Note: Excitation of the Auroral Green Line of Atomic Oxygen (^{1}S -> ^{1}D) by N_{2}(A ^{3}Σ_{u}^{+})

1969 ◽  
Vol 157 ◽  
pp. 1023 ◽  
Author(s):  
J. A. Meyer ◽  
D. W. Setser ◽  
D. H. Stedman
Keyword(s):  
Atomic Oxygen ◽  
Green Line

Decay of the O I λ5577 line in meteor wakes

1970 ◽  
Vol 48 (9) ◽  
pp. 1017-1025 ◽  
Author(s):  
W. A. Gault
Keyword(s):  
Decay Rate ◽  
Atomic Oxygen ◽  
Line Emission ◽  
Maximum Intensity ◽  
Time Interval ◽  
Green Line ◽  
Multiple Exposure ◽  
Natural Rate ◽  
Quenching Mechanisms ◽  
Two Parameters

Multiple-exposure spectra of six meteors showing the auroral green line of atomic oxygen have been measured photometrically. The decay of the green line is described in terms of two parameters which are given as functions of height. It is shown that the maximum intensity occurs after a measurable time interval, which varies from 0.3 s at 115 km to 0.06 s at 105 km and decreases further with decreasing height. The subsequent decay rate is close to the natural rate (1 s−1) of the 1S state above 110 km, but increases with decreasing height to 3 s−1 at 100 km. The height of the green-line emission is consistent with most previous measurements, and corresponds with the height of the atmospheric atomic oxygen layer. The observations do not show a correlation of green-line characteristics with geomagnetic activity. Various possible excitation and quenching mechanisms are discussed.

scholarly journals Observations of OI 557.7 nm nightglow at Kolhapur (17° N), India

2011 ◽  
Vol 29 (10) ◽  
pp. 1873-1884 ◽  
Author(s):  
N. Parihar ◽  
S. Gurubaran ◽  
G. K. Mukherjee
Keyword(s):  
Comparative Study ◽  
Atomic Oxygen ◽  
Temperature Measurements ◽  
Green Line ◽  
Low Latitude ◽  
Temperature Variations ◽  
First Report ◽  
Latitude Station

Abstract. Ground-based nightglow observations of the atomic oxygen green line at 557.7 nm have been carried out at a low latitude station Kolhapur (17° N), India, during November 2003–April 2004 and December 2004–May 2005. The nocturnal behaviour of OI 557.7 nm intensity and a comparative study with simultaneous OH Meinel band temperature measurements has been presented. OI 557.7 nm intensity and OH temperature variations covary on many occasions. It was found that an 8 h tide characterizes the variation of intensity and temperature on most nights, and especially during the month of January. This is the first report of prolonged measurements of OI 557.7 nm emission from India.

scholarly journals A method for the intensification of atomic oxygen green line emission by internal gravity waves

2008 ◽  
Vol 113 (A12) ◽  
pp. n/a-n/a ◽  
Author(s):  
T. D. Kaladze ◽  
W. Horton ◽  
T. W. Garner ◽  
J. W. Van Dam ◽  
M. L. Mays
Keyword(s):  
Gravity Waves ◽  
Atomic Oxygen ◽  
Line Emission ◽  
Internal Gravity Waves ◽  
Green Line

Spectroscopy of Perseid Meteors with an Image Orthicon

1971 ◽  
Vol 49 (10) ◽  
pp. 1365-1373 ◽  
Author(s):  
P. M. Millman ◽  
A. F. Cook ◽  
C. L. Hemenway
Keyword(s):  
Band Structure ◽  
Time Resolution ◽  
Atomic Oxygen ◽  
Decay Constant ◽  
Green Line ◽  
Positive Systems ◽  
Initial Formation ◽  
Atomic Lines ◽  
Observational Techniques ◽  
Visible System

An image orthicon technique for recording meteors, developed some years ago by Hemenway at the Dudley Observatory, has recently been used at the Springhill Meteor Observatory, Ontario, for the recording of meteor spectra and combined with three other observational techniques—meteor radars, spectrographs, and a team of visual observers. Fifteen meteors, observed with the image orthicon during the August campaign in 1969, are here discussed out of a total of more than forty. Apparent visual magnitudes range from −1 to +3 and all 14 Perseid spectra in this group exhibit the oxygen green line at 5577 Å as well as other atomic lines normally found in the spectra of members of this shower. At the beginning of their trails all meteors show either a strong continuum, or evidence of band structure where the 1st and 2nd positive systems of N2 have been identified with reasonable certainty, while the first negative systems of N2+ and O2+, and the visible system of OH, are possible contributors.Measures of the 5577 Å line indicate a height spread from 120 to 95 km with a maximum near 106 km. After initial formation the intensity of this line increases for 0.2 to 0.5 s, after which it decays over periods up to 2 s. The decay constant for the 1S metastable state of neutral atomic oxygen is 0.76 s−1.The two chief advantages of the image orthicon technique are: its ability to record meteor spectra down to fainter thresholds of luminosity than in the case of conventional spectrography, and the time-resolution given by a recording of 15 complete frames per second.

scholarly journals The emission of oxygen green line and density of O atom determined by using ISUAL and SABER measurements

2012 ◽  
Vol 30 (4) ◽  
pp. 695-701 ◽  
Author(s):  
H. Gao ◽  
J.-B. Nee ◽  
J. Xu
Keyword(s):  
Atomic Oxygen ◽  
Emission Rate ◽  
Temperature Structure ◽  
Emission Rates ◽  
Green Line ◽  
Atmospheric Parameters ◽  
Density Distributions ◽  
Broadband Emission ◽  
The Earth ◽  
Made In

Abstract. Emissions of the 557.7 nm green line airglow observed by the ISUAL (Imager of Sprites and Upper Atmospheric Lightning) instrument on board the FORMOSAT-2 satellite in May and November 2008 are studied here to derive the density distributions of the atomic oxygen by using atmospheric parameters from MSISE-00 model and TIMED (Thermosphere Ionosphere Mesosphere Energetics and Dynamics)/SABER (Sounding of the Atmosphere using Broadband Emission Radiometry) measurements. The May observations were made in 10 days from a fixed orbit of longitude (100° E) with the results showing emission rate and O atom density both peaked at heights of about 90 km over 10° to 20° latitudes in the Northern Hemisphere (NH). In the Southern Hemisphere (SH), the emission rate and density of O atom are both low compared with those in NH. In November, the observations were made as the satellite traveled over all 14 orbits around the earth, covering all longitudes and latitudes of 25° S–45° N. Strong peaks of emission rates and O atoms are found at heights of about 95 km in the mid-latitudes in both hemispheres. In the equator, the airglow layer has a weaker emission rate but with higher altitude compared with those of mid-latitudes. In the lower and upper mesosphere at heights below 85 km and above 105 km, there are more O atoms in the equatorial regions than in the mid-latitudes. And there is a good correlation between the O atom and the temperature structure. A comparison with O atom distribution derived from OH airglow observed by TIMED/SABER at about the same time shows similar results.

Sign in / Sign up

Export Citation Format

Share Document