Temporal and Spatial Variations of Heliospheric X-Ray Emissions Associated with Charge Transfer of the Solar Wind with Interstellar Neutrals

Details Temporal and Spatial Variations of Heliospheric X-Ray Emissions Associated with Charge Transfer of the Solar Wind with Interstellar Neutrals Temporal and Spatial Variations of Heliospheric X-Ray Emissions Associated with Charge Transfer of the Solar Wind with Interstellar Neutrals

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh21a11r&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH21A-11

Physics

2102 Corotating Streams, 2144 Interstellar Gas, 2164 Solar Wind Plasma, 7554 X Rays, Gamma Rays, And Neutrinos

Scientific paper

X-rays should be generated throughout the heliosphere as a consequence of charge transfer collisions between heavy solar wind ions and interstellar neutrals. The high charge state solar wind ions resulting from these collisions are left in highly excited states and emit extreme ultraviolet or soft X-ray photons. This solar wind charge exchange mechanism applied to cometary neutrals has been used to explain the soft X-ray emission observed from comets. Originally a simple model was developed that demonstrated that heliospheric X-ray emission can account for about 25-50 percent of the observed soft X-ray background intensities. Both the solar wind and the interstellar neutrals in this model were assumed to be spherically symmetric and time independent. A more complex model has now been developed to take into account temporal and spatial variations of the solar wind and interstellar neutrals and to allow for co-rotation of the sun. Measured time histories of the solar wind proton flux are used in the model and the results are compared with "long term enhancements" in the soft X-ray background measured by ROSAT for the same time period. We have also calculated time independent spatial maps across the sky of the heliospheric X-ray emission.

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