scholarly journals On the limit of Solar and stellar light in the ultra-violet part of the spectrum

1890 ◽  
Vol 46 (280-285) ◽  
pp. 133-135
Keyword(s):  
Solar Spectrum ◽  
Ultra Violet ◽  
The Sun ◽  
Earth’S Atmosphere ◽  
Rapid Extinction ◽  
Earth's Atmosphere

It has been long known that the solar spectrum stops abruptly, but not quite suddenly, at the ultra-violet end, and much sooner than the spectra of many terrestrial sources of light. The observations of Cornu, of Hartley, and, quite recently, of Liveing and Dewar, appear to show that the definite absorption to which the very rapid extinction of the solar spectrum is due, has its seat in the earth’s atmosphere, and not in that of the sun; and that, consequently, all ex-terrestrial light should be cut off at the same place in the spectrum.

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 III.—Note on the Little b Group of Lines in the Solar Spectrum and the New College Spectroscope

1883 ◽  
Vol 32 (1) ◽  
pp. 37-44
Author(s):  
C. Piazzi Smyth
Keyword(s):  
Solar Spectrum ◽  
The Sun ◽  
The Moon ◽  
Earth’S Atmosphere ◽  
Earth's Atmosphere

Every spectroscopist is perfectly aware that the group of dark Fraunhofer lines in the Solar Spectrum, known as “ little b,” is composed of the biggest, broadest, most colossal lines in all the brighter part of any and every spectrum depending on Sunlight, whether direct from the Sun or reflected from the earth's atmosphere, the Moon, or any of the planets.

scholarly journals Measurements of the amount of ozone in the earth’s atmosphere and its relation to other geophysical conditions

1926 ◽  
Vol 110 (756) ◽  
pp. 660-693 ◽  
Keyword(s):  
Absorption Band ◽  
Solar Spectrum ◽  
Ultra Violet ◽  
Equilibrium Temperature ◽  
Strong Absorption Band ◽  
Weak Band ◽  
Chemical Action ◽  
Earth’S Atmosphere ◽  
The Alps ◽  
Earth's Atmosphere

Several attempts have been made to determine the amount of ozone in the earth’s atmosphere during recent years. Until 1920 only chemical methods were employed, and these yielded very discordant results, the difficulty being to separate the chemical action of ozone from that of other oxidizing constituents of the atmosphere. Rayleigh in England, and Götz in the Alps, have shown that there cannot be more than a very small amount of ozone in the air near the earth’s surface. The first accurate measurements of the total amount of ozone in the atmosphere over any given region were made by Fabry and Buisson, who measured spectroscopically the intensity of the ultra-violet absorption band in the solar spectrum, which is due to ozone in the earth’s atmosphere. From measurements made on 14 days in May and June, 1920, they found the amount of ozone to be equivalent to a layer of pure ozone about 3 mm. thick at normal temperature and pressure. Small variations were observed from day to day. Ozone has a very strong absorption band, extending from about 3300 Å towards the shorter wave-lengths and reaching a maximum at about 2550 Å, and a weak band in the visible, which, however, absorbs some 4 per cent, of the solar energy at 6000 Å, and only rather narrow bands in the infra-red at about 9.5μ and 4.5μ (whose width and intensity are not accurately known) ; therefore its equilibrium temperature under solar and terrestrial radiation is high. It is thus of considerable interest to determine what variations in the amount of ozone take place over a long period, since these may have important relations to other geophysical phenomena.

1. Observations on the Lines of the Solar Spectrum, and on those produced by the Earth's Atmosphere, and by the Action of Nitrous Acid Gas

1845 ◽  
Vol 1 ◽  
pp. 21-24
Author(s):  
David Brewster
Keyword(s):  
Nitrous Acid ◽  
Solar Spectrum ◽  
Acid Gas ◽  
Earth’S Atmosphere ◽  
Transparent Media ◽  
Similar Character ◽  
Earth's Atmosphere

The author was led, in prosecution of his researches on the absorptive action of transparent media of light, which have been partly communicated in previous papers to the Society, to examine the influence of coloured gaseous bodies. Iodine vapour was one of these, and its action was found of a similar character to that of fluids having a similar tint. Nitrous acid gas presented a far more extraordinary phenomenon.

XXXIX.—Did the Tail of Halley's Comet affect the Earth's Atmosphere?

1910 ◽  
Vol 30 ◽  
pp. 529-550
Author(s):  
John Aitken
Keyword(s):  
The Sun ◽  
Earth’S Atmosphere ◽  
Magnetic Condition ◽  
The Earth ◽  
Electrical Condition ◽  
Halley's Comet ◽  
Earth's Atmosphere ◽  
Pass Through

The return of Halley's Comet in May of this year gave rise to much speculation as to its possible effects on the earth. As it was expected that the earth would pass through the tail of the comet when the comet passed between us and the sun, many observations were arranged for in order to see if the tail, whatever it was composed of, had any effect on the earth or on its atmosphere. If the tail was composed of matter in any form, gaseous, or fine solid or liquid particles, then it seemed possible to get some evidence of its presence in the atmosphere; or if the tail was composed of electrons, then these would disturb the electrical condition of the atmosphere, and also the magnetic condition of the earth.

scholarly journals VI. The ultra-violet band of ammonia, and its occurrence in the solar spectrum

1919 ◽  
Vol 218 (561-569) ◽  
pp. 351-372 ◽  
Keyword(s):  
Solar Spectrum ◽  
Ultra Violet ◽  
Maximum Intensity ◽  
Resolving Power ◽  
The Sun ◽  
Sufficient Detail ◽  
Other Substances ◽  
Violet Band ◽  
Band Spectra

A question of great interest in connection with the solar spectrum is that of the origin of the thousands of unidentified faint lines which were catalogued by Rowland in his “Preliminary Table of Solar Spectrum Wave-lengths.” Some of these lines may possibly be identical with faint lines in metallic spectra which have not yet been completely tabulated, but in view of the presence of bands of cyanogen, carbon and hydrocarbon, the possibility of the correspondence of most of them with band spectra of other substances should not be overlooked. As a contribution to this inquiry, the present investigation was undertaken primarily in order to determine whether Group P in the ultra-violet region of the solar spectrum might not be mainly due to the presence of ammonia in the absorbing atmosphere of the sun. Ammonia was already known to give a remarkable band in this region, having its position of maximum intensity near λ 3360, but it had not been investigated in sufficient detail to permit of an adequate comparison with the solar tables. Photographs have accordingly been taken with spectrographs of high resolving power for the purpose of this comparison, and, as will appear from the details which follow, it has been established that the ammonia band is certainly represented in the solar spectrum, and accounts for a considerable number of faint lines for which no other origins have been suggested.

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