Absolute Transition Probability of the Auroral Green Line

Nature ◽  
1968 ◽  
Vol 220 (5171) ◽  
pp. 1017-1018 ◽  
Author(s):  
J. W. MCCONKEY ◽  
J. A. KERNAHAN
Keyword(s):  
Transition Probability ◽  
Green Line ◽  
Absolute Transition ◽  
Absolute Transition Probability

OBSERVATION OF THE TRANSITION IN O2

1961 ◽  
Vol 39 (8) ◽  
pp. 1110-1119 ◽  
Author(s):  
J. F. Noxon
Keyword(s):  
Emission Spectrum ◽  
High Altitude ◽  
Transition Probability ◽  
Electric Quadrupole ◽  
The Absolute ◽  
Absolute Transition ◽  
Absolute Transition Probability

The Q branch of the (0,0) band of the electric quadrupole [Formula: see text] transition in O2 has been observed at 1.908 μ in the emission spectrum of a discharge through O2 and He. By a comparison with the (0,0) atmospheric O2 band [Formula: see text], the absolute transition probability for the (b–a) system has been found to be 2.5 × 10−3 sec−1, with an uncertainty of a factor of 2. The (0,0) band of the infrared atmospheric [Formula: see text] system of O2 has also been observed in emission. Using the observed intensity of the (0,1) atmospheric O2 band in the aurora and airglow one may predict that the (0,0) (b–a) band should be detectable in a strong aurora if observations are made from high altitude.

Messung der Energiebreiten von Röntgen-Niveaus mit Hilfe der Auger-Elektronenspektroskopie

1968 ◽  
Vol 23 (2) ◽  
pp. 287-294 ◽  
Author(s):  
W. Mehlhorn ◽  
D. Stalherm ◽  
H. Verbeek
Keyword(s):  
Fine Structure ◽  
Transition Probabilities ◽  
Transition Probability ◽  
Level Width ◽  
Experimental Transition ◽  
Absolute Transition ◽  
Good Agreement

From the Auger transitions KL2,3L2,3(1D2) of neon and L3M2,2M2,3 (1D2) of argon the level widths Γ(K) of neon and Γ (L3) and Γ (L2) of argon have been determined by folding Lorentzian distributions with the spectrometer function. The values found are: Γ(K) = (0.15 ± 0.03) eV, Γ (L3) = Γ (L2) = (0.16 ± 0.02) eV. From the level width Γ(Κ) of neon and the relative intensities of the KLL Auger lines of neon, determined very recently, absolute transition probabilities of the KLL Auger transitions of neon have been calculated to be (in units of 10-3 e2/ħ a0=4.1 · 1013 sec-1) :KL1L1(1S0) = 0.35 ± 0.07;KL1L2,3 (1P1) = 0.96 ± 0.19;KL1L2,3 (2P) = 0.35 ± 0.07;KL2,3L2,3,3 (1S0) = 0.55 ± 0.11;KL2,3L2,3 (1D2) = 3.28 ± 0.66;KL2,3L2,3 (3P0,2) = 0 .Whereas the experimental total transition probability KLL is in good agreement with theoretical values of the transition probability for Ζ=10, determined by extrapolation of Callan’s values for Ζ ≧ 12 and of Archard’s values for Z=11, 12, 15, 16, 17, 18, the experimental transition probabilities of the fine structure components do not agree with Callan’s values and agree only in some cases with Archard’s values.

Long-term Cyclic Variations of Prominences, Green and Red Coronae over Solar Cycles

2000 ◽  
Vol 179 ◽  
pp. 201-204
Author(s):  
Vojtech Rušin ◽  
Milan Minarovjech ◽  
Milan Rybanský
Keyword(s):  
Emission Lines ◽  
High Latitudes ◽  
Green Line ◽  
Solar Cycles ◽  
The South ◽  
Coronal Emission ◽  
Local Maxima ◽  
The North ◽  
Cyclic Variations

AbstractLong-term cyclic variations in the distribution of prominences and intensities of green (530.3 nm) and red (637.4 nm) coronal emission lines over solar cycles 18–23 are presented. Polar prominence branches will reach the poles at different epochs in cycle 23: the north branch at the beginning in 2002 and the south branch a year later (2003), respectively. The local maxima of intensities in the green line show both poleward- and equatorward-migrating branches. The poleward branches will reach the poles around cycle maxima like prominences, while the equatorward branches show a duration of 18 years and will end in cycle minima (2007). The red corona shows mostly equatorward branches. The possibility that these branches begin to develop at high latitudes in the preceding cycles cannot be excluded.

Periodic Variations in the Coronal Green Line Intensity and their Connection with the White-light Coronal Structures

2000 ◽  
Vol 179 ◽  
pp. 197-200
Author(s):  
Milan Minarovjech ◽  
Milan Rybanský ◽  
Vojtech Rušin
Keyword(s):  
Time Resolution ◽  
White Light ◽  
Short Time Scale ◽  
High Time Resolution ◽  
Green Line ◽  
Periodic Intensity ◽  
Coronal Green Line ◽  
Significant Intensity ◽  
Short Time ◽  
Coronal Structures

AbstractWe present an analysis of short time-scale intensity variations in the coronal green line as obtained with high time resolution observations. The observed data can be divided into two groups. The first one shows periodic intensity variations with a period of 5 min. the second one does not show any significant intensity variations. We studied the relation between regions of coronal intensity oscillations and the shape of white-light coronal structures. We found that the coronal green-line oscillations occur mainly in regions where open white-light coronal structures are located.

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