Imaging the three-dimensional solar wind flow in EUV

Details Imaging the three-dimensional solar wind flow in EUV Imaging the three-dimensional solar wind flow in EUV

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsh41b1133g&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SH41B-1133

Physics

2124 Heliopause And Solar Wind Termination, 2126 Heliosphere/Interstellar Medium Interactions, 2164 Solar Wind Plasma, 2194 Instruments And Techniques, 7549 Ultraviolet Emissions

Scientific paper

Charge exchange collisions between the solar wind alpha particles and heliospheric atomic hydrogen produce a unique emission in the 30.4-nm line. All-sky images in this emission with high spectral resolution could reveal the three-dimensional flow properties of the solar wind, including the flow in the regions over the sun's poles. The initial concept of solar wind imaging in EUV was based on a simplistic solar wind flow model with the effective solar magnetic dipole aligned with the sun spin axis and correspondingly a sharp boundary between fast and slow solar wind flows under the solar minimum conditions [Gruntman, J. Geophys. Res., 106, 8205-8216, 2001]. In this work, we make the next step in defining the concept of heliosphere imaging in EUV by simulating images of a realistic three-dimensional solar wind with the effective magnetic dipole tilted with respect to the sun spin axis and resulting in a complex truly three-dimensional flow pattern of the solar wind plasma. The results of simulations establish the sensitivity requirements (a number of all-sky images needed per year) for an experiment to image the global solar wind.

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