The aerosol layer of the lower thermosphere: III. Observation in absence of the Moon and under large Sun’s zenith angles

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Resumo

The results of the “Terminator” space experiment on board the International Space Station are given. Observations have been realized under limb geometry in the visual and near infrared ranges of the spectrum in absence of the Moon and under large Sun’s zenith angles (>145°). The treatment of the obtained digital photos has shown that our previous conception of the scattering mechanism of the observed emission layer to be faulty in absence of sun’s backlight. In the present paper the emission of the observed layer is considered as thermal radiation of meteoric particles, preheated to 2000–3000 K on entering the atmosphere.

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Sobre autores

A. Belyaev

Fedorov Institute of Applied Geophysics (IPG)

Autor responsável pela correspondência
Email: anb52@mail.ru
Rússia, Moscow

S. Nikolaishvili

Fedorov Institute of Applied Geophysics (IPG)

Email: ser58ge@mail.ru
Rússia, Moscow

A. Omel’chenko

Fedorov Institute of Applied Geophysics (IPG)

Email: alexom@mail.ru
Rússia, Moscow

A. Repin

Fedorov Institute of Applied Geophysics (IPG)

Email: repin_a_yu@mail.ru
Rússia, Moscow

M. Poluarshinov

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

Email: mikhail.poluarshinov@rsce.ru
Rússia, Korolev

Yu. Smirnov

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

Email: yury.v.smirnov@rsce.ru
Rússia, Korolev

A. Strakhov

Scientific Production Enterprise Robis (NPP Robis)

Email: lexand@robis.ru
Rússia, Moscow

A. Batishchev

National Research Nuclear University Moscow Engineering Physical Institute (MEPhI)

Email: alexey-batschev@mail.ru
Rússia, Moscow

V. Stasevich

Scientific Production Enterprise Robis (NPP Robis)

Email: walter@robis.ru
Rússia, Moscow

Yu. Platov

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

Email: yplatov@mail.ru
Rússia, Moscow, Troitsk

Bibliografia

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2. Fig. 1. Positions of the ISS and the photographed region of the atmosphere at the moments of shooting: 09:32:27 UTC (1), 11:05:17 UTC (2), 12:38:07 UTC (3), 14:10:57 UTC (4), 15:43:47 UTC (5), 17:16:37 UTC (6).

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3. Fig. 2. Photographs of the luminous SAS in three ranges (upper – 540 ± 5 nm, middle – 700 ± 5 nm, lower – 830 ± 5 nm).

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4. Fig. 3. Altitude profile of the brightness of the luminous SAS at a wavelength of 700 nm.

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5. Fig. 4. Vertical brightness profiles of the luminous SAS. Dashed line – 540 ± 5 nm, thin continuous – 830 ± 5 nm, thick continuous – 700 ± 5 nm. The numbering of the graphs corresponds to the numbering in Fig. 1.

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6. Fig. 5. Vertical brightness profiles of the luminous SAS, corrected for the spectral sensitivity of the matrix. Dashed line – 540 ± 5 nm, thin continuous – 830 ± 5 nm, thick continuous – 700 ± 5 nm. The numbering of the graphs corresponds to the numbering in Fig. 1.

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7. Fig. 6. Vertical profiles of the volumetric luminosity of the SAS. Dashed line – 540 ± 5 nm, thin continuous – 830 ± 5 nm, thick continuous – 700 ± 5 nm. The numbering of the graphs corresponds to the numbering in Fig. 1.

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