Source: http://proxy.osapublishing.org/oe/abstract.cfm?uri=oe-26-13-16984
Timestamp: 2019-04-23 18:54:13+00:00

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The O2(a1Δg) emission near 1.27 μm has relatively bright signal and extended altitude coverage and provides an important means to remotely sense the compositional structures and dynamical features of the upper atmosphere globally. In this paper, we report the simulation and application of O2(a1Δg) dayglow near 1.27 μm for wind observations from limb-viewing satellites. A line by line radiative transfer model of the O2(aΔ1g,υ′=0)→O2(XΣ3g,υ″=0) band is developed by taking both multiple scattering radiative transfer and nonlocal thermal equilibrium (non-LTE) models into account. The emission line O19P18 (7772.030 cm−1) with weak self-absorption, bright radiation intensity, and large spectral separation range is proved to be suitable for limb-viewing wind detection, due to its advantages of significantly lower cost, risk, and platform requirements. In order to ascertain the wind precision of O19P18, observations by a DASH-type (the Doppler asymmetric spatial heterodyne) instrument are simulated. The simulated results indicate a wind measurement precision of 1-2 m/s over an altitude range of 40 to 70 km in general, and possibly to 2-4 m/s due to a strong dependence on the spectral interference of the scattered sunlight background.
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Fig. 1 Dayglow production mechanism of the O2 infrared atmospheric band.
Fig. 2 Modelled number density profiles of the excited vibrational states. O 2 (a Δ 1 g , ν ′ ≥0).
Fig. 3 The vibrational temperature of the O 2 (a Δ 1 g , υ ′ =0) state, as well as the kinetic temperature varies with the altitude.
Fig. 4 The source functions of the infrared atmospheric band vary with the altitude in both LTE and non-LTE cases.
Fig. 5 Construction of path segments for the limb-viewing geometry.
Fig. 6 The emission spectra of the O2 infrared atmospheric band at tangent heights of 30 km, 50 km, 70 km and 90 km (with and without the effect of self-absorption).
Fig. 7 The scattered sunlight radiance in the red far wing of the O2 infrared atmospheric band at tangent heights of 20 km, 30 km, 40 km and 50 km.
Fig. 8 The total spectral radiance in the red far wing of the O2 infrared atmospheric band as a function of tangent height.
Fig. 9 The line center and asymptotic intensities vary with tangent height.
Fig. 10 The simulated interferogram images of the emission line O19P18 of the O2(a1Δg) dayglow (with and without the effect of the spectral interference of the scattered sunlight background).
Fig. 11 The signal to noise ratio, the limb-view weight and the interferogram contrast vary with tangent altitude.
Fig. 12 Calculated wind precision profiles along the line of sight (with and without the effect of the spectral interference of the scattered sunlight background).
Fig. 13 The signal to noise ratio and the wind precision vary with tangent height under day-time condition at mid-latitude (45°N) for the four seasons (January, April, June, and October).
(3) η 1.27 μm = A 1.27 μm n O 2 ( a Δ 1 g , ν ′ = 0 ) .
(5) α ¯ ( ν ) = S ( T K ) P ϕ ( ν − ν 0 , P , T K , γ a i r , γ s e l f , n , δ ) .
(8) J ( ν ) = B ( ν , T K ) n 2 n ¯ 2 α ( ν ) α ¯ ( ν ) .
(12) τ ( ν , z , z o b s ) = e x p ( − ∫ z s z o b s α ( ν , z ′ ) n ( z ′ ) d z ′ ) .
(14) ∫ z L z U τ ( ν , z , z U ) d z = 1 α ( ν ) l n l [ 1 − e x p ( − α ( ν ) l u l ) ] .
(15) I ( ν ) l = I ( ν ) l − 1 exp ( − ∑ i α ( ν ) l , i u l ) + ∑ i J ( ν ) l , i α ( ν ) l , i u l ∑ i α ( ν ) l , i u l [ 1 − e x p ( − ∑ i α ( ν ) l , i u l ) ] .

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