scholarly journals Total eclipse of the Sun, 1905, August 30. Preliminary account of the observations made at Sfax, Tunisia

1906 ◽  
Vol 77 (514) ◽  
pp. 28-41
Keyword(s):  
Solar Eclipse ◽  
Total Solar Eclipse ◽  
North Coast ◽  
The Sun ◽  
Total Eclipse ◽  
The North ◽  
Royal Observatory ◽  
Preliminary Account

An expedition to observe the total solar eclipse of August 30 having been sanctioned by the Admiralty, it was arranged, in concert with the Joint Permanent Eclipse Committee, that a party from the Royal Observatory should make observations at Sfax, a town on the north coast of Africa, about 150 miles south of Tunis. The programme of observations consisted of photographs of the corona on various scales for coronal detail and streamers, and photographs of the spectrum of the corona and chromosphere. The observers from Greenwich who took part in the expedition were Sir William Christie, Mr. Dyson, and Mr. Davidson. Professor Sampson, Mr. J. J. Atkinson, and Captain Brett, D. S. O., generously volunteered their assistance and shared the work of erecting and adjusting the instruments as well as of the observations on the day of the eclipse.

scholarly journals Total eclipse of the sun, 1901, May 18. Preliminary account of the observations made at Pulo Aoer Gadang, West Coast of Sumatra

1902 ◽  
Vol 69 (451-458) ◽  
pp. 235-247
Keyword(s):  
Solar Eclipse ◽  
West Coast ◽  
The Sun ◽  
The West ◽  
Total Eclipse ◽  
Royal Observatory ◽  
Preliminary Account

The Admiralty having approved of expeditions from the Royal Observatory to observe the Solar Eclipse of 1901, May 18, I was instructed by the Astronomer Eoyal to occupy a station on the West Coast of Sumatra with the instruments used at Ovar in the eclipse of 1900, May 28. Mr. J. J. Atkinson, who accompanied the Observatory expedition to Ovar, again generously volunteered his assistance and is associated with me in all the observations. His advice and co-operation were of the greatest value throughout.

scholarly journals Total eclipse of the sun, 1900, May 28. Preliminary account of the observations made at Ovar, Portugal

1901 ◽  
Vol 67 (435-441) ◽  
pp. 392-402
Keyword(s):  
Solar Eclipse ◽  
Large Scale ◽  
Total Solar Eclipse ◽  
Time Signal ◽  
The Sun ◽  
Structural Detail ◽  
Royal Observatory ◽  
Preliminary Account ◽  
Taking Charge ◽  
Daily Time

An expedition to observe the total solar eclipse of May 28 having been sanctioned by the Admiralty, it was arranged, in concert with the Joint Permanent Eclipse Committee, that the Royal Observatory party should take photographs of the corona on a large scale for structural detail, and on a smaller scale for the coronal streamers, and should also photograph the spectrum of the “flash” and of the corona. The programme thus naturally divided itself into two parts, Mr. Christie, assisted by Mr. Davidson, taking charge of the first part, and Mr. Dyson of the second. The party are much indebted to the Portuguese Government for the liberal arrangements made for the conveyance of the observers and their instruments in Portugal free of all charge to and from their observing station at Ovar, and for the great assistance rendered in erecting the instruments, and for a daily time-signal from the Lisbon Observatory direct to the observing station.

scholarly journals Total Eclipse of the Sun, 1901, May 18. Preliminary account of the observations made at the Royal Alfred observatory, Pamplemousses, Mauritius

1902 ◽  
Vol 69 (451-458) ◽  
pp. 247-261
Keyword(s):  
Solar Eclipse ◽  
General Structure ◽  
The Other ◽  
The Sun ◽  
The Moon ◽  
Total Eclipse ◽  
Royal Observatory ◽  
Preliminary Account ◽  
Coronal Streamers ◽  
The One

An expedition from the Royal Observatory to observe the Solar Eclipse of 1901 in the island of Mauritius having been sanctioned by the Admiralty, I was instructed by the Astronomer Royal to proceed to that island, there to act in concert with the Director of the Royal Alfred Observatory, Mr. T. F. Claxton, who had expressed his desire to co-operate in the observation of the eclipse. In accordance with a scheme approved by the Joint Permanent Eclipse Committee of the Royal and Royal Astronomical Societies, I took out with me two instruments belonging to the Royal Observatory, Greenwich, for photographing the corona; the one giving an image of the Moon 2·4 inches in diameter, and intended to secure the general structure of the corona, and the other giving an image 0·3 inch in diameter, and intended to secure the outer coronal streamers.

scholarly journals Total solar eclipse, 1905, August 29-30. Preliminary report of the observations made at Guelma, Algeria

1906 ◽  
Vol 77 (514) ◽  
pp. 56-76
Keyword(s):  
Solar Eclipse ◽  
Royal Society ◽  
Preliminary Report ◽  
Total Solar Eclipse ◽  
The South ◽  
Royal Astronomical Society ◽  
The North ◽  
Royal Observatory ◽  
The Government ◽  
Government Grant

The expedition to which this report refers was one of those organised by the Joint Permanent Eclipse Committee of the Royal Society and the Royal Astronomical Society; it was supported by a grant made by the Government Grant Committee. Guelma was chosen for the site of the observations, as being an inland station between Sfax, which was selected for an expedition from the Royal Observatory, Greenwich, and Philippeville, which it was at first expected Sir Norman Lockyer would occupy. Guelma is 58 kilometres from Bona, 65 kilometres from Philippeville, 55 kilometres from the nearest coast of the Mediterranean Sea; it lies at a height of about 1200 feet above sea-level on the south side of the Valley of the Seybouze, amongst hills which range in height from about 3100 feet at 13 kilometres to the north, to about 4700 feet at 11 kilometres on the south, where lies the celebrated mountain, Mahouna, “the sleeping lady,” so called from the resemblance of its silhouette to the form of a woman. (For the position of the observing hut, see p. 59.)

scholarly journals XXXIV.—On the Total Solar Eclipse of 1851

1853 ◽  
Vol 20 (3) ◽  
pp. 503-511
Author(s):  
C. Piazzi Smyth
Keyword(s):  
Solar Eclipse ◽  
Physical Characteristics ◽  
Total Solar Eclipse ◽  
The Other ◽  
The Sun ◽  
Total Eclipse ◽  
Crucial Test

Eclipses are still, as they have ever been, very important phenomena for the astronomical observer; partly on account of the crucial test which they afford for the examination of the truth of the theory and calculation of the motions, real and apparent, of the Sun and Moon, partly also for the special opportunities which they furnish of inquiring into some of the arcana of the physical characteristics of those bodies.For the former purpose, a partial eclipse will serve almost as well as a total one; while the continued improvement of the observation of meridian passages is now raising these daily measures fully to the importance of the other occasional phenomena, as a test of the theory. But for inquiry into the physics of the Sun, a perfectly total eclipse of that body is necessary; revelations may then happily be procured, which no observation of any other phenomena at any other time, can hope to afford any suspicion of.

scholarly journals A Fix by Total Solar Eclipse

1954 ◽  
Vol 7 (4) ◽  
pp. 402-404
Author(s):  
D. H. Sadler
Keyword(s):  
Solar Eclipse ◽  
Total Solar Eclipse ◽  
Circular Cone ◽  
The Sun ◽  
The Moon ◽  
Total Eclipse ◽  
The Earth

A total eclipse of the Sun provides an opportunity, rare though it may be, of obtaining an instantaneous fix from the Sun alone. Eclipses vary greatly in character, in position on the Earth, in the width of the path of totality, in the duration, and also in the direction of the path. However, the shadow of the Moon cast by the Sun is always a right circular cone which, in the case of a total eclipse, intersects the Earth's surface at some point before its vertex. Owing to the motion of the Moon in its orbit round the Earth the shadow moves at a speed of about 2000 m.p.h. from west to east (it varies considerably according to the distance of the Moon from the Earth).

scholarly journals The Astronomical Event of the Decade: Library Opportunities with the Coming Total Eclipse of the Sun

2017 ◽  
Vol 15 (1) ◽  
pp. 33
Author(s):  
Andrew Fraknoi ◽  
Dennis Schatz
Keyword(s):  
United States ◽  
Solar Eclipse ◽  
The United States ◽  
Total Solar Eclipse ◽  
The Sun ◽  
The Moon ◽  
Total Eclipse

On August 21, 2017, we will be treated to the first total eclipse of the sun visible in the continental United States in almost forty years. Because the total eclipse can only be seen in the United States, it is being called the “All American Total Solar Eclipse.” In this kind of eclipse, the Moon gets in front of the sun in the sky and blocks its light.

A Fix by Total Solar Eclipse

1999 ◽  
Vol 52 (2) ◽  
pp. 296-299
Author(s):  
D. H. Sadler
Keyword(s):  
Solar Eclipse ◽  
Total Solar Eclipse ◽  
Maximum Effect ◽  
The Sun ◽  
The Moon ◽  
Short Article ◽  
Total Eclipse ◽  
The Earth ◽  
Total Phase ◽  
February Issue

In anticipation of the TOTAL Solar Eclipse on 11 August 1999 (see the January/February issue of Navigation News), it seemed very appropriate to repeat this short article by one of the Institute's most respected Fellows. It was first published in Vol. VII, October 1954.A TOTAL eclipse of the Sun provides an opportunity, rare though it may be, of obtaining an instantaneous fix from the Sun alone. Eclipses vary greatly in character, in position on the Earth, in the width of the path of totality, in the duration, and also in the direction of the path. However, the shadow of the Moon cast by the Sun is always a right circular cone which, in the case of a total eclipse, intersects the Earth's surface at some point before its vertex. Owing to the motion of the Moon in its orbit round the Earth, the shadow moves at a speed of about 2000 m.p.h. from west to east (it varies considerably according to the distance of the Moon from the Earth). The intersection of this cone with the Earth's surface is an ellipse, which moves over the surface at speeds which are very high when the cone is nearly tangential (i.e. when the Sun's altitude is low) and at speeds as low as about 1000 m.p.h., when the eclipse is central over the equator at noon and the Earth's rotation has its maximum effect. The speed of the shadow is generally low enough to give a position line of considerable accuracy from the observed time of either second or third contacts, that is the beginning or ending of the total phase. An error of 1 second corresponds, in the most favourable case, to about one-third of a mile. The position line is, of course, the portion of the elliptic shadow corresponding to the observed phase and time; these can be precomputed.

XVII. On the measurement of the chemical intensity of total daylight made at Catania during the total eclipse of Dec. 22nd,1870

1871 ◽  
Vol 161 ◽  
pp. 467-476
Keyword(s):  
Solar Eclipse ◽  
Total Solar Eclipse ◽  
The Sun ◽  
Special Series ◽  
Total Eclipse ◽  
John Herschel ◽  
Primary Object ◽  
Subsequent Calculation ◽  
Photochemical Action

The following communication contains the results of a series of measurements of photochemical action made at Catania in Sicily, on Dec. 22nd, 1870, during the total solar eclipse of that date, with the primary object of determining experimentally the relation existing between this action and the changes of area in the exposed portion of the sun’s disk. The attempt to establish this relation has already been made by one of us from the results of observations carried out by Captain John Herschel, R. E., F. R. S., at Jamkhandi, in India, during the total eclipse of August 18th, 1868. Unfortunately the weather at Jamkhandi at the time of the eclipse was very unfavourable for observation; the estimated amount of cloud during the time of the eclipse amounted to about 7, the sun occasionally being even completely obscured. In addition to the errors arising from the unsettled state of the weather, a further element of uncertainty was unavoidably introduced in the subsequent calculation in allowing for the variation in chemical intensity caused by the alteration in the sun’s altitude during the progress of the eclipse. It has been shown that the relation between the sun’s altitude and the chemical intensity at any given place is represented by the equation CI a = CI 0 + const. × a , where CI a signifies the chemical intensity at any altitude ( a ) in circular measure, CI 0 the chemical intensity at 0°, and const, a a number derived from the observations. Since no special series of observations were made at Jamkhandi (lat. 16° 30' N.) in order to determine the constant, its approximate value could only be obtained from observations made at Pará, in Brazil (lat. 1° 25' S.), during a different season of the year.

scholarly journals I. Report of the observations of the total solar eclipse of August 29, 1886, made at Carriacou

1887 ◽  
Vol 42 (251-257) ◽  
pp. 316-318
Keyword(s):  
Solar Eclipse ◽  
West Indies ◽  
Royal Society ◽  
Total Solar Eclipse ◽  
Small Island ◽  
Small Islands ◽  
The West ◽  
The North

Carriacou is a small island situated about twenty miles to the north of the island of Grenada, the chief of the Windward group, and furnished an excellent site for the observation of the last solar eclipse. Most of the observers sent by the Eclipse Committee of the Royal Society to the West Indies in August of last year remained at Grenada, or on the small islands in its immediate vicinity, whilst Mr. Maunder and myself occupied the more distant northern station, where the totality was slightly diminished in duration. The work proposed for Mr. Maunder was to secure a series of photographs of the corona, with exposures of 40s. and under, and also to obtain two photographs of the spectrum of the corona with the longest exposures possible.

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