scholarly journals III. Spectroscopic observations of the sun.—No. IV

1869 ◽  
Vol 17 ◽  
pp. 415-418 ◽  
Keyword(s):  
Royal Society ◽  
The Sun ◽  
Spectroscopic Observations

I beg to lay before the Royal Society very briefly the results of observations made on the 11th instant in the neighbourhood of a fine spot, situated not very far from the sun’s limb. I. Under certain conditions the C and F lines may be observed bright on the sun , and in the spot-spectrum also, as in prominences or in the chromosphere. II. Under certain conditions, although they are not observed as bright lines, the corresponding Fraunhofer lines are blotted out.

scholarly journals V. Spectroscopic observations of the Sun.— No. III

1869 ◽  
Vol 17 ◽  
pp. 350-356 ◽  
Keyword(s):  
Royal College ◽  
Royal Society ◽  
The Sun ◽  
Spectroscopic Observations

Since my second paper under the above title was communicated to the Royal Society, the weather has been unfavourable to observatory work to an almost unprecedented degree; and, as a consequence, the number of observations I have been enabled to make during the last four months is very much smaller than I had hoped it would be. Fortunately, however, the time has not been wholly lost in consequence of the weather; for, by the kindness of Dr. Frankland, I have been able in the interim to familiarize myself at the Royal College of Chemistry with the spectra of gases and vapours under previously untried conditions, and, in addition to the results already communicated to the Royal Society by Dr. Frankland and myself, the experience I have gained at the College of Chemistry has guided me greatly in my observations at the telescope.

scholarly journals II. On the atmospheric lines of the solar spectrum, illustrated by a map drawn on the same scale as that adopted by Kirchhoff

1875 ◽  
Vol 23 (156-163) ◽  
pp. 201-202
Keyword(s):  
Sea Level ◽  
Royal Society ◽  
Solar Spectrum ◽  
The Sun ◽  
Atmospheric Absorption ◽  
Spectroscopic Observations ◽  
Clear Atmosphere

The spectroscopic observations described in this paper were made with instruments belonging to the Royal Society, and in accordance with certain suggestions which had been made to the author by a committee appointed in consequence of a letter of his to Sir Edward Sabine, President, dated 13th February, 1866. In view of his residence at a considerable height above the sea-level, and of the exceedingly clear atmosphere prevailing at some periods of the year, it was suggested that the locality was peculiarly favourable for a determination of the lines of the solar spectrum due to atmospheric absorption, and that, for this purpose, the solar spectrum when the sun was high should be compared with the spectrum at sunset, and any additional lines which might appear in the latter case should be noted with reference to Kirchhoff’s map. Accordingly the author set to work with the spectroscope first supplied to him, and in the autumns of 1868 and 1869 mapped the differences in question from the extreme red to D. These results appeared in the 'Proceedings of the Royal Society' for June 16,1870, and the map of the spectra, sun high and sun low, of the region in question forms plate 1 of the 19th volume.

scholarly journals XX. Spectroscopic observations of the sun

1875 ◽  
Vol 165 ◽  
pp. 577-586
Keyword(s):  
Royal Society ◽  
The Sun ◽  
Spectroscopic Observations ◽  
The Temple ◽  
Made In

We have the honour to communicate to the Royal Society the accompanying Spectroscopic Observations of the Chromosphere and of the Sun generally, made during the period between the 1st October, 1872, and the 31st December, 1873. The London observations have been made in Alexandra Road, Finchley Road, N. W.; the Rugby observations in the Temple Observatory at that place. The following details are given of the instruments and methods of observation employed.

scholarly journals XII. Spectroscopic observations of the sun.—No. II

1869 ◽  
Vol 159 ◽  
pp. 425-444 ◽  
Keyword(s):  
Royal Society ◽  
The Sun ◽  
Spectroscopic Observations ◽  
Sun Spots

In my first paper under the above title, kindly communicated by Dr. Sharpey to the Royal Society in 1866, was contained an account of the determination of the nature of Sun-spots by means of the spectroscope. The paper concluded as follows:— “May not the spectroscope afford us evidence of the existence of the 'red-flames’ which total eclipses have revealed to us in the sun’s atmosphere, although they escape all other methods of observation at other times? and if so, may we not learn something from this of the recent outburst of the star in Corona?”

III. Spectroscopic observations of the sun

1867 ◽  
Vol 15 ◽  
pp. 256-258 ◽  
Keyword(s):  
The Other ◽  
The Sun ◽  
Chemical Action ◽  
Spectroscopic Observations ◽  
Gaseous Mass ◽  
Other Hand ◽  
Sun Spots ◽  
Physical Constitution ◽  
Upward Current

The two most recent theories dealing with the physical constitution of the sun are due to M. Faye and to Messrs. De la Rue, Balfour Stewart, and Loewy. The chief point of difference in these two theories is the explanation given by each of the phenomena of sun-spots. Thus, according to M. Faye, the interior of the sun is a nebulous gaseous mass of feeble radiating-power, at a temperature of dissociation; the photosphere is, on the other hand, of a high radiating-power, and at a temperature sufficiently low to permit of chemical action. In a sunspot we see the interior nebulous mass through an opening in the photosphere, caused by an upward current, and the sun-spot is black, by reason of the feeble radiating-power of the nebulous mass.

scholarly journals I.—Secular Earth-Creep

1909 ◽  
Vol 6 (4) ◽  
pp. 145-148 ◽  
Author(s):  
E. H. L. Schwarz
Keyword(s):  
South Africa ◽  
Diurnal Variation ◽  
Royal Society ◽  
The Sun ◽  
Special Design ◽  
Important Paper ◽  
Preliminary Results ◽  
Gravitational Pull ◽  
Set Up ◽  
Horizontal Pendulum

Dr. J. R. Sutton has recently read a most important paper to the Royal Society of South Africa on the diurnal variation of level at Kimberley. The paper gave the preliminary results of observations made during the course of three years upon the variation of the level of the ground as recorded by a large horizontal pendulum of a special design made for the author by the Cambridge Instrument Company. It appeared from the results that the movements in the surface of the ground, which set up corresponding movements in the pendulum, were very great. The maximum westerly elongation of the extremity of the pendulum occurred about 5.30 a.m., the maximum easterly about 4.15 p.m., the medium positions a little before 11 a.m. and 9.30 p.m. Geometrically these movements may be represented on the hypothesis that the hemisphere facing the sun bulges out, forming a sort of meniscus to the geosphere. The rise and fall of the surface of the ground which such a supposition would postulate is enormous, and the very magnitude has led Dr. Sutton to hesitate in giving the figures. There can, however, be very little doubt that some rise and fall in the earth's surface is occasioned by the sun's gravitational pull, although the present figures may have to be lessened by taking into consideration other causes which contribute to the disturbance of the pendulum.

scholarly journals XXXIV. On the transit of Venus in 1769. To the Right Honourable The Earl of Morton, President to the Council and Fellows of the Royal Society, this discourse is, with all humility, inscribed, by their humble servant, Thomas Hornsby

1765 ◽  
Vol 55 ◽  
pp. 326-344 ◽  
Keyword(s):  
Royal Society ◽  
The Sun ◽  
The Real ◽  
The Earth ◽  
Theory Of Gravity ◽  
The Right ◽  
Made In

The observations of the late transit of Venus, though made with all possible care and accuracy, have not enabled us to determine with certainty the real quantity of the sun's parallax; since, by a comparison of the observations made in several parts of the globe, the sun's parallax is not less than 8" 1/2, nor does it seem to exceed 10". From the labours of those gentlemen, who have attempted to deduce this quantity from the theory of gravity, it should seem that the earth performs its annual revolution round the sun at a greater distance than is generally imagined: since Mr. Professor Stewart has determined the sun's parallax to be only 6', 9, and Mr. Mayer, the late celebrated Professor at Gottingen, who hath brought the lunar tables to a degree of perfection almost unexpected, is of opinion that it cannot exceed 8".

New Zealand, New Zealanders and the Royal Society

1994 ◽  
Vol 48 (2) ◽  
pp. 263-281 ◽  
Keyword(s):  
New Zealand ◽  
Royal Society ◽  
The Sun ◽  
Foreign Born ◽  
Future Health ◽  
Society Islands ◽  
James Cook ◽  
Group Of Seven ◽  
New Zealand Flora ◽  
Natural Historian

On 5 May 1768 Lieutenant James Cook was chosen by the Admiralty to take command of a Royal Society expedition funded by George III on the ship Endeavour , the purpose being to sail to a suitable point (Tahiti) in the Southern Pacific from which to observe the transit of Venus across the Sun on 3 June 1769. It was thought that, by observing the transit from different points on Earth, it would be possible to determine the distance of the Earth from both Venus and the Sun. The Royal Society asked that Joseph Banks (then a young Fellow aged 25) and a group of seven be allowed to join. Among them were two artists, Alexander Buchan and Sydney Parkinson, who were employed to draw views and specimens of natural historical interest, and Daniel Carl Solander a distinguished Swedish natural historian. Banks’s enthusiasm ensured that the voyage was exceptionally well equipped to handle natural historical discoveries. Having observed the transit of Venus, Cook was secretly under orders from the Admiralty then to sail to 40° south in search of the supposed Great Southern Continent; if not encountered, he was then to head due west to find the east coast of New Zealand. Following these instructions, Cook arrived at New Zealand on 6 October 1769. He then initiated the first detailed geographical survey of New Zealand, and Banks and Solander began putting together their rich collections of New Zealand flora; Cook also observed the transit of Mercury in Mercury Bay. On his second voyage in 1772 Cook went further south, entered the Antarctic circle twice (to 71° 10' S) and ruled out the existence of a Great Southern Continent, and first defined Antarctica as we know it. He returned to London in 1775 to be promoted to Captain and elected to the Royal Society. Banks went on to be elected President in 1778, a post which he held for nearly 42 years. Three other ties between Cook and the Royal Society include the naming of the Society Islands after his sponsors, the testing of a new chronometer for them, and a report to the Society on scurvy, which was to have great consequences for the future health of seamen. The Royal Society was thus instrumental in making possible Cook’s voyages, the outcome of which was a set of pioneering geographical, botanical, geological and anthropological descriptions of New Zealand. Here we trace some aspects of the subsequent interactions between New Zealand and the Royal Society by outlining the careers of relevant Fellows, namely (a) those foreign-born Fellows (30 identified) who spent parts of their careers in New Zealand, and (b) those New Zealand-born scientists (34) who have been elected Fellows for their work, whether carried out in New Zealand or elsewhere.

scholarly journals XXVIII. On the discordances between the sun's observed and computed right ascensions, as determined at the Blackman-street observatory, in the years 1821 and 1822; with experiments to show that they did not originate in instrumental derangement. also a description of the seven-feet transit with which the observations were procured, and upon which the experiments were made

1826 ◽  
Vol 116 ◽  
pp. 423-483 ◽  
Keyword(s):  
Royal Society ◽  
The Sun ◽  
Accurate Knowledge ◽  
The Subject ◽  
Right Ascension ◽  
Solar Rays

In presenting to the Royal Society the following pages, I am well aware that some apology is necessary; the subject however to which they refer being intimately connected with the progress of astronomy, I am induced to hope that the Society will still receive with indulgence, what would long since have been communicated to them, had other astronomical pursuits allowed me the opportunity. That the sun's right ascension, found by observation , frequently disagrees with that afforded by calculation , astronomers I believe now generally admit; an opinion however has been as generally entertained, that the discordances were the results of instrumental inaccuracy, occasioned by the effects of the solar rays upon certain parts of the instrument; hence observations of the sun have fallen into disrepute, whenever an accurate knowledge of the time is the object of research.

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