Observed Versus Modeled O 1356 Å and N2 LBH Emissions from the Earth's Space Environment

Details Observed Versus Modeled O 1356 Å and N2 LBH Emissions from the Earth's Space Environment Observed Versus Modeled O 1356 Å and N2 LBH Emissions from the Earth's Space Environment

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsa51c1963h&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SA51C-1963

Physics

[0355] Atmospheric Composition And Structure / Thermosphere: Composition And Chemistry, [7900] Space Weather

Scientific paper

The O/N2 ratio, which can be derived from the O 1356 Å to N2 LBH (Lyman-Birge-Hopfield) emission ratio, is frequently used to quantify changes in the state of Earth's space environment. The brightness of these emissions also provides important constraints on the state of the space environment and its drivers, e.g., the solar irradiance. In this work, the observed O 1356 Å and LBH emissions from the GUVI (Global Ultraviolet Imager) on the TIMED (Thermosphere Ionosphere Mesosphere Energetics and Dynamics) satellite is compared to the calculated O 1356 Å and LBH emissions from the GLOW model. These comparisons allow us to examine the agreement between the observed and calculated emissions as well as their dependence on the emission cross sections. GUVI observations from 2010-2011 and coincident with solar irradiance observations from the Solar Dynamics Observatory (SDO), both at 30 second cadence, are used in the analysis. In addition, recent experimental excitation cross-section data are used to determine the N2 LBH brightness and its ratio to O 1356 Å. The observed 1356/LBH emission ratio (which is proportional to the O/N2 ratio) is approximately half that calculated, while the calculated emissions are both brighter than those observed. While uncertainties in both the calibrations of the instruments and the neutral densities of the atmosphere may contribute to the lack of agreement, the differences in the emission ratios indicate a need for better O 1356 Å emission cross sections.

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