RADIO OBSERVATIONS ON THE UPPER IONIZED LAYER OF THE ATMOSPHERE AT THE TIME OF THE TOTAL SOLAR ECLIPSE OF AUGUST 31, 1932

1933 ◽  
Vol 8 (1) ◽  
pp. 15-28
Author(s):  
D. C. Rose
Keyword(s):  
Solar Eclipse ◽  
Research Council ◽  
Short Pulse ◽  
Time Lag ◽  
National Research Council ◽  
Ultra Violet ◽  
Total Solar Eclipse ◽  
Ion Content ◽  
Violet Light ◽  
Set Up

This report contains the results from one of the three stations set up by the National Research Council of Canada to take observations on radio reflections from the ionized layers in the upper atmosphere during the total solar eclipse of August 31, 1932. The station concerned was located at Kingston, Ontario, and was approximately under the centre of totality for the upper or Appleton layer. Hence observations at this station were limited to the upper layer. The results from the other two stations at Corner Brook, Newfoundland, and at Vankleek Hill, Ontario, are reported in the paper immediately preceding (8).The method was that developed by Breit and Tuve, in which a short pulse is transmitted, the reflection being received and its time delay recorded by means of a cathode ray oscillograph.The results indicate that the ionization of the upper layer is caused by radiation (presumably ultra-violet light) from the sun. Whether or not this is the sole cause is uncertain because of the time lag in recombination of ions in the layer. A reduction in ionization of over 30% was noted.A magnetic storm which occurred a few days before the eclipse made the results more difficult to interpret but gave some information of the effect of such a storm on the upper layer. It appeared to cause considerable instability in the layer and a somewhat lower ion content.

MEASUREMENTS OF IONIZATION IN THE KENNELLY-HEAVISIDE LAYER DURING THE SOLAR ECLIPSE OF 1932

1933 ◽  
Vol 8 (1) ◽  
pp. 1-14 ◽  
Author(s):  
John T. Henderson
Keyword(s):  
Solar Eclipse ◽  
Marked Effect ◽  
Lower Layer ◽  
Ultra Violet ◽  
Total Solar Eclipse ◽  
The Sun ◽  
Effective Height ◽  
Ultra Violet Light ◽  
Violet Light ◽  
Sudden Decrease

The ionization of the Kenelly-Heaviside layer was measured by Appleton's method during the total solar eclipse of August 31, 1932. In contrast to normal days, a sudden decrease of 58% during the period of optical totality was found. This is shown to be in accord with Appleton's, but not with Chapman's, theory that the cause of lower layer ionization is ultra-violet light from the sun. Some measurements were made of the effective height of the Appleton layer and these are discussed in detail. There is a marked effect at the time of optical totality on this layer also.

scholarly journals Internet-Based Administration of Shared Instruments with Facility Online Manager

2006 ◽  
Vol 14 (6) ◽  
pp. 36-39
Author(s):  
Shu-You Li ◽  
Vinayak P. Dravid
Keyword(s):  
Resource Sharing ◽  
Research Council ◽  
Scientific Research ◽  
National Research Council ◽  
Research Area ◽  
Research Groups ◽  
Principal Investigators ◽  
Materials Research ◽  
Set Up ◽  
Large Research

Resource sharing has become an absolute necessity for modern scientific research because of the increasing expense and complexity of instruments, and the ever changing funding paradigm which often requires sharing of major instrumentation resource across multiple disciplines. Many universities and even large companies have set up centralized facilities to serve researchers from different departments, divisions and units to minimize expenses and maximizing usage.Just in the materials research area alone, it is estimated that there are more than 500 mid-size facilities existing nationwide, as reported in 2005 by the Committee on Smaller Facilities of National Research Council. Resource sharing is also common in large research groups, between Principal Investigators, as well as in corporate/industrial laboratories.

scholarly journals Some further measurements of upper atmospheric ionization

1935 ◽  
Vol 150 (871) ◽  
pp. 685-708 ◽  
Keyword(s):  
Solar Eclipse ◽  
Seasonal Variations ◽  
Critical Frequency ◽  
Ultra Violet ◽  
Frequency Method ◽  
Ultra Violet Light ◽  
Violet Light ◽  
South East England ◽  
Atmospheric Ionization ◽  
Maximum Ionization

In a previous communication an account was given of some measurements of upper atmospheric ionization in south-east England made by the critical frequency method. These measurements were confined principally to the Kennelly-Heaviside region (region E) and showed that the maximum ionization at that level in the ionosphere exhibits a diurnal and seasonal variation such as may be explained in terms of a solar ionizing agency travelling rectilinearly. It was found, for example, that the ionization reaches a maximum about noon, falls off rapidly as sunset approaches, and continues to decrease less rapidly during the night. A short time before ground sunrise a minimum of ionization is attained, after which the value increases rapidly until the noon maximum is again reached. In the same communication reasons were advanced, based on the radio measurements made by one of us during the solar eclipse of 1927, for believing the ionizing agency for this region to be ultra-violet light from the sun, as opposed to the view then prevailing that a neutral stream of corpuscles was the effective agent, and it was pointed out that the solar eclipse of August 31, 1932, visible in Canada, provided an excellent opportunity for deciding the matter. Using the same critical-frequency method, Dr. J. T. Henderson working at Vankleek Hill, Ontario, was able to set the question beyond doubt and it may now be regarded as established that ultra-violet light is the principal ionizing agency for the Kennelly-Heaviside region. The present communication deals with further measurements made in south-east England by the critical-frequency method in which it is applied to the study of diurnal and seasonal variations in ionization in the upper ionized region (region F) as well as in region E. Since 1932, many workers in different parts of the world have adopted the critical-frequency method for the measurement of maximum ionization content and it is hoped that, in due course, the results of a world-wide survey of the diurnal and seasonal variations in ionospheric conditions will be available. Meanwhile, we are able to compare our present results with those we have previously obtained and also with those obtained in America at places of lower latitude.

scholarly journals L’EDIZIONE CARDANIANA DEL CONSIGLIO NAZIONALE DELLE RICERCHE; UN’OCCASIONE PERDUTA

2014 ◽  
Author(s):  
Enrico Isacco Rambaldi
Keyword(s):  
Critical Edition ◽  
Research Council ◽  
Systematic Approach ◽  
National Research Council ◽  
Philosophical Thought ◽  
Set Up ◽  
Consiglio Nazionale Delle Ricerche ◽  
Scientific Questions

The Cardano edition from the Consiglio nazionale delle ricerche has been a wasted opportunity. It shows the lack of an accurate systematic approach that led to the Cardano Project ending in fialure. The project had been fostered by the “National research council Center for the study of philosophical thought in the 16th and 17th centuries in relation to scientific questions”, set up by Mario Dal Pra. The aim had been for it to prepare a critical edition of the works of the doctor, mathematician, astrologist and philosopher Girolamo Cardano (Pavia 1501-Rome 1576).

scholarly journals Report on the total solar eclipse of 1911, April 28. (Observed the expedition of the joint permanent eclipse committee to Vavau, Tonga Islands, South Pacific.)

1912 ◽  
Vol 87 (595) ◽  
pp. 293-301 ◽  
Keyword(s):  
Solar Eclipse ◽  
Focal Length ◽  
Ultra Violet ◽  
South Pacific ◽  
Total Solar Eclipse ◽  
Small Scale ◽  
The Government ◽  
Flash Spectrum ◽  
Government Grant ◽  
Reasonable Prospect

1. General Arrangements . The expedition to observe the total solar eclipse of 1911, April 28, was organised by the Joint Permanent Eclipse Committee, the expenses being defrayed by the Government Grant Fund. Of the few islands in the South Pacific crossed by the track of the moon’s shadow during totality, Vavau, one of the northernmost group of the Tonga or Friendly Islands, was the most suitable for observing the eclipse, the duration of totality being computed at 217 seconds, and there being a reasonable prospect of good weather. The programme of observations consisted of photographs of the corona on a large and relatively small scale for coronal detail and extension of the streamers, and photographs of the spectrum of the corona and of the lower chromosphere. For these purposes the expedition was furnished with a 4-inch photographic lens of 20 feet focal length, kindly lent by the Council of the Royal Irish Academy, and the 4-inch Dallmeyer “Abney” lens of 34 inches focal length. For the spectrum of the corona Prof. Newall kindly lent the quartz spectroscope of four prisms, presented to the Cambridge Observatory by Major Hills, in order further to investigate the ultra-violet spectrum. The fourth instrument was made up of a large 7-inch prism of 40° in combination with a 6-inch Dallmeyer portrait lens of 30 inches focal length, This objective prismatic camera gave a short but very bright spectrum, 4⋅5 cm. from H α to H ζ . The intention was to investigate the red end of the coronal spectrum on dyed plates, and incidentally to photograph the flash spectrum. The members of the expedition were Father Cortie and Mr. W. McKeon, from the Stonyhurst College Observatory, and Father E. Pigot, Director of the Observatory of St. Ignatius’ College, Rivervievv, Sydney, N. S. W., who also acted as agent for the expedition in Sydney, in the preparation of huts to cover the instruments, and in the gathering of materials for building the piers for the foundations. The Admiralty gave instructions that H. M. S. “Encounter” should convey the observers and the instruments from Sydney to Vavau and back, and that every assistance should be rendered to the expedition in the erection of the instruments and in the observations. The expedition is greatly indebted to Captain Colomb, and to the officers and men of the “Encounter,” for their enthusiastic co-operation in the work of the expedition.

scholarly journals The dynamics of surface boundary layer during total Solar eclipse 1995

MAUSAM ◽  
2021 ◽  
Vol 49 (4) ◽  
pp. 475-480
Author(s):  
S. ARULRAJ ◽  
T. DHARMARAJ ◽  
S. B. DEBAJE ◽  
A. BAGAVATH SINGH ◽  
K. G. VERNEKAR
Keyword(s):  
Boundary Layer ◽  
Wind Speed ◽  
Soil Temperature ◽  
Solar Eclipse ◽  
Total Solar Eclipse ◽  
Surface Boundary ◽  
Data Logger ◽  
Surface Boundary Layer ◽  
Set Up ◽  
Period Decrease

A microclimatological tower of 1.6 m height with six instrumented booms at different heights carrying wind speed, temperature and humidity sensors was set up at Robertsgun 24° 42'N, 83°4'E, 3l2m amsl) to study the implication of the total Solar eclipse on the dynamics of Atmospheric Boundary Layer (ABL). Apart from this, the soil temperature and heat flux were also measured during the same time. The observations were taken with a one minute average interval and recorded continuously with the data logger and then transferred to a PC for later use. The data were collected during 2l –26 October 1995. During the eclipse period decrease of surface temperature and soil temperature by 6.2°C and 3.5°C respectively and increase of humidity by nearly 60% were observed. Due to the decrease in velocity fluctuations, the mean wind speed showed the sharp increase compared to other days. The setting of stable atmosphere before the total solar eclipse was observed.

Paper Moon: Simulating a Total Solar Eclipse

2006 ◽  
Vol 99 (5) ◽  
pp. 312-320
Author(s):  
Seán P. Madden ◽  
James P. Downing ◽  
Jocelyne M. Comstock
Keyword(s):  
Mathematical Model ◽  
Solar Eclipse ◽  
Graphing Calculators ◽  
Total Solar Eclipse ◽  
Classroom Activity ◽  
Student Work ◽  
Set Up

This article describes a classroom activity in which a solar eclipse is simulated and a mathematical model is developed to explain the data. Students use manipulative devices and graphing calculators to carry out the experiment and then compare their results to those collected in Koolymilka, Australia, during the 2002 eclipse. Includes a description of how to set up the simulation and examples of student work.

Comparison of systems for estimating protein allowances for dairy cows

1987 ◽  
Vol 1987 ◽  
pp. 56-56 ◽  
Author(s):  
C.J. Waters ◽  
R.J. Dewhurst ◽  
A.J.F. Webster
Keyword(s):  
Milk Yield ◽  
Evaluation System ◽  
Research Council ◽  
Agricultural Research ◽  
National Research Council ◽  
Working Party ◽  
Dairy Herd ◽  
Previous Treatment ◽  
Two Systems ◽  
Set Up

The proposed Agricultural Research Council (ARC 1984) protein evaluation system for ruminants provides lower nitrogen allowances than any other. (National Research Council 1985; Alderman 1987). A U.K. Interdepartmental Working Party (IDWP) was set up to consider the ARC (1980) proposals and recommend a practical protein evaluation system for ruminants for use by the advisory services. Its provisional proposals have been reported by Webster (1987). This trial was set up to provide a practical evaluation of the two systems in a commercial dairy herd.Animals. Thirty-three Friesian cows (mean livewewight 590kg, mean previous milk yield 6120 kg), in early lactation were blocked according to (a) previous treatment, (b) number of previous lactations and (c) previous milk yield. The cows were randomly allocated within blocks to one of three dietary treatments.Treatments. Dietary nitrogen allowances were calculated, according to (1) ARC(1984) and (2) IDWP (Webster, 1987) except that the ARC (1984) concept of essential amino acid nitrogen was included in the IDWP calculations. The difference in nitrogen allowances between the two systems was so great as to warrant a third intermediate treatment (INT), calculated to provide allowances mid-way between the other two.

scholarly journals 47. Observation of the solar eclipse of 30 June 1954 at 9·4 cm. wave-length

1957 ◽  
Vol 4 ◽  
pp. 269-272
Author(s):  
C. H. Mayer ◽  
R. M. Sloanaker ◽  
J. P. Hagen
Keyword(s):  
Solar Eclipse ◽  
Research Laboratory ◽  
Wave Length ◽  
Total Solar Eclipse ◽  
Naval Research Laboratory ◽  
Naval Research ◽  
Centre Line ◽  
Set Up ◽  
The City

The observation of the total solar eclipse of 30 June 1954 at 9·4 cm. wavelength was one of the experiments carried out by the Naval Research Laboratory eclipse expedition to Sweden. The apparatus was set up in the city of Oskarshamn at a point about 5 km. north of the centre-line of totality. At this location the eclipse was total, with magnitude 1·035, at 12h 48m u.t.

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