The Aerosol Layer of the Lower Thermosphere: II. Observation Under the Full Moon

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Abstract

The results of the “Terminator” space experiment on board the International Space Station are given. Images of the Earth atmosphere are obtained in the near IR spectral range at limb-geometry of observations under the full Moon. The calculated vertical profiles of volume emission/scattering rate point that the aerosol layer occurs within the height region of 80 – 100 km in the Earth atmosphere. It is proposed that this layer is of meteoric origin. Estimations show that the size spectrum of aerosol particles lies within the region of 1 – 100 nm.

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About the authors

A. N. Belyaev

Fedorov Institute of Applied Geophysics (IPG)

Author for correspondence.
Email: anb52@mail.ru
Russian Federation, Moscow

S. Sh. Nikolaishvili

Fedorov Institute of Applied Geophysics (IPG)

Email: ser58ge@gmail.ru
Russian Federation, Moscow

A. N. Omel’chenko

Fedorov Institute of Applied Geophysics (IPG)

Email: alexom@mail.ru
Russian Federation, Moscow

A. Yu. Repin

Fedorov Institute of Applied Geophysics (IPG)

Email: repin_a_yu@mail.ru
Russian Federation, Moscow

M. A. Poluarshinov

S.P. Korolev Rocket and Space Corporation Energia (RKK Energia)

Email: mikhail.poluarshinov@rsce.ru
Russian Federation, Korolev, Moscow oblast

Yu. V. Smirnov

S.P. Korolev Rocket and Space Corporation Energia (RKK Energia)

Email: yury.v.smirnov@rsce.ru
Russian Federation, Korolev, Moscow oblast

A. V. Strakhov

Scientific Production Enterprise Robis (NPP Robis)

Email: lexand@robis.ru
Russian Federation, Moscow

A. G. Batishchev

National Research Nuclear University Moscow Engineering Physical Institute (MEPhI)

Email: alexey-batschev@mail.ru
Russian Federation, Moscow

V. I. Stasevich

Scientific Production Enterprise Robis (NPP Robis)

Email: walter@robis.ru
Russian Federation, Moscow

Yu. V. Platov

Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation (IZMIRAN), Russian Academy of Sciences

Email: yplatov@mail.ru
Russian Federation, Moscow, Troitsk

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Supplementary files

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2. Fig. 1. ISS trajectory (dashed line) and position of the registered SAS (continuous thick line) during the session on 07.03.2023.

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3. Fig. 2. (a) Photograph of the atmosphere in the 700 ± 5 nm wavelength range taken from the ISS RS on 07.03.2023 at 13:49:26 UTC. (b) Photograph of the atmosphere in the wavelength range 830 ± 5 nm, taken from the ISS RS on 07.03.2023 at 13:49:26 UTC.

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4. Fig. 3. Actual and calculated positions of the SAS on the camera matrices. Crosses (camera No. 4) and circles (camera No. 3) indicate the position of the brightest pixels in the central part of the observed layer (see Table 2). The thin line corresponds to the projection with α=17.3°+0.0°, β=5.66°+1.64°=7.3°, θ=72.0°. The thick line is the projection with α=17.3°-0.63°=16.67°, β=5.66°+3.34°=9.0°, θ=72.0°.

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5. Fig. 4. Averaged vertical brightness profiles of the atmosphere. The thick line indicates the vertical brightness profiles of the atmosphere in the wavelength interval 700 ± 5 nm, the thin line - in the interval 830 ± 5 nm. The brightness profiles were constructed from the images taken on 07.03.2023 at the time points: 10:43:46 UTC (a), 13:49:26 UTC (b), 15:22:26 UTC (c).

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6. Fig. 5. The same atmospheric brightness profiles as in Fig. 4, but after subtracting the background component.

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7. Fig. 6. Vertical profiles of the atmospheric bulk luminosity as a result of moonlight scattering calculated from the corresponding luminosity profiles in Fig. 5.

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8. Fig. 7A1. Perspective projection on the matrix plane. T is the camera sensor plane; S is the projection center; SM is the optical axis of the camera lens; the length of the SM segment is equal to its focal length f , M is the main point of the sensor, i.e., the point of intersection of the optical axis O with the T sensor plane.

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9. Fig. 8A2. Position of the photodetector matrix (M) relative to the cone of the visible horizon.

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