I.R. Radiation of the upper atmosphere

Gordiet︠s︡, B. F.; Markov, M. N.; Shelepin, L. A.

doi:10.1016/0032-0633(78)90076-4

Cited by 36 publications

(11 citation statements)

References 34 publications

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“…The model also includes neutral gas molecular heat conduction, IR cooling in the vibrational-rotational bands of CO 2 (15 m), CO, and O 3 and in the 63 m O line, and turbulent energy dissipation and heat conduction. The volume heating and cooling rates for the processes included in the simulations and the heating rates due to photodissociation are discussed in detail by Gordiets et al (1977Gordiets et al ( , 1978Gordiets et al ( , 1982 and Gordiets and Kulikov (1985). IR emission of CO 2 in the 15 m band is the major cooling agent in the lower thermospheres of Venus, Earth, and Mars (e.g., Dickinson, 1972Dickinson, , 1984Gordiets et al, 1982;Gordiets and Kulikov, 1985;Dickinson et al, 1987;Bougher et al, 1999Bougher et al, , 2000Kulikov et al, 2006).…”

Section: Numerical Modeling Of Thermospheric Heat Budgetsmentioning

confidence: 98%

“…The most important heating and cooling processes in the upper atmosphere of Earth are summarized as follows (e.g., Izakov 1971;Blum et al, 1972;Dickinson, 1972Dickinson, , 1984Dickinson et al, 1974;Chandra and Sinha, 1974;Gridchin et al, 1975;Gordiets et al, 1978Gordiets et al, , 1982Kulikov, 1981, 1985;Dickinson et al, 1987;Crowley, 1991;Bauer and Lammer, 2004): heating due to N 2 , O 2 , and O photoionization by solar (or stellar) XUV ( Յ102.7 nm), heating due to O 2 and O 3 photodissociation by solar ultraviolet radiation, chemical heating in exothermic reactions with O and O 3 , neutral gas heat conduction, IR cooling in the vibrational-rotational bands of CO 2 , NO, O 3 , OH, NO ϩ , 14 N 15 N, CO, O 2 , etc., and heating and cooling due to contraction and expansion of the thermosphere (to model the thermosphere diurnal variations), as well as turbulent energy dissipation and heat conduction. Gordiets et al (1982) applied a numerical model to calculate the thermal budget of the Earth's upper atmosphere in the altitude range of 90-500 km by including the main energy sources and sinks, such as IR radiative cooling in the vibrational-rotational bands of NO, CO 2 , OH, and O 3 , as well as heating and cooling arising from dissipation of turbulent energy and eddy heat transport.…”

Section: Thermospheric Heating Due To X-rays and Euv Radiationmentioning

confidence: 99%

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Coronal Mass Ejection (CME) Activity of Low Mass M Stars as An Important Factor for The Habitability of Terrestrial Exoplanets. II. CME-Induced Ion Pick Up of Earth-like Exoplanets in Close-In Habitable Zones

et al. 2007

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Atmospheric erosion of CO2-rich Earth-size exoplanets due to coronal mass ejection (CME)-induced ion pick up within close-in habitable zones of active M-type dwarf stars is investigated. Since M stars are active at the X-ray and extreme ultraviolet radiation (XUV) wave-lengths over long periods of time, we have applied a thermal balance model at various XUV flux input values for simulating the thermospheric heating by photodissociation and ionization processes due to exothermic chemical reactions and cooling by the CO2 infrared radiation in the 15 microm band. Our study shows that intense XUV radiation of active M stars results in atmospheric expansion and extended exospheres. Using thermospheric neutral and ion densities calculated for various XUV fluxes, we applied a numerical test particle model for simulation of atmospheric ion pick up loss from an extended exosphere arising from its interaction with expected minimum and maximum CME plasma flows. Our results indicate that the Earth-like exoplanets that have no, or weak, magnetic moments may lose tens to hundreds of bars of atmospheric pressure, or even their whole atmospheres due to the CME-induced O ion pick up at orbital distances

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Section: Numerical Modeling Of Thermospheric Heat Budgetsmentioning

confidence: 98%

Section: Thermospheric Heating Due To X-rays and Euv Radiationmentioning

confidence: 99%

Coronal Mass Ejection (CME) Activity of Low Mass M Stars as An Important Factor for The Habitability of Terrestrial Exoplanets. II. CME-Induced Ion Pick Up of Earth-like Exoplanets in Close-In Habitable Zones

et al. 2007

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“…The most important heating and cooling processes in the upper atmosphere of Earth can be summarized as follows (e.g., Izakov 1971;Dickinson 1972;Chandra and Sinha 1974;Gridchin et al 1975;Gordiets et al 1978Gordiets et al , 1979Gordiets andKulikov 1981, 1982;Gordiets et al , 1987Gordiets 1991;Dickinson et al 1987): 1) heating due to CO 2 , N 2 , O 2 , and O photoionization by the solar XUV radiation (λ ≤ 102.7 nm), 2) heating due to O 2 and O 3 photodissociation by the solar UV radiation, 3) chemical heating in exothermic binary and 3-body reactions, 4) neutral gas molecular heat conduction, 5) turbulent energy dissipation and heat conduction, 6) heating and cooling due to contraction and expansion of the thermosphere, 7) IR-cooling in the vibrational-rotational bands of CO 2 , NO, O 3 , OH, NO + , 14 N 15 N, CO, etc. Gordiets et al (1979, applied a numerical model to calculate the thermal budget of the Earth's thermosphere in the altitude range of 90-500 km.…”

Section: Thermospheric Heat Balance and Composition Modellingmentioning

confidence: 99%

“…It takes into account heating due to the CO 2 , N 2 , O 2 , CO, and O photoionization by the XUV-radiation (λ ≤ 102.7 nm), heating due to O 2 and O 3 photodissociation by solar UV-radiation, chemical heating in exothermic 3-body reactions, neutral gas molecular heat conduction, IR-cooling in the vibrational-rotational bands of CO 2 (15 μm), CO, O 3 , and in the 63 μm O line, and turbulent energy dissipation and heat conduction. We use the volume heating and cooling rates for the processes included in our simulations and the heating rates owing to photodissociation which are discussed in detail by Gordiets et al (1978Gordiets et al ( , 1979 and . The lower boundary conditions for the system of 1-D time-dependent hydrodynamic equations modelling the termosphere are…”

Section: Thermospheric Heat Balance and Composition Modellingmentioning

confidence: 99%

A Comparative Study of the Influence of the Active Young Sun on the Early Atmospheres of Earth, Venus, and Mars

et al. 2007

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Because the solar radiation and particle environment plays a major role in all atmospheric processes such as ionization, dissociation, heating of the upper atmospheres, and thermal and non-thermal atmospheric loss processes, the long-time evolution of planetary atmospheres and their water inventories can only be understood within the context of the evolving Sun. We compare the effect of solar induced X-ray and EUV (XUV) heating on the upper atmospheres of Earth, Venus and Mars since the time when the Sun arrived at the Zero-Age-Main-Sequence (ZAMS) about 4.6 Gyr ago. We apply a diffusive-gravitational equilibrium and thermal balance model for studying heating of the early thermospheres by photodissociation and ionization processes, due to exothermic chemical reactions and cooling by IR-radiating molecules like CO 2 , NO, OH, etc. Our model simulations result in extended thermospheres for early Earth, Venus and Mars. The exospheric temperatures obtained for all the three planets during this time period lead to diffusion-limited hydrodynamic escape of atomic hydrogen and high Jeans' escape rates for heavier species like H 2 , He, C, N, O, etc. The duration of this blow-off phase for atomic hydrogen depends essentially on the mixing ratios of CO 2 , N 2 and H 2 O in the atmospheres and could last from ∼100 to several hundred million years. Furthermore, we study the efficiency of various non-thermal atmospheric loss processes on Venus and Mars and investigate the possible protecting effect of the early martian magnetosphere against solar wind induced ion pick up Yu.N. Kulikov et al. erosion. We find that the early martian magnetic field could decrease the ion-related nonthermal escape rates by a great amount. It is possible that non-magnetized early Mars could have lost its whole atmosphere due to the combined effect of its extended upper atmosphere and a dense solar wind plasma flow of the young Sun during about 200 Myr after the Sun arrived at the ZAMS. Depending on the solar wind parameters, our model simulations for early Venus show that ion pick up by strong solar wind from a non-magnetized planet could erode up to an equivalent amount of ∼250 bar of O + ions during the first several hundred million years. This accumulated loss corresponds to an equivalent mass of ∼1 terrestrial ocean (TO (1 TO ∼1.39 × 10 24 g or expressed as partial pressure, about 265 bar, which corresponds to ∼2900 m average depth)). Finally, we discuss and compare our findings with the results of preceding studies.

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“…The detailed study of the various mechanisms of vibrational excitation of molecules in the upper atmosphere was first carried out by Gordiets et al (18). Since then, much attention has been paid to theoretical examination of thermospheric emissions in vibrational molecular bands.…”

Section: History Of the Problemmentioning

confidence: 99%

Excitation of vibrational emission bands in aurora and airglow

Gordiet︠s︡¹

1986

Can. J. Phys.

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The major results of the theoretical study of infrared radiation in the vibrational-rotational bands of minor molecular constituents in the terrestrial thermosphere are reviewed. Various mechanisms of vibrational excitation of radiating molecules are discussed for both quiet and disturbed conditions (e.g., aurorally enhanced electric fields, etc.). Intensities of infrared emissions and correlations between some of them and emissions in other spectral regions are analyzed, as well as the role that infrared radiation plays in the thermospheric energetics.On revoit les principaux rtsultats de I'Ctude theorique du rayonnement infrarouge dans les bandes de vibration-rotation des constituants molCculaires mineurs dans la thermosphkre terrestre. On discute differents mecanismes d'excitation vibrationnelle des molCcules rayonnantes, dans des conditions paisibles ou perturbees (champs Clectriques intensifies par I'aurore, par exemple, etc ...). Les intensites des Cmissions infrarouges, ainsi que les corrClations entre certaines d'entre elks et les Cmissions dans d'autres regions spectrales sont analysCes, de m&me que le r61e jouC par le rayonnement infrarouge dans I'CnergCtique thermospherique.[Traduit par la revue]Can. J. Phys. 64. 1673 (1986)

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I.R. Radiation of the upper atmosphere

Cited by 36 publications

References 34 publications

Coronal Mass Ejection (CME) Activity of Low Mass M Stars as An Important Factor for The Habitability of Terrestrial Exoplanets. II. CME-Induced Ion Pick Up of Earth-like Exoplanets in Close-In Habitable Zones

Coronal Mass Ejection (CME) Activity of Low Mass M Stars as An Important Factor for The Habitability of Terrestrial Exoplanets. II. CME-Induced Ion Pick Up of Earth-like Exoplanets in Close-In Habitable Zones

A Comparative Study of the Influence of the Active Young Sun on the Early Atmospheres of Earth, Venus, and Mars

Excitation of vibrational emission bands in aurora and airglow

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