Effect of the solar wind velocity field vector on the polarization of the O VI λ1032 coronal line

Details Effect of the solar wind velocity field vector on the polarization of the O VI λ1032 coronal line Effect of the solar wind velocity field vector on the polarization of the O VI λ1032 coronal line

Jun 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.508..471r&link_type=abstract

In: Proceedings of the SOHO 11 Symposium on From Solar Min to Max: Half a Solar Cycle with SOHO, 11-15 March 2002, Davos, Switze

Computer Science

Polarization, Resonance Scattering, Solar Wind

Scientific paper

The linear polarization parameters of the O VI λ1032 coronal line (D2 line) are measured by using spectropolarimetric observations performed by the SUMER spectrometer on board the SoHO spacecraft during activity minimum of the solar cycle (March, 1996), in the south coronal hole. The interpretation of the determined polarization parameters in terms of the macroscopic velocity field vector of the O VI coronal ions (which can be assimilated to the solar wind velocity field) gives constraints on the strength and direction of the solar wind velocity field vector. They are obtained by comparing the numerical and the observational results of the linear polarization parameters of the O VI D2 coronal line.

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