THE ABSORPTION DUE TO CARBON MONOXIDE IN THE INFRARED SOLAR SPECTRUM

1953 ◽  
Vol 31 (4) ◽  
pp. 504-516 ◽  
Author(s):  
J. L. Locke ◽  
L. Herzberg
Keyword(s):  
Carbon Monoxide ◽  
Laboratory Data ◽  
Solar Spectrum ◽  
Absorption Lines ◽  
Resolving Power ◽  
Absorption Bands ◽  
Solar Absorption ◽  
Earth’S Atmosphere ◽  
Earth's Atmosphere ◽  
Geographical Locations

New tracings of the absorption bands due to carbon monoxide in the 4.7 μ and 2.4 μ regions of the solar spectrum were obtained with a spectrometer of high resolving power. From the observed absorption intensity at 4.7 μ the abundance of carbon monoxide in the earth's atmosphere over Ottawa was found, during spring and fall 1952, to vary between 0.1 and 0.2 cm-atm. Similar observations, made at other stations, were re-evaluated with the laboratory data used at Ottawa. The values for the carbon monoxide abundance in the earth's atmosphere at different geographical locations, determined in this way, were found to be within the limits of the values obtained at Ottawa. Absorption lines due to solar carbon monoxide in the 4.7 μ region of the spectrum were resolved. Their intensity relative to the intensity of the solar carbon monoxide absorption in the 2.4 μ region of the spectrum was found to be in agreement with expectations based on the theoretical curves of growth for solar absorption lines.

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.

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.

Radio astronomical measurements from earth satellites

1959 ◽  
Vol 253 (1275) ◽  
pp. 494-500 ◽  
Keyword(s):  
Low Frequency ◽  
Radio Spectrum ◽  
Absorption Bands ◽  
Frequency Limit ◽  
Low Frequencies ◽  
Earth’S Atmosphere ◽  
Upper Limit ◽  
The Earth ◽  
Earth's Atmosphere

It may be thought that radio astronomical measurements made on the earth are not subject to the influence of the atmosphere and ionosphere to any great extent and that consequently there is no demand for measurements from earth satellites or other space stations. Unfortunately this is not the case and certain measurements from outside the earth’s atmosphere are very much desired. The radio spectrum so far explored extends from a low frequency limit in the 10 to 20 Mc/s band, to an upper limit in the millimetre waveband. In the millimetre band the limitation to the extension of the spectrum arises from absorption bands in the atmosphere, whereas at low frequencies the extension is limited by absorption and disturbances in the ionosphere. In this paper some examples will be given of the need to overcome these obstacles.

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 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.

Carbon monoxide in the Earth's atmosphere: indications of a global increase

Nature ◽  
1988 ◽  
Vol 332 (6161) ◽  
pp. 242-245 ◽  
Author(s):  
M. A. K. Khalil ◽  
R. A. Rasmussen
Keyword(s):  
Carbon Monoxide ◽  
Earth’S Atmosphere ◽  
Earth's Atmosphere ◽  
Global Increase
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