I. Researches on solar physics. Heliographical positions and areas of sun-spots observed with the Kew photoheliograph during the years 1862 and 1863

1869 ◽  
Vol 159 ◽  
pp. 1-110 ◽  
Keyword(s):  
Solar Physics ◽  
Physical Nature ◽  
Full Description ◽  
The Sun ◽  
Present Stage ◽  
Sun Spots ◽  
Numerical Expression

1. We have been hitherto engaged in preliminary researches devoted chiefly to the physical nature of the sun, but we now propose to give a first instalment of the mea­surements made with a view of making the solar photographs taken at Kew the basis of a new determination of the sun’s astronomical elements. Accordingly the present paper contains the results of measurements of the Kew sun-pictures for 1862 and 1863, i. e . the heliographical longitudes and latitudes of all spots observed in these two years, together with a full description of the methods pursued in the reductions. The results of the succeeding years, and their final discussion with reference to the sun’s elements, will be published hereafter. In addition to those measurements which have reference to the heliographical position of each spot, we have also measured the area of each group on each occasion when it was observed; and we conceive that in thus giving the position and area of each group we give all the information regarding sun-spots that is capable of accurate numerical expression, at least in the present stage of our knowledge.

scholarly journals II. Researches on solar physics

1872 ◽  
Vol 20 (130-138) ◽  
pp. 289-289
Keyword(s):  
Solar Surface ◽  
Solar Physics ◽  
Great Activity ◽  
The Sun ◽  
Considerable Time ◽  
Extended System ◽  
The Third ◽  
Sun Spots ◽  
To Come

The authors present in this paper the third instalment of the determination of the areas and heliographic positions occupied by the sun-spots observed by the Kew photoheliograph, comprising the years 1867, 1868, and 1869. They announce that the fourth and last instalment is in active progress, and will be preceded by the final discussion of the whole tenyearly period, during which the photoheliograph has been at work. This final discussion will contain the determination of the astronomical elements of the sun on the basis of photographic observations ; and this work, they anticipate, will not only settle the question of rotation for a considerable time to come, but will also throw light upon many points which have only recently been brought under the consideration of scientific men. The results in general, they believe, will prove the superiority of photographic sun-observations over previous methods. The second question which will be discussed is the distribution of sun-spots over the solar surface. The facts already brought out indicate that the progress of the inquiry may lead to some definite laws which regulate the distribution; there appear to exist centres of great activity on the sun, and the different solar meridians seem to have various but definite intervals of rest and activity. In conclusion the authors point out the necessity of devoting in future greater attention to the study of the faculse, and express a hope of seeing photographic sun-observations carried on in this country on a more extended system, connecting from day to day solar phenomena with terrestrial meteorology and magnetism.

VI. Account of some recent observation on Sun-spots, made at the Kew Observatory

1868 ◽  
Vol 16 ◽  
pp. 447-447
Keyword(s):  
Recent Observation ◽  
Solar Physics ◽  
The Sun ◽  
The West ◽  
West Limb ◽  
Sun Spots

The authors, after reviewing briefly the two theories on the nature of sun-spots, which are still subjects of dispute, refer to the stereoscopic views obtained and the results published in their ‘Researches on Solar Physics,’ and state the reasons which have led them to believe that sun-spots are cavities and at a lower level than the sun s photosphere. Their opinion has been recently strengthened by observations of a sun-spot on the 7th of May, which in disappearing produced in two successive photograms indentations in the west limb. After proving by the measurements made, which, with the calculations, are appended to their paper, that there can be no doubt about the identity of the heliographical elements of the previously observed spot and the successive indentations, they prove from the established details of the phenomena of sun-spots that such indentations must under all circumstances be very rare occurrences, and state fully the conditions favourable to the recurrence of similar observations, inviting observers to give their particular attention to them.

scholarly journals XXI. Researches on solar physics.—No. II. The positions and areas of the spots observed at Kew during the years 1864, 1865, 1866, also the spotted area the sunʼs visible disk from the commencement of 1832 up to May 1868

1870 ◽  
Vol 160 ◽  
pp. 389-496 ◽  
Keyword(s):  
Solar Disk ◽  
Solar Physics ◽  
Full Description ◽  
Paper Form ◽  
Sun Spots ◽  
Visible Disk

20. In a paper presented to the Society and published in the Philosophical Transactions for 1869 (vol. clix. p. 1), we have given a full description of the method adopted by us for ascertaining the positions and areas of the various sun-spots observed at Kew, and we have likewise, in Tables II. and III. of that paper, given the areas and the positions determined after the method described by us, for the various sun-spots of the years 1862 and 1863. In the present paper we give the same elements for the years 1864, 1865, and 1866, forming Tables II. and III., so that these Tables in our present paper form a continuation of the Tables bearing the same number in our previous paper. We have stated elsewhere that Hofrath Schwabe, of Dessau, had very generously put into our hands the valuable collection of drawings of the solar disk made by him during the course of about forty years, and thus it became an object of importance to us to fix upon some method of testing the value of these drawings, and of extracting from them what information they might contain.

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?”

Researches on solar physics. Heliographical positions and areas of sun-spots observed with the Kew photoheliograph during the years 1862 and 1863

1868 ◽  
Vol 16 ◽  
pp. 336-336 ◽  
Keyword(s):  
Solar Physics ◽  
The Other ◽  
The Sun ◽  
Heliographic Latitude ◽  
Other Hand ◽  
Considerable Length ◽  
Sun Spots

In this paper the sun-pictures taken by the Kew photoheliograph for the years 1862 and 1863 are discussed; the heliographic latitude and longitude of every spot is given, and the area of each group on each day when it was observed is expressed in millionth parts of the sun’s whole hemisphereal area. The Kew photoheliograph itself, as well as the instrument invented by Mr. De la Rue for measuring sun-pictures, have been already described by Mr. De la Rue in the Bakerian Lecture for 1862. These descriptions are not therefore repeated in this paper; but, on the other hand, the method by which the heliographic position of spots is deduced from the measurements made is given at considerable length. The results of succeeding years, and their final discussion with reference to the sun’s elements, will be published hereafter.

scholarly journals III. Preliminary Report to the solar physics Committee on the sun-spot observations made at Kensington

1882 ◽  
Vol 33 (216-219) ◽  
pp. 154-158
Keyword(s):  
Preliminary Report ◽  
Solar Physics ◽  
The Sun ◽  
Full Report ◽  
Sun Spots ◽  
The Mean ◽  
Mean Time

Since the commencement of the observations, in November, 1879, of the twelve most widened lines in sun-spots, about 220 observations have have been drawn up and the tabulation of the first hundred completed. The reductions are being carried on, and I hope shortly to be able to lay a full report upon the 200 observations before the Committee, but desire, in the mean time, to bring the present preliminary one before it The reduction of the first hundred observations, extending from November, 1879, to September, 1880, has yielded the following re­sults :-

Galactic orbits of stars

1966 ◽  
Vol 25 ◽  
pp. 93-97
Author(s):  
Richard Woolley
Keyword(s):  
Globular Cluster ◽  
Potential Field ◽  
High Velocity ◽  
Velocity Vector ◽  
Variable Stars ◽  
The Sun ◽  
Proper Motions ◽  
Rr Lyrae ◽  
The Galaxy

It is now possible to determine proper motions of high-velocity objects in such a way as to obtain with some accuracy the velocity vector relevant to the Sun. If a potential field of the Galaxy is assumed, one can compute an actual orbit. A determination of the velocity of the globular clusterωCentauri has recently been completed at Greenwich, and it is found that the orbit is strongly retrograde in the Galaxy. Similar calculations may be made, though with less certainty, in the case of RR Lyrae variable stars.

The Interpretation of Solar Spectral Intensities

1988 ◽  
Vol 102 ◽  
pp. 329
Author(s):  
R.W.P. McWhirter
Keyword(s):  
Emission Measure ◽  
Physical Nature ◽  
Atomic Data ◽  
The Sun ◽  
Atomic Properties ◽  
Outer Atmosphere ◽  
Spectral Intensities ◽  
Thin Plasma ◽  
Number Of Authors

The intensity of a specrtal line from an optically thin plasma such as the outer atmosphere of the sun depends on both the atomic properties of the atomic ion responsible for the line and the physical nature of the plasma. In this paper we discuss the various ways in which the measured spectral intensities from the sun are used to discover something about the nature of the sun’s atmosphere. The technique has been referred to as the emission measure method. It has important limitations in terms of the accuracy of the specrtal data as well as the atomic data. We discuss some of these and suggest methods by which they may be assessed. The technique is illustrated by application to real observations from a number of authors.

About the concept of synthesis of high-performance detection and positioning systems in the areas of elements falling, separated from strategic and space missiles on the trajectories of their flight during tests and regular operation

2018 ◽  
pp. 10-21
Author(s):  
G. G. Vokin
Keyword(s):  
High Performance ◽  
Physical Nature ◽  
Positioning Systems ◽  
Physical Conditions ◽  
Highly Efficient

The article describes the approach and topical issues of synthesis of highly efficient transportable systems for search and determination of coordinates in the areas of elements falling, separated from the missiles, taking into account the dislocation of pre-empted areas of fall and physical conditions in their territories. The principles of these systems are based on the rational integration of traditional and non-traditional information sensors of different physical nature, which record the moments of landing of separated parts of the missiles.

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