ISSN 0016-7932, Geomagnetism and Aeronomy, 2018, Vol. 58, No. 2, pp. 273–280. © Pleiades Publishing, Ltd., 2018. Original Russian Text © A.I. Semenov, I.V. Medvedeva, V.I. Perminov, 2018, published in Geomagnetizm i Aeronomiya, 2018, Vol. 58, No. 2, pp. 287–294.

Spatial and Temporal Variations of Infrared Emissions in the Upper Atmosphere. 3. 5.3-μm Nitric Oxide Emission A. I. Semenova, *, I. V. Medvedevab, and V. I. Perminova a

Obukhov Institute of Atmospheric Physics, Russian Academy of Sciences, Moscow, Russia Institute of Solar–Terrestrial Physics, Siberian Division, Russian Academy of Sciences, Irkutsk, Russia *e-mail: [email protected]

b

Received May 16, 2017

Abstract—The results of rocket and satellite measurements available in the literature of 5.3-μm nitric oxide emission in the upper atmosphere have been systematized and analyzed. Analytical dependences describing the height distribution of volumetric intensity of 5.3-μm emission of the NO molecule and its variations in a range of heights from 100 to 130 km as a function of the time of year, day, latitude, and solar activity have been obtained. DOI: 10.1134/S0016793218020172

1. INTRODUCTION The nitric oxide (NO) molecule is a key component of the upper atmosphere. Its structure governs many close electronic states with very similar potential functions, and most of them have almost no shift relative to each other (Gilmore, 1965). Due to this feature and according to the Franck–Condon principle, only transitions with Δv = 0 actually occur in this case. A specific feature of this emission is that groundbased observations cannot be used. Direct data on NO-molecule emission can be obtained only from rocket and satellite measurements, which are limited in time and are usually irregular due to their technological characteristics and expense. These factors strongly limit the possibilities for the study of its spatial and temporal variations. This paper systematizes the measurement data on nitric oxide emission intensity for a number of years that are available in the literature in order to reveal the regularities of its variations for different heliogeophysical conditions. We consider different types of regular variations in the intensity and height of the emitting layer of 5.3-μm emission and attempt to regularize them using an empirical approximation of the regularities revealed. 2. PHOTOCHEMICAL PROCESSES OF EMISSION UNDER UPPER ATMOSPHERIC CONDITIONS Under daytime upper atmospheric conditions, we attempted to observe the NO emission bands in the ultraviolet region of the spectrum (170–250 nm) of

β(B 2Π − X 2Π), γ( A 2Σ + − X 2Π), δ(C 2Π − X 2Π), and ε(D 2Σ + − X 2Π) systems. Unfortunately, due to the lack of measurement data, it is almost impossible to conduct systematic studies of NO emission variations in this spectral range. In view of this, it is most interesting to investigate the infrared radiation caused by vibrational transitions of the ground state NO (1–0) – λ 5.3 μm and NO (2– 0) – λ 2.7 μm:

NO( X 2Π, ν = 1) → NO( X 2Π, ν = 0) + hν(λ5.3 μm), A1–0 = 13.38 s–1, NO( X 2Π, ν = 2) → NO( X 2Π, ν = 0) + hν(λ2.7 μm), A2–0 = 0.852 s–1. For the band NO (3–0) – λ 1.8 μm, we have А3–0 = 0.067 s–1 (Schurin and Ellis, 1966; Rothman et al., 1983). The data from rocket and satellite measurements of the emission intensity of NO (1–0) 5.3 μm in the upper atmosphere can be found in the literature (Baker et al., 1977; Ulwick et al., 1985; Zachor et al., 1985; Adler-Golden et al., 1991; Ballard et al., 1993; Smith and Ahmadjin, 1993; Sharma et al., 1996a, 1996b, 1998; Sharma and Duff, 1997; Funke et al., 2005; Gardner et al., 2007; Mlynczak et al., 2010; Bermejo-Pantaleón et al., 2011; Sheese et al., 2013). According to these measurements, the thickness of the emitting layer of this emission at altitudes of ~125 km is 30 km. Theoretical concepts on the possible mechanisms of the origin of this emission can be found in the literature (Degges, 1971; Ogawa, 1976; Ogawa and Kondo, 1977; Baker et al., 1977; Witt et al., 1981).

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The formation of vibrationally excited NO molecules is mostly contributed by the reaction (Ogawa, 1976)

as well as by remission of the NO molecule from the level ν = 2. However, the efficiency of this process is much lower than that of fluorescence:

NO(ν = 0) + O → NO(ν = 1) + O, α NO,O = 6.5 × 10−11 exp − 2900 cm3 s −1. T Krasovskii (1971) showed that the formation of fast oxygen atoms can significantly increase the yield of this reaction at high latitudes during auroras. At heights below 100 km, the vibrational energy transfer to NO molecules from excited oxygen and nitrogen molecules may have a significant impact (Ogawa, 1976):

NO(ν = 0) + hν(λ2.7 μm) → NO(ν = 2), NO(ν = 2) → NO(ν = 1) + hν(λ5.4 μm).

)

(

In this case, the fluorescence occurs due to both the solar radiation with the excitation rate

⎞ cm3 s −1. α NO,N2 = 4.22 × 10−10 exp ⎛⎜ − 86.35 13 ⎟ ⎝ T ⎠ The vibrationally excited O2 and N2 molecules are generated through collisions with thermal electrons (Rusanov and Fridman, 1984):

−4 S = gS 5.3 exp ( −τChpχ ) , gS 5.3 = 1.0 × 10 s–1 (Ogawa, 1976), and the thermal radiation of the lower atmosphere with gT5.3 = 3.8 × 10–4 s–1 (Ogawa, 1976). Here, it was taken that the absorption coefficient is σNO,5.3 = 1.0 × 10–15 cm2. The optical thickness of τ5.3 is actually determined by the absorption of NO molecules, including up to heights of 80 km, because the attenuation due to Rayleigh scattering is small (σR = 5 × 10–31 cm2). Therefore, τ5.3 = σNO n(NO) HNO(Z). A quite similar relation holds also for 2.7-μm emission. In this case, gS2.7 = 3.1 × 10–4 s–1, gT2.7 = 2.3 × 10–9 s–1, σNO,5.3 = 1.0 × 10–15 cm2 (Degges, 1971). The contribution of transition (2–1) to the emission is small and can be disregarded. At daytime, the formation of NO (ν = 1, 2) is possible due to fluorescence in the ultraviolet transitions:

O2 + e → O2(ν) + e, σ O2,e = 1 × 10−17 cm2,

NO(ν = 0) + hν(γ; λ 0.226 μm)

NO(ν = 0) + O2(ν = 1) → NO(ν = 1) + O2, α NO,O2 = 2 × 10−14 exp − 460 cm3 s −1, T

( )

NO(ν = 0) + N2(ν = 1) → NO(ν = 1) + N2(ν = 0),

αO2,e = 1.1 × 10

−10

⎛ Te ⎞ ⎜ ⎟ ⎝1000 ⎠

0.5

⎛ ⎞ exp ⎜ − 2240 ⎟ cm3 s–1, ⎝ Te ⎠

N2 + e → N2(ν) + e, σ N2,e = 3 × 10−16 cm2, 0.5

⎛ 3380 ⎞ Te ⎞ 3 –1 ⎜ ⎟ exp ⎜ − ⎟ cm s . T ⎝1000 ⎠ ⎝ e ⎠ In addition, at altitudes above 100 km, there are reactions with nitrogen atoms that lead to excited NO molecules: α N2,e = 3.3 × 10

−11 ⎛

2 +

→ NO( A Σ , ν) → NO( X Π, ν = 1), 2

g γ1 = 3 × 10

−5

−1

s ,

NO(ν = 0) + hν(δ; λ 0.190 μm) → NO(C 2Π, ν) → NO(ν2Π, ν = 1), gδ1 = 2.5 × 10

−5

−1

s ,

NO(ν = 0) + hν(ε; λ 0.190 μm) 2 +

N( S) + O2 → NO(ν = 0 −10) + O, α N(S),O2 = 1.1 × 10−14T exp − 3151 cm3 s −1, T

→ NO(D Σ , e) → NO( X Π, ν = 1). In addition to the above-mentioned processes, the vibrational levels of the ground state of NO molecules can also become excited due to collisions with electrons:

N(2 D) + O2 → NO + O,

NO(ν = 0) + e → NO(ν = 1) + e,

4

)

(

α N(D),O2 = 7.4 × 10

−12

( ) T 300

0.5

3

−12

cm s ,

3

−1

It should be noted that the role of all of these processes is amplified during polar auroras. At heights of 80–110 km, the formation of 5.3-μm emission is predominantly contributed by fluorescence

0.5

⎛ Te ⎞ exp ⎛ − 5360 ⎞ cm3 s −1. ⎜ ⎟ ⎜ T ⎟ ⎝1000 ⎠ ⎝ e ⎠ It can be seen from these reaction rates that the contribution of excitation by electrons under normal conditions is much lower than the contribution due to other processes. Naturally, the excitation processes are concurrent with deactivation processes occurring when excited α NO,2,e = 1.8 × 10

cm s .

NO(ν = 0) + hν(λ5.3 μm) → NO(ν = 1)

0.5

⎛ ⎞ exp ⎜ − 2680 ⎟ cm3 s −1, T ⎝ e ⎠ NO(ν = 0) + e → NO(ν = 2) + e,

T α NO,1,e = 1.8 × 10−10 ⎜⎛ e ⎟⎞ ⎝1000 ⎠

−1

N(2 P) + O2 → NO + O, α N(P),O2 = 2.6 × 10

2

−10

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NO molecules collide with surrounding atoms and molecules (M):

believed to prevail over photoionization (Rothman et al., 1978)

NO(ν = 1) + M → NO(ν = 0),

NO + hν(λ ≤ 0.134 μm) → NO + e,

+

βNO,10 = 6.5 × 10−11 cm3 s −1,

−7

NO(ν = 2) + M → NO(ν = 1), βNO,21 = 3.0 × 10

−11

3

−1

cm s ,

NO(ν = 2) + M → NO(ν = 0), βNO,20 = 4.1 × 10−11 cm3 s −1,

NO + O2+ → NO+ + O2, βNO,O+ = 4.4 × 10−10 cm3 s −1.

as well as through photodissociation

2

NO + hν(λ ≤ 0.190 μm) → N + O, jNO,i = 1.34 × 10−5 s −1, which leads to the destruction of excited molecules (Nicolet, 1981). This mechanism is commonly

Q5.3

Reactions of collision with other ionized components of the atmosphere have much lower rates. From the reactions considered above, we can determine the volume intensity of NO 5.3-μm emission by the relation

{

}

= [NO] ⎡α NO,O[O] + α [O∗2 ] + α [N∗2 ] + S + gT 5.3 ⎤ NO,O*2 NO,N*2 ⎢⎣ ⎥⎦

The importance of nitric oxide 5.3-μm emission is associated with the involvement of NO in the excitation of atomic oxygen of 630-nm emission during intense red auroras, which leads to an energy release from the upper atmosphere. According to Krasovskii (1971), large geomagnetic disturbances and intensified red emissions lead to increased continuum intensity, which indicates that the content of NO molecules increases. The intensity of red emission increases because this emission is stimulated in the upper part of the ionospheric F2 layer, which is sufficiently heated due to the absorption of magnetohydrodynamic waves. The collisions of oxygen atoms collide with NO molecules create favorable conditions for the excitation of the O(1D) state. The section for recharge of atmospheric atomic ions with their neutral atoms is sufficiently large (~10–15 cm2). Therefore, the magnetohydrodynamic waves with a frequency of more than 1 Hz can be effectively absorbed in the upper ionosphere. In addition, infrared NO radiation cools the upper atmosphere. It is this fact that provides an efficient energy discharge from upper layers of the atmosphere. 3. MEASUREMENT RESULTS Rocket and satellite measurements of NO (1–0) 5.3-μm emission were conducted in a number of the studies mentioned above. The emission spectrum is shown in Fig. 1. Its characteristic feature is that the spectral distribution of rotational structure lines corresponds to a much higher temperature than the temperature of the ambient atmosphere. This is caused by GEOMAGNETISM AND AERONOMY

−1

jNO, ph = 5 × 10 s . However, it should be noted that Ogawa and Kondo (1977) used a photoionization rate of 1.38 × 10–6 s–1. In this context, it makes sense to note also the ionexchange reaction

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⎧⎪ βNO,10 [[O] + [O2 ] + [N2 ]] + βNO,O+[O2+ ]⎫⎪ 2 ⎨1 + ⎬. A 5.3 ⎪⎩ ⎪⎭

the small number of collisions during the radiation lifetime τr = 1 = 0.075 s of excited NO molecules A1−0 at the first vibrational level. The number of collisions is determined by the relation (Shefov et al., 2006)

Z r = τr [M]πσ2k 8kT , πμ where [M] is the concentration of molecules of the medium; k = 1.36 × 10–16 erg K–1 is the Boltzmann constant; πσ2 is the cross section of elastic scattering; mNOmM is the reduced mass, and mNO and mM μ= mNO + mM are the masses of relaxing and surrounding molecules, respectively. At the height of the maximum (123 km) of the emitting layer of (1–0) 5.3-μm emission, we have Zr = 5 (Fig. 2). 4. RESULTS AND DISCUSSION OF VARIATION REGULARITIES The published and available studies mainly describe the results of limb measurements of NO (1– 0) 5.3-μm emission intensity. An example of these data is shown in Fig. 2. Here, the intensity is given in rayleighs and in the linear scale of wavelengths, unlike the data used by us for analysis, which are given in watts and in a logarithmic scale. The profile of the height distribution of the volume intensity of 5.3-μm emission can be approximated as 2018

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1.0

Intensity

0.8 0.6 0.4 0.2 0 5.0

5.1

5.2

5.3

5.4 5.5 5.6 Wavelength λ, μm

5.7

5.8

5.9

6.0

6.1

Fig. 1. Calculated spectrum of NO (1–0) 5.3-μm emission band for rotational temperature of 488 K (at an emitting layer height of 123 km) obtained in the wavelength scale used in (Ballard et al., 1993).

200

⎡ ln 2(Z − Z 0 )2 ⎤ Q(Z ) = Qmax (Z 0 ) exp ⎢− ⎥ P 2W 2 ⎣ ⎦

Height Z, km

180

for the upper part of the emitting layer, where Q(Z) is given in photons/cm3, and

160 140

⎡ ln 2(Z − Z 0 )2 ⎤ Q(Z ) = Qmax (Z 0 ) exp ⎢− 2 2 ⎥ ⎣ (1 − P ) W ⎦

120 100 80 0

1 2 3 4 5 6 7 Volume intensity Q(Z), 105 photons cm–3 s–1

for the lower part, where Qmax(Z0) = 6.65 × 105 photons/cm3; the layer half-width is W = 29 km and the asymmetry parameter of the altitude profile of the layer is P = 0.62. The emitting layer intensity I = 1.9 Mrayleighs at the zenith for the indicated measurement conditions.

Limb height Z, km

200 180

4.1. Diurnal Variations

160

Limb satellite measurements of the 5.3-μm emission parameters by the MIPAS and SABER radiometers in the southern hemisphere (Smith and Ahmadjin, 1993) made it possible to determine the diurnal variations in its emission intensity and the emitting layer height at 125–130 km as a function of the solar zenith angle χ (Fig. 3).

140 120 100 80 0

20 40 60 80 Intensity I(Z), Mrayleighs

100

Fig. 2. Altitude limb profile of NO (1–0) 5.3-μm emission intensity (bottom) according to measurements at a latitude of 28.0° S and longitude of 102.6° E at 1900 local time (χ = 110°) on Apr. 29, 1991 on the CIRRIS-1A satellite (Sharma et al., 1996a). The upper panel shows the height distribution of the volume intensity of emission according to data of (Sharma et al., 1996b); the emitting layer intensity is 1.9 Mrayleighs.

In view of the small number of measurement data used, the dependencies of the emitting layer intensity and height on solar zenith angle can be approximated (in the first approximation) by the single harmonic

I = 0.9 + 2 cos χ, where I is given in Mrayleighs,

Z = 130 + 7 cos χ, where Z is expressed in km.

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I = 1.3 + 0.7cos 2π td , 365 where I is given in Mrayleighs.

3.5 3.0 2.5 2.0 1.5

135 130

125 120 0

where I is in Mrayleighs, Z = 129 + 11.5 cos 2(ϕ − 80) + 2.3 cos 4(ϕ + 29) + 2.0 cos 6(ϕ + 55) + 1.6 cos 8(ϕ + 49), where Z is in km,

T = 407 + 117 cos 2(ϕ − 86) + 18.2 cos 4(ϕ + 16) + 26.0 cos 6(ϕ + 55) + 7.9 cos 8(ϕ + 50), where Т is in K. 4.4. Analytical Relations between Given Parameters The measured parameters of the emitting layer of the NO molecule (intensity I (in Mrayleighs), layer height Z (in km) (Smith and Ahmadjian, 1993; Gardner et al., 2007), and temperature T (in K)) according to model data for the solar activity level (F10.7 = 161) at nighttime and daytime conditions are highly correlated. The cross-correlation of these parameters of the emitting layer is shown in Fig. 6. Vol. 58

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60 90 120 150 Solar zenith angle χ, deg

180

2.5

Intensity I, Mrayleighs

4.3. Latitudinal Variations The satellite measurements of NO 5.3-μm emission at various latitudes made it possible to estimate the latitudinal variations in the emission intensity and height at daytime (Smith and Ahmadjian, 1993) (Fig. 5). The resulting latitudinal variations of the intensity I and the heights of the emitting layer maximum Zmax and atmospheric temperature T at the height of the maximum according to the CIRA-72 model in the range of latitudes between 60° S and 60° N can be approximated as I = 1.83 + 1.33 cos 2(ϕ − 83) + 0.38 cos 4(ϕ + 12) + 0.54 cos 6(ϕ + 56) + 0.10 cos 8(ϕ + 52),

30

Fig. 3. Diurnal variations in intensity and height of the maximum of the emitting layer of NO 5.3-μm emission according to satellite measurement data (Smith and Ahmadjian, 1993) (dots); the solid lines indicate approximation curves.

2.0 1.5 1.0 0.5 0.0 130

Height Z, km

Z = 125 + 4.5 cos 2π td , 365 where Z is given in km.

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1.0 Height Z, km

4.2. Seasonal Variations The seasonal variations in the emitting layer parameters were rather approximate, because the studies describing the results of rocket and satellite measurements used by us in this paper (Gardner et al., 2007; Mlynczak et al., 2010; Shesse et al., 2013) present no measurement data on the intensity of nitrogen oxide emissions. The main focus in these experiments was the study of different variations in the concentration of unexcited NO molecules. Hence, the resulting seasonal variations (Fig. 4) are based on data derived from different studies. The approximation of these dependencies is limited to only a single harmonic of the form

Intensity I, Mrayleighs

SPATIAL AND TEMPORAL VARIATIONS OF INFRARED EMISSIONS

125

120

0

100 200 Days of the year td, days

300

Fig. 4. Seasonal variations in NO 5.3-μm emission intensity according to OSIRIS satellite measurements in the southern hemisphere (Shesse et al., 2013); the solid lines indicate data for northern hemispheric conditions. The dots stand for data of the studies (Smith and Ahmadjian, 1993; Gardner et al., 2007). 2018

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Intensity I, Mrayleighs

Temperature T, K

500 450 400 350 300

2.0 1.5 1.0 0.5 0 250

300

350 400 Temperature T, K

450

500

300

350 400 Temperature T, K

450

500

140

2.0 1.5 1.0 0.5 0 140

135 130 125 120 115 110 250

130

140

120 110 100 –90

–60

–30 0 30 Latitude ϕ, deg

60

90

Fig. 5. Latitudinal variations (the southern hemisphere) of intensity I and height of maximum of the emitting layer Zmax of NO (1–0) 5.3-μm emission according to Jun 14, 2003, MIPAS and SABER (Gardner et al., 2007) (dots) and Apr 29, 1991, CIRRIS (Smith and Ahmadjian, 1930 (squares) satellite measurements, as well as temperature T (F10.7 = 161) according to the CIRA-72 model. The solid lines indicate approximation curves.

Z = 125 + 8(I − 1.35), I = 1.35 + Z − 125 , r = 0.810 ± 0.122, 8

Height Z, km

Height Z, km

2.5

2.5 Height Z, km

Intensity I, Mrayleighs

250

3.0

135 130 125 120 115 110 0

0.5

1.0 1.5 2.0 Intensity I, Mrayleighs

2.5

3.0

Fig. 6. Correlation of the intensity and height of the emitting layer of NO 5.3-μm emission according to measurements for the southern hemisphere on Jun 14, 2003, by the MIPAS and SABER satellites (Gardner et al., 2007) (dots) and the CIRRIS satellite for the northern and southern hemispheres on Apr 29, 1991 (Smith and Ahmadjian, 1993) (squares), as well as the same parameters with a temperature (F10.7 = 161) according to the CIRA-72 model.

3.0 Intensity I, Mrayleighs

Z = 88 + T − 375 , 10.2 T = 375 + 10.2(Z − 125), r = 1, T = 375 + 82(I − 1.43), I = 1.43 + T − 375 , r = 0.811 ± 0.121. 82 4.5. Dependence on Solar Activity Level The effect of solar activity was obtained from satellite measurement data given by Mlynczak et al. (2010) (Fig. 7, denoted as dots). The solid line indicates approximation by the formula

2.5 2.0 1.5 1.0 0.5 0 60

80

100

120 140 F10.7

160

180

200

Fig. 7. Dependence of NO 5.3-μm emission intensity on solar activity level according to data of Mlynczak et al. (2010) (dots). The solid line indicates the approximation curve.

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3 , F 1 + exp − 10.7 − 110 33 where I is in Mrayleighs. This relation describes the dependence of NO 5.3-μm emission intensity on solar activity up to F10.7 = 150. This is explained by the fact that no data on emission intensity are currently available for higher values of solar activity. I=

(

)

5. CONCLUSIONS Vibrationally excited nitrogen molecules, which form an emitting layer at lower thermospheric heights, significantly affect the process of energy release from the atmosphere under increased geomagnetic activity. Their role increases significantly with increased solar activity. The systematization and analysis of existing data on the characteristics of the layer of NO 5.3-μm emission obtained from rocket and satellite data allowed us to obtain analytical expressions that describe the statistical regularities of variations in the height distribution of emission intensity, seasonal and latitudinal behavior, and its dependence on solar activity level. We obtained analytic relationships to describe the relationship between the NO 5.3-μm emission intensity, the emitting layer height, and atmospheric temperature at the heights of this emission. The dependence of this emission intensity on solar activity has a clearly expressed nonlinear character. Thus, the long-term satellite and rocket data collected and systematized by us on infrared emission of the nitric oxide molecule made it possible to identify a number of spatial and temporal variations of different types that can be used further to develop empirical models for infrared emission variations in the middle and upper atmosphere. ACKNOWLEDGMENTS This work was supported by the Russian Foundation for Basic Research, project no. 16-05-00120. REFERENCES Adler-Golden, S.M., Matthew, M.W., and Smith, D.R., Upper atmospheric infrared radiance from CO2 and no observed during the SPIRIT 1 rocket experiment, J. Geophys. Res., 1991, vol. 96, no. A7, pp. 11319–11329. Baker, K.D., Baker, D.J., Ulwick, J.C., and Stair, A.T., Measurements of 1.5- to 5.3-μm infrared enhancements associated with a bright auroral breakup, J. Geophys. Res., 1977, vol. 82, no. 25, pp. 3518–3528. Ballard, J., Kerridge, B.J., Morris, P.E., and Taylor, F.W., Observations of ν = 1–0 emission from thermospheric nitric oxide by ISAMS, Geophys. Res. Lett., 1993, vol. 20, no. 12, pp. 1311–1314. GEOMAGNETISM AND AERONOMY

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Bermejo-Pantaleón, D., Funke, B., López-Puertas, M., García-Comas, M., Stiller, G.P., von Clarmann, T., Linden, A., Grabowski, U., Höpfner, M., Kiefer, M., Glatthor, N., Kellmann, S., and Lu, G., Global observations of thermospheric temperature and nitric oxide from MIPAS spectra at 5.3 μm, J. Geophys. Res., 2011, vol. 116, A10313. doi 10.1029/2011JA016752 Degges, T.C., Vibrationally excited nitric oxide in the upper atmosphere, Appl. Opt., 1971, vol. 10, no. 8, pp. 1856– 1860. Funke, B., López-Puertas, M., von Clarmann, T., Stiller, G.P., Fischer, H., Glatthor, N., Grabowski, U., Höpfner, M., Kellmann, S., Kiefer, M., Linden, A., Tsidu, G.M., Milz, M., Steck, T., and Wang, D.Y., Retrieval of stratospheric NOx from 5.3 and 6.2 μm nonlocal thermodynamic equilibrium emissions measured by Michelson Interferometer for Passive Atmospheric Sounding (MIPAS) on Envisat, J. Geophys. Res., 2005, vol. 110, D09302. doi 10.1029/2004JD005225 Gardner, J.L., Funke, B., Mlynczak, M.G., López-Puertas, M., Martin-Torres, F.J., Russell, J.M., Miller, S.M., Sharma, R.D., and Winick, J.R., Comparison of nighttime nitric oxide 5.3 μm emissions in the thermosphere measured by MIPAS and SABER, J. Geophys. Res., 2007, vol. 112, A10301. doi 10.1029/2006JA011984 Gilmore, F.R., Potential energy curves for N2, NO, O2 and corresponding ions, J. Quant. Spectrosc. Radiat. Transfer, 1965, vol. 5, no. 2, pp. 369–390. Krasovskii, V.I., Shtili i shtormy v verkhnei atmosfere (Calms and Storms in the Upper Atmosphere), Moscow: Nauka, 1971. Mlynczak, M.G., Hunt, L.A., Marshall, B.T., Martin-Torres, F.J., Mertens, C.J., Russell, J.M., Remsberg, E.E., López-Puertas, M., Picard, R., Winick, J., Wintersteiner, P., Thompson, R.E., and Gordley, L.L., Observations of infrared radiative cooling in the thermosphere on daily to multiyear timescales from the TIMED/SABER instrument, J. Geophys. Res., 2010, vol. 115, A03309. doi 10.1029/2009JA014713 Nicolet, M., The solar spectral irradiance and its action in the atmospheric photodissociation processes, Planet. Space Sci., 1981, vol. 29, no. 9, pp. 951–974. Ogawa, T., Excitation processes of infrared atmospheric emissions, Planet. Space Sci., 1976, vol. 24, no. 8, pp. 749–756. Ogawa, T. and Kondo, Y., Diurnal variability of thermospheric N and NO, Planet. Space Sci., 1977, vol. 25, no. 8, pp. 735–742. Rothman, L.S., Clough, S.A., McClatchey, R.A., Young, L.G., Snider, D.E., and Goldman, A., AFGL trace gas compilation, Appl. Opt., 1978, vol. 17, no. 4, p. 507. Rothman, L.S., Goldman, A., Gillis, J.R., Gamache, R.R., Pickett, H.M., Poynter, R.L., Husson, N., and Chedin, A., AFGL trace gas compilation: 1982 version, Appl. Opt., 1983, vol. 22, no. 11, pp. 1616–1627. Rusanov, V.D. and Fridman, A.A., Fizika khimicheski aktivnoi plazmy (Physics of the Chemically Active Plasma), Moscow: Nauka, 1984. Schurin, B. and Ellis, R.E., First and second-overtone intensity measurements for CO and NO, J. Chem. Phys., 1966, vol. 45, no. 7, pp. 2528–2532. 2018

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GEOMAGNETISM AND AERONOMY

Translated by V. Arutyunyan

Vol. 58

No. 2

2018