Statistical comparison of WINDII auroral green line emission rate with DMSP/SSJ4 electron energy input for high and low solar flux years

2007 ◽  
Vol 112 (A12) ◽  
pp. n/a-n/a ◽  
Author(s):  
Y.-S. Lee ◽  
G. G. Shepherd
Keyword(s):  
Electron Energy ◽  
Energy Input ◽  
Emission Rate ◽  
Line Emission ◽  
Solar Flux ◽  
Green Line ◽  
Statistical Comparison

scholarly journals Effects of solar cycle variations on oxygen green line emission rate over Kiso, Japan

2011 ◽  
Vol 63 (8) ◽  
pp. 941-948 ◽  
Author(s):  
Uma Das ◽  
C. J. Pan ◽  
H. S. S. Sinha
Keyword(s):  
Solar Cycle ◽  
Emission Rate ◽  
Line Emission ◽  
Green Line

scholarly journals Preliminary results of rocket attitude and auroral green line emission rate in the DELTA campaign

2006 ◽  
Vol 58 (9) ◽  
pp. 1107-1111 ◽  
Author(s):  
Naomoto Iwagami ◽  
Sayaka Komada ◽  
Takao Takahashi
Keyword(s):  
Emission Rate ◽  
Line Emission ◽  
Green Line ◽  
Preliminary Results

scholarly journals First Ground Observations of OI5577 Green Line Emission over the Taiwan Area

2007 ◽  
Vol 18 (4) ◽  
pp. 843
Author(s):  
Sing-Wei Chiou ◽  
Lin-Ni Hau ◽  
Jan-Bai Nee ◽  
Chun-Sung Jao ◽  
Bo-Jhou Wang ◽  
...  
Keyword(s):  
Line Emission ◽  
Green Line ◽  
Taiwan Area

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.

Two day wave induced variations in the oxygen green line volume emission rate: WINDII observations

1997 ◽  
Vol 24 (9) ◽  
pp. 1127-1130 ◽  
Author(s):  
W. E. Ward ◽  
B. H. Solheim ◽  
G. G. Shepherd
Keyword(s):  
Emission Rate ◽  
Green Line ◽  
Volume Emission ◽  
Wave Induced

Morning and evening behavior of the F region green line emission: Evidence concerning the sources of O(¹S)

1977 ◽  
Vol 82 (29) ◽  
pp. 4715-4719 ◽  
Author(s):  
J. P. Kopp ◽  
J. E. Frederick ◽  
D. W. Rusch ◽  
G. A. Victor
Keyword(s):  
Line Emission ◽  
Green Line ◽  
F Region

scholarly journals Testing an inversion method for estimating electron energy fluxes from all-sky camera images

2004 ◽  
Vol 22 (6) ◽  
pp. 1961-1971 ◽  
Author(s):  
N. Partamies ◽  
P. Janhunen ◽  
K. Kauristie ◽  
S. Mäkinen ◽  
T. Sergienko
Keyword(s):  
Electron Energy ◽  
Energy Flux ◽  
Low Cost ◽  
Auroral Oval ◽  
Inversion Method ◽  
Green Line ◽  
Energy Fluxes ◽  
Good Spatial Resolution ◽  
Multi Wavelength ◽  
Order Of Magnitude

Abstract. An inversion method for reconstructing the precipitating electron energy flux from a set of multi-wavelength digital all-sky camera (ASC) images has recently been developed by tomografia. Preliminary tests suggested that the inversion is able to reconstruct the position and energy characteristics of the aurora with reasonable accuracy. This study carries out a thorough testing of the method and a few improvements for its emission physics equations. We compared the precipitating electron energy fluxes as estimated by the inversion method to the energy flux data recorded by the Defense Meteorological Satellite Program (DMSP) satellites during four passes over auroral structures. When the aurorae appear very close to the local zenith, the fluxes inverted from the blue (427.8nm) filtered ASC images or blue and green line (557.7nm) images together give the best agreement with the measured flux values. The fluxes inverted from green line images alone are clearly larger than the measured ones. Closer to the horizon the quality of the inversion results from blue images deteriorate to the level of the ones from green images. In addition to the satellite data, the precipitating electron energy fluxes were estimated from the electron density measurements by the EISCAT Svalbard Radar (ESR). These energy flux values were compared to the ones of the inversion method applied to over 100 ASC images recorded at the nearby ASC station in Longyearbyen. The energy fluxes deduced from these two types of data are in general of the same order of magnitude. In 35% of all of the blue and green image inversions the relative errors were less than 50% and in 90% of the blue and green image inversions less than 100%. This kind of systematic testing of the inversion method is the first step toward using all-sky camera images in the way in which global UV images have recently been used to estimate the energy fluxes. The advantages of ASCs, compared to the space-born imagers, are their low cost, good spatial resolution and the possibility of continuous, long-term monitoring of the auroral oval from a fixed position.

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