Stokes parameters of the O VI 103.2 NM line as a probe of the matter velocity field vector in the solar wind acceleration region

Details Stokes parameters of the O VI 103.2 NM line as a probe of the matter velocity field vector in the solar wind acceleration region Stokes parameters of the O VI 103.2 NM line as a probe of the matter velocity field vector in the solar wind acceleration region

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992esasp.344...81s&link_type=abstract

In ESA, Solar Physics and Astrophysics at Interferometric Resolution p 81-85 (SEE N93-10901 01-90)

Physics

5

Parameter Identification, Plasma Acceleration, Solar Wind, Solar Wind Velocity, Stokes Theorem (Vector Calculus), Velocity Distribution, Doppler Effect, Line Spectra, Polarimetry, Polarization (Waves), Solar Corona, Solar Physics

Scientific paper

A theoretical method to determine the matter velocity field vector in the solar wind acceleration region is presented. The O VI 103.2 nm line should be observed high in the corona in the solar wind acceleration region. Preliminary results show that the interpretation of polarimetric data, associated to the shift and the Doppler dimming effect, provided that the partial anisotropy of the incidence radiation field be taken into account, should offer a method of diagnostic of the complete velocity field vector which is currently missing and which is indispensable to understand the acceleration mechanisms of the solar wind and to develop a dynamical modelization of the solar structures.

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