Comparison of the results of theoretical calculations of night glow intensity with measurement data obtained by both ground-based methods and from space shuttles

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The integral luminosity values of the Herzberg I, Chamberlain and Atmospheric bands at mid-latitudes and in the equatorial zone of the Earth are calculated. The correlation of the results of theoretical calculations of the intensity of excited molecular oxygen glow on Earth with experimental data on the night glow of O2 obtained from space shuttles, from the ground-based Kitt Peak Observatory (USA) for the Herzberg I and Chamberlain bands is discussed. For the Atmospheric bands, the correlation of the results of theoretical calculations with similar calculations based on measurement data from the ground-based Keck Observatory (USA) is analyzed. The integral luminosity values of the Herzberg I and Atmospheric bands for the northern latitudes of Mars are calculated.

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作者简介

O. Antonenko

Polar Geophysical Institute (PGI)

编辑信件的主要联系方式.
Email: antonenko@pgia.ru
俄罗斯联邦, Apatity

A. Kirillov

Polar Geophysical Institute (PGI)

Email: antonenko@pgia.ru
俄罗斯联邦, Apatity

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2. Fig. 1. Altitude profiles of O concentrations: Panel (a) – dark lines according to measurements [1] at mid-latitudes of the Earth for the 1st, 4th, 7th and 10th months; light lines – data from NRLMSISE-00 for the same conditions; (b) – dark lines – data obtained from the TIMED satellite in the region of the Earth’s equator (April, August) and in the northern tropics (autumn, winter) [15]; light lines – data from NRLMSISE-00; (c) – dark lines – data for the atmosphere of Mars obtained from the SPICAM IR spectrometer for orbits at points Ls ≈ 152.1°, Ls ≈ 164.5°, 82° S of Mars [9]; light lines – data from LMD-MGCM; (g) – LMD-MGCM data for the equatorial region and 67° N of Mars, for points Ls ≈ 180° and Ls ≈ 0° [16]

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3. Fig. 2. Panel (a) – experimental data obtained from the Endeavour space shuttle [14] in the 620–900 nm range (Atmospheric bands); (b) – calculated values of the integrated luminosity of the Atmospheric bands for the Earth’s atmosphere for mid-latitudes (55.7° N) for the 10th month of 1986; (c) – calculated values for the equatorial zone and northern tropics of the Earth (23° N) for the autumn period of 1995; (d) – experimental data from the Discovery shuttle, December 1992 in the 300–870 nm range (Chamberlain bands); (d) – calculated values of the integrated luminosity of the Chamberlain bands for the Earth's atmosphere for midlatitudes (55.7° N) for the 10th month of 1986; (e) – calculated values for the equatorial zone and northern tropics of the Earth (23° N) for the autumn period of 1995.

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4. Fig. 3. Panel (a) – experimental data obtained from the space shuttle Endeavour [14] in the range of 620–900 nm (Atmospheric bands); (b) – calculated values of the integrated luminosity of the Atmospheric bands for the atmosphere of Mars at a latitude of 67° N at Ls ≈ 180°

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5. Fig. 4. Panel (a) – experimental data obtained from the EbertFastie spectrograph in the range of 300–370 nm (Kitt Peak Observatory); (b) – experimental data obtained with the EbertFastie spectrograph in the range of 360–440 nm; (c) – calculated values of the integrated luminosity of the Herzberg I bands for the middle latitudes of the Earth; (d) – calculated values of the integrated luminosity of the Chamberlain bands for the middle latitudes of the Earth

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6. Fig. 5. Panel (a) – calculated values of the intensity of the Atmospheric Bands for the middle latitudes of the Earth (55.7° N) for the 1st month of 1986; (b) – data from measurements performed by the High Resolution Spectrograph (HIRES) on the Keck I telescope [28]; (c) – results of calculations for the equatorial zone including the northern tropics (23° N), for the winter period of 1995.

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