Upper-atmosphere carbon dioxide is altering satellite orbits

Physics Today ◽  
2012 ◽  
Keyword(s):  
Carbon Dioxide ◽  
Upper Atmosphere ◽  
Satellite Orbits

scholarly journals Mariner 6: Ultraviolet spectrum of Mars upper atmosphere

1971 ◽  
Vol 40 ◽  
pp. 253-256 ◽  
Author(s):  
C. A. Barth ◽  
W. G. Fastie ◽  
C. W. Hord ◽  
J. B. Pearce ◽  
K. K. Kelly ◽  
...  
Keyword(s):  
Carbon Dioxide ◽  
Carbon Monoxide ◽  
Spectral Region ◽  
Atomic Hydrogen ◽  
Atomic Oxygen ◽  
Ultraviolet Spectrum ◽  
Upper Atmosphere

Emission features from ionized carbon dioxide and carbon monoxide were measured in the 1900- to 4300-Å spectral region. The Lyman-α 1216-Å line of atomic hydrogen and the 1304-, 1356-, and 2972-Å lines of atomic oxygen were observed.

Variation of Upper-Atmosphere Density with Latitude and Season: Further Evidence from Satellite Orbits

Nature ◽  
1960 ◽  
Vol 185 (4715) ◽  
pp. 727-729 ◽  
Author(s):  
D. G. KING-HELE ◽  
D. M. C. WALKER
Keyword(s):  
Upper Atmosphere ◽  
Satellite Orbits ◽  
Atmosphere Density

scholarly journals Photodissociation of Carbon Dioxide in the Mars Upper Atmosphere

1974 ◽  
Vol 29 (2) ◽  
pp. 185-188
Author(s):  
Charles A. Barth
Keyword(s):  
Carbon Dioxide ◽  
Carbon Monoxide ◽  
Atomic Oxygen ◽  
Emission Rate ◽  
Upper Atmosphere ◽  
Emission Rates ◽  
Laboratory Measurements

Photodissociation of carbon dioxide produces O (1S) atoms and CO (a3Π) molecules in the Mars upper atmosphere. Calculations of the emission rate of the atomic oxygen 2972 Å line and the carbon monoxide Cameron bands produced by the photodissociation mechanism are factors of 3 and 10, respectively, smaller than the emission rates observed by Mariner ultraviolet spectrometers. Laboratory measurements are needed to understand the discrepancies.

scholarly journals Influence of gravity waves on the climatology of high-altitude Martian carbon dioxide ice clouds

2018 ◽  
Author(s):  
Erdal Yiğit ◽  
Alexander S. Medvedev ◽  
Paul Hartogh
Keyword(s):  
Carbon Dioxide ◽  
High Altitude ◽  
Gravity Waves ◽  
General Circulation ◽  
Middle Atmosphere ◽  
Circulation Model ◽  
Upper Atmosphere ◽  
Cloud Formation ◽  
Ice Clouds ◽  
Ice Cloud

Abstract. Carbon dioxide (CO2) ice clouds have been routinely observed in the middle atmosphere of Mars. However, there are still uncertainties concerning physical mechanisms that control their altitude, geographical, and seasonal distributions. Using the Max Planck Institute Martian General Circulation Model (MPI-MGCM), incorporating a state-of-the-art whole atmosphere subgrid-scale gravity wave parameterization (Yiğit et al., 2008), we demonstrate that internal gravity waves generated by lower atmospheric weather processes have wide reaching impact on the Martian climate. Globally, GWs cool the upper atmosphere of Mars by ~10 % and facilitate high-altitude CO2 ice cloud formation. CO2 ice cloud seasonal variations in the mesosphere and the mesopause region appreciably coincide with the spatio-temporal variations of GW effects, providing insight into the observed distribution of clouds. Our results suggest that GW propagation and dissipation constitute a necessary physical mechanism for CO2 ice cloud formation in the Martian upper atmosphere during all seasons.

scholarly journals The Thermosphere Responds to a Weaker Than Normal Solar Cycle

Eos ◽  
2019 ◽  
Vol 100 ◽  
Author(s):  
Aaron Sidder
Keyword(s):  
Nitric Oxide ◽  
Carbon Dioxide ◽  
Solar Cycle ◽  
Solar Radiation ◽  
Upper Atmosphere ◽  
Incoming Solar Radiation ◽  
Infrared Emissions

Infrared emissions from nitric oxide and carbon dioxide in Earth’s upper atmosphere, which are closely tied to incoming solar radiation, are drastically lower than in the previous solar cycle.

scholarly journals Drivers of Upper Atmosphere Climate Change

Eos ◽  
2020 ◽  
Vol 101 ◽  
Author(s):  
Sarah Stanley
Keyword(s):  
Climate Change ◽  
Magnetic Field ◽  
Carbon Dioxide ◽  
Upper Atmosphere ◽  
Earth’S Magnetic Field ◽  
Temperature Trends ◽  
Earth's Magnetic Field ◽  
New Research

New research confirms the influence of carbon dioxide on long-term temperature trends in the upper atmosphere, but changes in Earth’s magnetic field also play a key role.

Density of the Upper Atmosphere from Analysis of Satellite Orbits: Further Results

Nature ◽  
1959 ◽  
Vol 184 (4695) ◽  
pp. 1267-1270 ◽  
Author(s):  
D. G. KING-HELE
Keyword(s):  
Upper Atmosphere ◽  
Satellite Orbits

Earth's thermospheric evolution and implications for planetary habitability

2020 ◽  
Author(s):  
Colin Johnstone
Keyword(s):  
Carbon Dioxide ◽  
Solar Wind ◽  
Chemical Composition ◽  
Solar System ◽  
Planetary Atmospheres ◽  
Upper Atmosphere ◽  
The Sun ◽  
The Earth ◽  
First Time ◽  
Planetary Habitability

<p>During the Archean eon from 3.8 to 2.5 billion years ago, the Earth's upper atmosphere and interactions with the magnetosphere and the solar wind were likely significantly different to how it is today due to major differences in the chemical composition of the atmosphere and the younger Sun being signifcantly more active. Understanding these factors is important for understanding the evolution of planetary atmospheres within our solar system and beyond. While the higher activity of the Sun would have caused additional heating and expansion of the atmosphere, geochemical measurements show that carbon dioxide was far more abundant during this time and this would have led to significantly thermospheric cooling which would have protected the atmosphere from losses to space. I will present a study of the effects of the carbon dioxide composition and the Sun's activity evolution on the thermosphere and ionosphere of the Archean Earth, studying for the first time the effects of different scenarios for the Sun's activity evolution. I will show the importance of these factors for the exosphere and escape processes of the Earth and terrestrial planets outside our solar system.</p>

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