TIMED-SABER Observations of the Influence of Auroral Electron Dosing on Nighttime 4.3 um Emission

Details TIMED-SABER Observations of the Influence of Auroral Electron Dosing on Nighttime 4.3 um Emission TIMED-SABER Observations of the Influence of Auroral Electron Dosing on Nighttime 4.3 um Emission

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmsa23b..02m&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SA23B-02

Physics

0310 Airglow And Aurora, 2407 Auroral Ionosphere (2704), 2419 Ion Chemistry And Composition (0335), 2427 Ionosphere/Atmosphere Interactions (0335), 2455 Particle Precipitation

Scientific paper

The large thermospheric infrared radiance enhancements observed from the TIMED-SABER experiment during recent solar storms provide an exciting opportunity to study the influence of solar-geomagnetic disturbances on the upper atmosphere and ionosphere. In particular, nighttime enhancements of 4.3 um emission, due to vibrational excitation and prompt radiative emission by NO+, provide an excellent proxy to study and analyze the response of the ionospheric E-region to auroral electron dosing. Essential to this analysis is the removal of the CO2 contribution to 4.3 um emission. In principle, nighttime CO2 4.3 um emission can be accurately modeled using SABER-retrieved temperature, pressure (and possibly CO2 volume mixing ratios derived from daytime scans), and the SABER non-LTE CO2 and forward radiance models. However, auroral electron dosing may have an indirect effect on CO2 4.3 um emission through the near resonant V-V transfer between the CO2 4.3 um fundamental band and vibrationally excited N2, since N2 is also vibrationally excited by inelastic electron collisions and E-region chemical reactions. In this paper, we assess the impact of the indirect effect of auroral dosing on 4.3 um emission using 4.3 um limb radiance measurements and temperature, pressure data products from SABER, SABER non-LTE CO2 and radiation transfer algorithms, simulations from the field- line interhemispheric plasma (FLIP) model, and auroral electron energy characteristics derived from the NOAA/POES instrument.

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