scholarly journals V. Researches in spectrum-analysis in connexion with the spectrum of the sun

1874 ◽  
Vol 22 (148-155) ◽  
pp. 391-391
Keyword(s):  
Spectrum Analysis ◽  
Wave Length ◽  
Solar Spectrum ◽  
The Other ◽  
Photographic Method ◽  
The Sun ◽  
The Third

Maps of the spectra of calcium, barium, and strontium have been constructed from photographs taken by the method described in a former communication (the third of this series). The maps comprise the portion of the spectrum extending from wave-length 3900 to wave-length 4500, and are laid before the Society as a specimen of the results obtainable by the photographic method, in the hope of securing the cooperation of other observers. The method of mapping is described in detail, and tables of wave-lengths accompany the maps. The wave-lengths assigned to the new lines must be considered only as approximations to the truth. Many of the coincidences between lines in distinct spectra recorded by former observers bave been shown, by the photographic method, to be caused by the presence of one substance as an impurity in the other; but a certain number of coincidences still remain undetermined. The question of the reversal of the new lines in the solar spectrum is reserved till better pho­tographs can be obtained.

scholarly journals III. Researches in spectrum analysis in connection with the spectrum of the sun

1878 ◽  
Vol 27 (185-189) ◽  
pp. 49-50
Keyword(s):  
Spectrum Analysis ◽  
Solar Spectrum ◽  
The Sun ◽  
Chemical Constitution

The author refers to the work already done in the new map of the Solar Spectrum as enabling the chemical constitution of the Sun’s atmosphere to be studied under more favourable conditions. He shows that, the work already done enables him to confirm the presence of Sr, Pb, Cd, K, Ce and U, and also that it indicates the probability of the presence of Va, Pd, Mo, In, Li, Rb, Cs, Bi, Sn, La, Gl, Yt or Er.

scholarly journals On the action of ultra-violet sunlight upon the upper atmosphere

1937 ◽  
Vol 160 (901) ◽  
pp. 155-173 ◽  
Keyword(s):  
Wave Length ◽  
Charged Particles ◽  
Solar Spectrum ◽  
Ultra Violet ◽  
Magnetic Storms ◽  
Upper Atmosphere ◽  
The Sun ◽  
Polar Aurora ◽  
Night Sky ◽  
Photochemical Action

The ordinary solar spectrum extends, as is well known, to about λ2913, the more ultra-violet parts being cut off by ozone absorption in the upper atmosphere. We have thus no direct knowledge of the distribution of intensity in the solar spectrum beyond λ2913, as it will appear to an observer situated outside the atmosphere of the earth. But it is now recognized that a number of physical phenomena is directly caused by the photochemical action of this part of sunlight on the constituents of the upper atmosphere. Such phenomena are (1) the luminous spectrum of the night sky and of the sunlit aurora, (2) the ionization in the E, F and other layers which is now being intensely studied by radio-researchers all over the world, (3) the formation and equilibrium of ozone (see Ladenburg 1935), (4) magnetic storms and generally the electrical state of the atmosphere. Formerly it was a debatable point whether some of these phenomena were not to be ascribed to the action of streams of charged particles emanating from the sun. There seems to be no doubt that the polar aurora and certain classes of magnetic storms are to be ascribed to the bombardment of molecules of N 2 and O 2 by such charged particles, for these phenomena show a period which is identical with the eleven year period of the sun, and are found in greater abundance, the nearer we approach the magnetic poles. But there now exists no doubt that the ionization observed by means of radio-methods in the E and F 1 regions, their variation throughout day and night, and at different seasons is due to the action of ultra-violet sunlight. This was decisively proved by observations during several total solar eclipses since 1932 (Appleton and Chapman 1935). The luminous night-sky spectrum, though it has certain points of similarity to the polar aurora, is on the whole widely different, and is found on nights free from electrical disturbances. The prevailing opinion is that it is mainly due to the ultra-violet solar rays, i. e. in the course of the day sunlight is stored up by absorption by the molecules in the upper atmosphere, and again given up during the night, in one or several steps, as a fluorescence spectrum. According to S. Chapman (1930) the formation of the ozone layer and its equilibrium under different seasonal conditions is also to be mainly ascribed to the action of ultra-violet sunlight. In the following paper an attempt will be made to discuss some of these questions in as rigorous a way as is possible with our present knowledge. It is evident that an adequate discussion is possible only if we have a good knowledge of (1) the distribution of intensity in the solar spectrum beyond λ2900, (2) the photochemical action of light of shorter wave-length than λ2900 on the constituent molecules of the upper atmosphere, which are mainly oxygen and nitrogen. We shall first consider (1).

scholarly journals MODEL SPEKTRUM RADIASI SURYA DAN SUHU DI DALAM RUMAH PLASTIK (THE SOLAR SPECTRUM AND TEMPERATURE MODEL IN THE PLASTICHOUSE)

Agromet ◽  
2006 ◽  
Vol 20 (1) ◽  
pp. 10
Author(s):  
. Yushardi ◽  
Yonny Kusmaryono ◽  
H.M. H. Bintoro ◽  
A. H. Tambunan
Keyword(s):  
Field Experiment ◽  
Solar Spectrum ◽  
The Other ◽  
Temperature Model ◽  
Temperature Optimum ◽  
Active Radiation ◽  
Optimum Result ◽  
The Third ◽  
Ultraviolet Protection ◽  
C 50

<p>Research has been conducted to develop the solar spectrum and temperature model in the plastic house. The objective of this research is to determine spectrum and temperature optimum in the plastic house. The method was used by field experiment and simulation. Field experiment consist of three treatments. These are first treatment used the plastic Polyethylene (PE) with UV (Ultraviolet) protection (0 %. 6 % and 14 %). The second treament was determined the tilt angle between plastic cover and horizontal planar. The third treatment was flooring by used soil and grass. The expriment reveals that optimum condition for the plastic house that used plastic UV protection 14%, and use grass as the floor. Produce a optimum result in decreasing Tin for 2.9 % in plastic UV 14%, 2.7 % in β= 67o and 5.7 % in using grass as the floor. Spectrum of UV, PAR (Photosintetically Active Radiation) and IR (Infrared) that transmited from PE 14 % plastik 3.0 W/m2. 143.2 W/m2 and 192.8 W/m2 respectively. The other parameter that influence the temperature in plastic house is natural convection coeficient (hi) and ventilation coeficient (hv). For type Hexagonal plastic house hi and hv 1.5 W/m2.C, 50 W/m2.C respectively. For type Tunnel plastic house hi and hv 1.5 W/m2.oC and 55 W/m2.C respectively.</p>

scholarly journals Analog Video Magnetograms in Real Time

1971 ◽  
Vol 43 ◽  
pp. 76-83 ◽  
Author(s):  
R. C. Smithson ◽  
R. B. Leighton
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Solar Magnetic Field ◽  
Solar Spectrum ◽  
Zeeman Splitting ◽  
The Other ◽  
Line Of Sight ◽  
Zero Field ◽  
The Sun ◽  
Solar Magnetic Fields

For many years solar magnetic fields have been measured by a variety of techniques, all of which exploit the Zeeman splitting of lines in the solar spectrum. One of these techniques (Leighton, 1959) involves a photographic subtraction of two monochromatic images to produce a picture of the Sun in which the line-of-sight component of the solar magnetic field appears as various shades of gray. In a magnetogram made by this method, zero field strength appears as neutral gray, while magnetic fields of one polarity or the other appear as lighter or darker areas, respectively. Figure 1 shows such a magnetogram.

scholarly journals The spectrum of magnesium hydride

1910 ◽  
Vol 83 (561) ◽  
pp. 210-210 ◽  
Keyword(s):  
Wave Length ◽  
Solar Spectrum ◽  
Magnesium Hydride ◽  
High Dispersion ◽  
Calcium Hydride ◽  
The Sun ◽  
Or Groups ◽  
Concave Grating ◽  
Limits Of Error ◽  
Reduced Temperature

The author has previously discovered that many of the band lines peculiar to the sun-spot spectrum are identical with lines composing the green fluting attributed to magnesium hydride by Liveing and Dewar. The present paper gives the results of a further investigation of this spectrum with high dispersion, together with details of wave-length determinations. The principal results may be briefly summarised as follows: -(1) No sufficient reason has been found for modifying Leveing and Dewar’s conclusion that the spectrum is produced by the combination of magnesium with hydrogen. (2) Lines are shown at short intervals in all parts of the spectrum from the extreme red to λ 2300, and definite groups of flutings begin at 5621.57, 5211.11, 4844.92, 4371.2, and near 2430. (3) From photographs of the magnesium arc in hydrogen at low temperatures, taken with a 10-foot concave grating, the positions of close upon 2000 lines composing the three principal bands have been determined. The wave-lengths were derived from the interference standards of Fabry and Buisson, but have been corrected to Rowland’s scale to facilitate comparsion with solar spectra. (4) Twelve of the series of none of the formulæ which have been proposed are sufficiently general in their application to represent all of these series within the limits of error of measurements. For the longer series the closest approximation is given by Halm’s equation. (5) The identification of magnesium hydride in the sun-spot spectrum has been fully confirmed, and is clearly demonstrated by photographs submitted for reproduction. (6) It is shown that many of the bright lines, but merely clear interspaces between lines or groups of lines in the spectrum of magnesium hydride. (7) The presence of the magnesium hydride flutings, together with flutings of titanium oxide and calcium hydride discovered at Mount Wilson, accords with the view that spots are regions of reduced temperature, and that their darkness is at least partly due to absorption. (8) The investigation of the possible presence of lines of magnesium hydride in the ordinary solar spectrum is for several reasons inconclusive, but there is evidence that very few, if any, of the thousands of faint lines tabluated by Rowland are to be accounted for by this substance.

scholarly journals NON-STATIONARY MODEL OF THE SOLAR CORE

2020 ◽  
pp. 101-104
Author(s):  
S.F. Skoromnaya ◽  
V.I. Tkachenko
Keyword(s):  
Electromagnetic Waves ◽  
Three Dimensional ◽  
The Other ◽  
Spherically Symmetric ◽  
The Sun ◽  
Axially Symmetric ◽  
Stationary Model ◽  
The Third ◽  
The Standard Model ◽  
Oscillatory Processes

The main parameters of the standard model of the Sun are considered, according to which the Sun is considered as a spherically symmetric and quasistatic star, and thermonuclear reactions of the pp-cycle mainly occur inside it and the energy is uniformly released at a rate of 2·10-4J/(kg·s). Based on observational data it was concluded that the Sun is not a star with uniformly ongoing processes, it is characterized by oscillatory processes and flashes. It is proposed to consider the non-stationary model of the Sun, in which it is required to take into account the existence of electromagnetic waves in the plasma of the solar core and, as a result, the existence of wave collapses (WC). A three-dimensional axially symmetric WC is considered and an estimate of the velocity of removal of the plasma of the solar core during the development of a three-dimensional axially symmetric WC is given. For the considered WC the existence of three directions of flows of elementary plasma volumes relative to the observer is demonstrated: one direction is due to the moving the elementary plasma volume from the observer and the other  to him. The third direction of moving of the elementary plasma volumes is perpendicular to the direction of observation and their velocity relative to the observer is zero. It is concluded that the existence of such motions of elementary plasma volumes during the development of WC can leave a definite imprint on the parameters of the synthesis products in them.

XII. Researches in spectrum-analysis in connexion with the spectrum of the sun.— No. V

1881 ◽  
Vol 172 ◽  
pp. 561-576 ◽  
Keyword(s):  
Spectrum Analysis ◽  
Solar Spectrum ◽  
The Sun ◽  
Construct Maps

It has long been clear that the means placed at our disposal by photography for studying the solar spectrum enable us to construct maps of the region more refrangible than b on a much larger scale than those hitherto employed. At the same time, as our knowledge of the molecular conditions under which changes in spectra occur is increased, it becomes neccessary to embrace more and more detail in the inquiry.

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

1875 ◽  
Vol 165 ◽  
pp. 157-160
Keyword(s):  
Rainy Season ◽  
Royal Society ◽  
General Procedure ◽  
Solar Spectrum ◽  
The Other ◽  
The Sun ◽  
Single Group ◽  
Short Period ◽  
Clear Atmosphere ◽  
Do So

The spectroscopic observations hereafter discussed were made with instruments belonging to the Royal Society, and in accordance with certain suggestions which a Committee were good enough to make in connexion with my letter to Sir Edward Sabine, President, dated 13th February, 1866. In view of my residence at a considerable height, and the exceedingly clear atmosphere prevailing at some periods of the year, it was suggested that the locality was peculiarly favourable for comparing the solar spectrum when the sun was high with the corresponding spectrum at sunset; any differences between these aspects which might appear were to be noted on Kirchhoff’s well-known maps. Accordingly I set to work with the spectroscope first supplied to me (hereafter distinguished by the prefix old ), and during the autumns of 1868 and 1869 I mapped the differences in question from the extreme red to D: these results appeared in the ‘Proceedings of the Royal Society,’ No. 123, 1870, the Map being marked vol. xix. pl. 1; it is unnecessary, therefore, to dwell on this portion of my labours, excepting to add that the definitions and general procedure there adopted have been retained in the remarks which follow. 2. The observations hereafter noticed were always taken in the autumn , when, the rainy season having passed away, the atmosphere on these mountains is exceedingly clear, so that the sun, the object of inquiry, is bright even to his setting, and a spectrum may therefore be then obtained through a long stretch of terrestrial atmosphere corresponding to the height of the station of observation; on the other hand, with the sun about the meridian, the height of station places the observer above a relative amount of atmosphere, so that the spectrum obtainable at this time and about sunset are highly eligible for the comparison in view. Accordingly the two spectra are given in the accompanying map (Plate 25); and for easy comparison they are placed in juxtaposition. By “sun high” is to be understood any position for the sun within a couple of hours of the meridian; by “sun low” that the sun was within 3 or 4 diameters of his setting and yet quite bright. Indeed it is only when very near sunset that the marked alterations in the lines appear; so that the spectrum required is not only rarely obtainable, but it hardly lasts beyond 10 minutes of an evening. In this short period (when, moreover, the observer is fatigued with previous watching) changes from the sun-high spectrum must first be detected; then their position must be identified, and, failing this, found by measurement; next, the appearance should be drawn, and finally the drawing should be compared with the original: under these conditions a week may be easily absorbed by a single group. It is also to be borne in mind that no human eye will endure, without at least temporary injury, protracted watching of the bright solar spectrum for more than four or five weeks at a time; indeed, though I habitually used both eyes as a relief to one another, they both invariably suffered, and continued to do so for several weeks after every autumn. The following facts may be here mentioned:—

scholarly journals III. Researches in spectrum-analysis in connexion with the spectrum of the Sun.—Part III

1873 ◽  
Vol 21 (139-147) ◽  
pp. 508-514 ◽  
Keyword(s):  
Spectrum Analysis ◽  
The Other ◽  
New Method ◽  
The Sun ◽  
Other Hand ◽  
General Line

The paper commences with an introduction, in which the general line of work since the last paper is indicated. Roughly speaking, this has been to ascertain the capabilities of the new method in a quantitative direction. It is stated that while qualitative spectrum-analysis depends upon the positions of the lines, quantitative spectrum-analysis on the other hand depends not on position but on the length, brightness , and thickness of the lines.

scholarly journals Researches in spectrum analysis in connexion with the spectrum of the sun

1878 ◽  
Vol 27 (185-189) ◽  
pp. 279-284
Keyword(s):  
Solar Atmosphere ◽  
Spectrum Analysis ◽  
Solar Spectrum ◽  
Spectral Lines ◽  
The Sun

In a map of the solar spectrum, containing a greatly increased number of lines, such as that upon which I am now engaged, it is possible to seek under favourable conditions the coincidence or non-coincidence of lines due to elements hitherto undetected in the solar atmosphere, on account of their existing in quantities insufficient to give very marked spectral lines. A search has accordingly been made, on the principles laid down in previous communications, for those elements which contain in their spectra long and well-characterised lines in the photographic region.

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