Determining exospheric hydrogen density by reconciliation of H-alpha measurements with radiative transfer theory

Details Determining exospheric hydrogen density by reconciliation of H-alpha measurements with radiative transfer theory Determining exospheric hydrogen density by reconciliation of H-alpha measurements with radiative transfer theory

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993jgr....9821611h&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 98, no. A12, p. 21,611-21,626

Physics

13

Atmospheric Models, Exosphere, Gas Density, Geocoronal Emissions, H Alpha Line, Hydrogen, Radiative Transfer, Resonance Scattering, Balmer Series, Lyman Beta Radiation, Mathematical Models, Solar Flux Density

Scientific paper

The singly scattered resonant fluorescent component of the geocoronal Balmer-alpha (H-alpha) emission is obtained by subtracting the multiply scattered component of H-alpha, determined by a radiative-transfer (RT) model, from H-alpha measurements. Exospheric column abundance then follows a striaghtforward single-scattering calculation. The reality of that abundance depends upon the validity of the model exosphere used by the RT model, upon the validity of the estimated solar Ly-beta flux, and upon the statistical measurement errors. Iterative adjustments of the hydrogen density (H) profile input to the RT model, converging to a best fit to H-alpha observations, generate a unique atmosphere best matching model intensity to measured H-alpha brightness. Applying this method to ground-based measurements of the geocoronal H-alpha emission made at Arecibo, Peurto Rico, in 1988, we find that the best estimated multiply and singly scattered components of H-alpha are about 85 and 60%, respectively, in excess of the initial model values, while the derived (H) is generally in agreement with the initial model (H) is generally in agreement with the initial model (H) at lower altitudes and about 35% higher than the initial model (H) at higher altitudes.

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