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. 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 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 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.

scholarly journals III. Researches in spectrum-analysis in connexion with the spectrum of the sun.—No. V

1877 ◽  
Vol 25 (171-178) ◽  
pp. 546-546
Keyword(s):  
Spectrum Analysis ◽  
Royal Society ◽  
Solar Spectrum ◽  
The Sun ◽  
Preliminary Note

The author submits to the Royal Society the first portion of a new map of the solar spectrum, w.l. 39-40 ten millionths, constructed after the manner described in a previous “Preliminary Note.”

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

1878 ◽  
Vol 27 (185-189) ◽  
pp. 409-409 ◽  
Keyword(s):  
Spectrum Analysis ◽  
Solar Spectrum ◽  
The Sun ◽  
New Normal ◽  
Normal Map

The author submits the first strip of a new normal map of the Solar Spectrum, on four times the scale of Ängström’s. It embraces W. L. 3900—4000, and has been produced by means of photography.

VI. Researches in spectrum analysis in connexion with the spectrum of the Sun. No. VII

1879 ◽  
Vol 28 (190-195) ◽  
pp. 157-180 ◽  
Keyword(s):  
Spectrum Analysis ◽  
Large Scale ◽  
Solar Spectrum ◽  
Electric Arc ◽  
The Sun ◽  
Metallic Elements ◽  
Complete Spectrum

It is known to many Fellows of the Society that I have for the last four years been engaged upon the preparation of a map of the solar spectrum on a large scale, the work including a comparison of the Fraunhofer lines with those visible in the spectrum of the vapour of each of the metallic elements in the electric arc. To give an idea of the thoroughness of the work, at all events in intention, I may state that the complete spectrum of the sun, on the scale of the working map, will be half a furlong long; that to map the metallic lines and purify the spectra in the manner which has already been described to the Society, more than 100,000 observations have been made and about 2,000 photographs taken.

scholarly journals Modeling the center-to-limb variation of the Ca i 4227 Å line using FCHHT models

2014 ◽  
Vol 10 (S305) ◽  
pp. 381-386
Author(s):  
H. D. Supriya ◽  
H. N. Smitha ◽  
K. N. Nagendra ◽  
J. O. Stenflo ◽  
M. Bianda ◽  
...  
Keyword(s):  
Solar Spectrum ◽  
Visible Spectrum ◽  
Observational Constraints ◽  
Solar Model ◽  
The Sun ◽  
Dimensional Modeling ◽  
Height Dependence ◽  
Computationally Expensive ◽  
Chromospheric Line ◽  
The Magnetic Field

AbstractThe Ca i 4227 Å is a chromospheric line exhibiting the largest degree of linear polarization near the limb, in the visible spectrum of the Sun. Modeling the observations of the center-to-limb variations (CLV) of different lines in the Second Solar Spectrum helps to sample the height dependence of the magnetic field, as the observations made at different lines of sight sample different heights in the solar atmosphere. Supriya et al. (2014) attempted to simultaneously model the CLV of the (I, Q/I) spectra of the Ca i 4227 Å line using the standard 1-D FAL model atmospheres. They found that the standard FAL model atmospheres and also any appropriate combination of them, fail to simultaneously fit the observed Stokes (I, Q/I) profiles at all the limb distances (μ) satisfying at the same time all the observational constraints. This failure of 1-D modeling approach can probably be overcome by using multi-dimensional modeling which is computationally expensive. To eliminate an even wider choice of 1-D models, we attempt here to simultaneously model the CLV of the (I, Q/I) spectra using the FCHHT solar model atmospheres which are updated and recent versions of the FAL models. The details of our modeling efforts and the results are presented.

scholarly journals High-resolution spectroscopy and spectropolarimetry of the total lunar eclipse January 2019

2020 ◽  
Vol 635 ◽  
pp. A156
Author(s):  
K. G. Strassmeier ◽  
I. Ilyin ◽  
E. Keles ◽  
M. Mallonn ◽  
A. Järvinen ◽  
...  
Keyword(s):  
Large Scale ◽  
Solar Spectrum ◽  
High Resolution Spectroscopy ◽  
Strong Increase ◽  
Lunar Eclipse ◽  
The Sun ◽  
The Moon ◽  
Earth’S Atmosphere ◽  
The Earth ◽  
Earth's Atmosphere

Context. Observations of the Earthshine off the Moon allow for the unique opportunity to measure the large-scale Earth atmosphere. Another opportunity is realized during a total lunar eclipse which, if seen from the Moon, is like a transit of the Earth in front of the Sun. Aims. We thus aim at transmission spectroscopy of an Earth transit by tracing the solar spectrum during the total lunar eclipse of January 21, 2019. Methods. Time series spectra of the Tycho crater were taken with the Potsdam Echelle Polarimetric and Spectroscopic Instrument (PEPSI) at the Large Binocular Telescope in its polarimetric mode in Stokes IQUV at a spectral resolution of 130 000 (0.06 Å). In particular, the spectra cover the red parts of the optical spectrum between 7419–9067 Å. The spectrograph’s exposure meter was used to obtain a light curve of the lunar eclipse. Results. The brightness of the Moon dimmed by 10.m75 during umbral eclipse. We found both branches of the O2 A-band almost completely saturated as well as a strong increase of H2O absorption during totality. A pseudo O2 emission feature remained at a wavelength of 7618 Å, but it is actually only a residual from different P-branch and R-branch absorptions. It nevertheless traces the eclipse. The deep penumbral spectra show significant excess absorption from the Na I 5890-Å doublet, the Ca II infrared triplet around 8600 Å, and the K I line at 7699 Å in addition to several hyper-fine-structure lines of Mn I and even from Ba II. The detections of the latter two elements are likely due to an untypical solar center-to-limb effect rather than Earth’s atmosphere. The absorption in Ca II and K I remained visible throughout umbral eclipse. Our radial velocities trace a wavelength dependent Rossiter-McLaughlin effect of the Earth eclipsing the Sun as seen from the Tycho crater and thereby confirm earlier observations. A small continuum polarization of the O2 A-band of 0.12% during umbral eclipse was detected at 6.3σ. No line polarization of the O2 A-band, or any other spectral-line feature, is detected outside nor inside eclipse. It places an upper limit of ≈0.2% on the degree of line polarization during transmission through Earth’s atmosphere and magnetosphere.

scholarly journals XXIX.—The Visual, Grating and Glass-lens, Solar Spectrum (in 1884)

1886 ◽  
Vol 32 (3) ◽  
pp. 519-543 ◽  
Author(s):  
C. Piazzi Smyth
Keyword(s):  
Solar Spectrum ◽  
The Sun ◽  
Deep Blue ◽  
Glass Lens

Throughout the year 1884 the sun was seen over most countries under peculiar atmospheric circumstances; and these, instead of being confined to low altitudes, were never more conspicuous than during the summer of the year, and noon-tide of each day, and in the clear air on mountain heights of every country, whenever the sky was more or less free of actual clouds.On such occasions then, the usual phenomenon to be noticed by the eye, was, that nothing like blue sky could be witnessed near the sun. But in place of that, there was a broad glare of whitish light extending for several degrees around the luminary; and beyond that range, or over 20 degrees distant from him, there spread a wide reddish haze, passing into purple, and at greater distances into blue, but nowhere a very decided and deep blue sky.

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