of the Christchurch Magnetic Observatory, died suddenly from a heart attack which overcame him just before noon whilst he was having a cup of tea with his wife.He was born in April, 1877, at Dunedin, New Zealand, where he attended the Otago Boys' High School, and later the Otago University. There he gained a senior scholarship, and next year graduated with honors in Physics.
Sitka Magnetic Observatory January to March, 1947
Authors: Campbell Joel B. 
Published: February 2008

(Latitude 57° 03′.0 N., longitude 135° 20′.1 or 9h 01m.3 W. of Gr.)January 2–6—An extended period of moderately disturbed conditions was recorded during the first few days of January. The disturbance began gradually at about 08h 30m GMT, January 2, and continued until about 16h 00m, January 6. Activity consisted chiefly of variations of rather large amplitude and long period forming small bays throughout the storm. One K‐index of 6 was recorded near the beginning of the disturbance and four K‐indices of 5 were recorded just before the end.
Report of temporary Sub‐Commission on liquidation of agenda of the International Commission for the Polar Year 1932–1933
Authors: Fleming J. A. , Keränen J. , Stagg J. M. , Thomson A. 
Published: February 2008

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

(Latitude 18° 38′.3 N., longitude 72° 52′.3 or 4h 51m.5 E. of Gr.)July 17–18—A storm of great intensity commenced suddenly at 17h 48m GMT, July 17, with an unusually large increase of 109 γ in H, a decrease of 27 γ in Z, and an increase of 1′.3 in westerly declination. After a period of intense activity lasting for about three hours, all three elements became fairly steady until about 03h 15m, July 18, when rapid fluctuations began to be recorded continuously until about 11h 15m. A crochet of the type usually associated with a solar flare was also recorded on all the magnetograms at 10h 37m, July 17. The storm ended at about 20h, July 18, giving K‐indices one each of 8, 7, and 6 and two of 5. Ranges: D, 8′.5; H, 298 γ; Z, 62 γ.
Statistics of heights of various auroral forms from Southern Norway: Second communication
Authors: Störmer Carl 
Published: February 2008

(1) Introduction—In a short paper published in this Journal in December, 1946, I gave the results of 12,330 measurements of height of polar aurora observed in Southern Norway during 1911–44. The present paper deals with the statistical work undertaken since that publication.If we compare the diagram of height (Fig. 1) in the above‐mentioned paper with the corresponding one from my expedition to Northern Norway in 1913 [see 1 of “References” at end of this paper], one of the essential differences is that the aurora in Southern Norway occur at much greater heights than those in Northern Norway. There are two reasons for this. First, certain aurora occurring in the Earth's shadow during years of great solar activity as rays and red diffuse surfaces [2], often reach great heights (from 300 to 700 km) and are seldom observed in Northern Norway. Second, the auroral rays in that part of the atmosphere lying in sunshine—which have only once been measured in Northern Norway [3]—have a position very much higher than aurora in shadow, as already pointed out in my paper on sunlit auroral rays published in 1929 [4]. This difference is clearly seen in Figure 1, where the 12,330 heights from my first paper of 1946 are split into heights of aurora in shadow (left) and aurora partly or completely in sunlight (right) [5]. For each kilometer the measured heights are distributed as points along the corresponding horizontal line at approximately equal distances. The same remark applies to the other Figures in this paper.
Apia Observatory April to June, 1948
Authors: Gerard V. B. 
Published: February 2008

(Latitude 13° 48′.4 S., longitude 171° 46′.5 or 11h 27m.1 W. of Gr.)April 6–7—A sudden commencement of 18 gammas in H at 03h 58m GMT, April 6, introduced a period of mild disturbance lasting until 16h 51m when a large positive bay in H, with rapid irregular oscillations superimposed, commenced. The bay lasted until 18h 22m and was terminated by a rapid fall of 42 gammas in H over a period of ten minutes. Further rapid oscillations continued to about 08h 30m, April 7, with minor activity persisting for some hours afterwards. K‐index 5 was recorded during the sixth and seventh three‐hour periods of April 6.
A summary of the results of the recent magnetic survey of Great Britain and Ireland conducted by professors Rücker and Thorpe: Part I. On the accuracy of the delineation of the terrestrial isomagnetic lines
Authors: Rücker A. W. 
Published: February 2008

My friend Dr. Thorpe and I have completed a Magnetic Survey of the United Kingdom of Great Britain and Ireland, of which a full account has recently been published in the Transactions of the Royal Society. I do not propose in this article to give a detailed description of our work, but there are certain points which we have been able to discuss with unusual fulness, an account of which may be interesting.observations have been made by us or under our direction at 882 places in the British Isles. There is therefore one station to every 139 square miles of land area.
On the distribution of magnetic observatories over the globe
Authors: Schmidt Adolf 
Published: February 2008

The first and most important object being to investigate the main features of terrestrial magnetism in its totality, the points of observation evidently should be disposed as uniformly as feasible. This holds, whatever general problem may be pursued: that of establishing the average magnetic condition, or the secular variation; of observing regular oscillations or disturbances. For special problems, which certainly should not be neglected, but are, in immediate importance, second to the main problem, it may be desirable or necessary to condense stations in certain localities, but it is not here contemplated to enter upon the discussion of special questions.The existing observatories are far from satisfying the above demand. The great majority are on European ground; i. e., within
of the earth's surface. Of the others, the southern hemisphere contains three, none of them south of lat. 38°. The immense surface of the Pacific, too, is entirely devoid of them. The defects of this arrangement, though they have less influence in the case of phenomena (as e.g., the daily variation), which depend mainly, though not entirely, on latitude, become more noticeable, as the phenomena vary likewise in longitude. It is immaterial whether the results of the observatories be treated simply statistically and comparatively, or a generalization be attempted graphically or by computation. The one way or the other may be better adapted to the individual problem, yet upon the selection of the particular method to be employed can not depend the maximum reliability of the results deduced from the available data in a given case. The lack of uniformity in the distribution of magnetic stations would lead us to expect rather uncertain conclusions with regard to the earth's magnetic action, unless in a special case some law should appear simple and undisturbed. For this very reason, on the other hand, a marked improvement in the results might be hoped for, by a judicious disposition of but a few stations within the area not covered hitherto.
Erdmagnetische Observatorien und Electrische Bahnen
Authors: Eschenhagen M. 
Published: February 2008

Bei der grossen Ausbreitung, welche in neuester Zeit der Betrieb elektrischer Bahnen im Stadtverkehr, sowie auch zur Verbindung mehrerer Orte unter einander gewinnt, scheint die Zeit nicht mehr fern, dass die Beobachtungen der erdmagnetischen Erscheinungen durch jene Betriebe mindestens sehr beeinträchtigt, wenn nicht ganz verhindert werden.Zu Washington und Toronto (Canada) ist dies bereits der Fall, wahrend in Deutschland eine ganze Reihe physikalischer Universitäts‐Institute an der Ausführung magnetometrischer Messungen verhindert und die Beobachtungen an Galvanometern wesentlich auf unempfindliche Instrumente beschränkt sind.
Discussion of ‘Mathematical Assessment of Synthetic Hydrology’ by N. C. Matalas
Authors: Young G. K. 
Published: February 2008

I wish to comment on the paper by N. C. Matalas, ‘Mathematical Assessment of Synthetic Hydrology,’ with regard to calculating the coefficients of equation 13.Assume that the cells of M0 and M1 are directly derived from data. This implies thatA may be found using equation 16, which leaves the solution of B as the item of interest. Define C = M0 − M1M0−1M1t; thus, C = BBt. Matalas demonstrates that B is not unique. The fact that C is symmetric permits a simple and direct solution for B, which avoids the application of principal component analysis.
Further to the Hydrologic Importance of Transpiration Control by Stomata
Authors: Van Bavel C. H. M. 
Published: February 2008

An exchange of views on the above subject [Idso, 1968; Lee, 1968] revolves principally around results of several experiments carried out by me and former colleagues. Some clarifying comments appear in order, since all relevant details were not published.A general view must admit that, together with a number of internal and external conditions, leaf stomata determine the rate of transpiration. From a hydrologie or an engineering view, however, what matters is whether this role is of consequence. The issue can be settled only by a study of the transpiration from naturally exposed canopies of vegetation, of their atmospheric environment and, simultaneously, of the transpiration resistance of the leaves. Generalities derived from theoretical or simulation studies cannot supply the answer, and I agree completely with similar comments made by Idso [1968]. Experiments in which vegetation is wetted by rain or artificially cannot be used as evidence, unless the complete energy balance is simultaneously studied. Experiments involving singly exposed individual plants cannot inform us by simple analogy about the transpiration of natural stands.