High Resolution Measurements and Modeling of Auroral Hydrogen Emission Line Profiles

Details High Resolution Measurements and Modeling of Auroral Hydrogen Emission Line Profiles High Resolution Measurements and Modeling of Auroral Hydrogen Emission Line Profiles

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsa52a0391l&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SA52A-0391

Physics

0310 Airglow And Aurora, 2407 Auroral Ionosphere (2704), 2455 Particle Precipitation

Scientific paper

Measurements in the visible at high spectral resolution (1.3 A) have been made at Longyearbyen, Svalbard (15.8E, 78.2N), during an interval of intense proton precipitation, The shape and Doppler shift of Hydrogen Balmer beta line profiles have been compared with model line profiles, using as input ion energy spectra from almost coincident passes of the FAST and DMSP spacecraft. The comparison shows that the simulation contains the important physical processes that produce the profiles, and confirms that measured changes in the shape and peak wavelength of the hydrogen profiles are the result of changing energy input. This combination of high resolution measurements with modeling provides a direct method of estimating the incoming energy and changes in flux of precipitating protons over Svalbard. Whereas for electron precipitation information of the incident particles is derived from brightness and brightness ratios which require at least two spectral windows, for proton precipitation the Doppler profile of resulting hydrogen emission is directly related to the energy and flux of the incident energetic protons and can be used to gather information about the source region. As well as the expected Doppler shift to shorter wavelengths, the measured profiles have a significant red shifted component, the result of upward flowing hydrogen atoms.

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