Implications of Saito's coronal density model on the polar solar wind flow and heavy ion abundances

Details Implications of Saito's coronal density model on the polar solar wind flow and heavy ion abundances Implications of Saito's coronal density model on the polar solar wind flow and heavy ion abundances

Mar 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976ssim.conf..108f&link_type=abstract

In NASA. Goddard Space Flight Center Proc. of the Symp. on the Study of the Sun and Interplanetary Medium in Three Dimensions

Physics

Heavy Ions, Mathematical Models, Proton Flux Density, Solar Activity, Solar Corona, Solar Wind, Astronomical Models, Comets, Ecliptic, Electron Energy, Latitude, Lyman Spectra, Solar Physics, Solar Protons

Scientific paper

A comparison of polar solar wind proton flux upper limits derived using a coronal density model, with Lyman alpha measurements of the length of the neutral H tail of comet Bennet at high latitudes, shows that either extended heating beyond 2 solar radii is necessary some of the time or that the model's polar densities are too low. Whichever possibility is the case, the fact that the solar wind particle flux does not appear to decrease with increasing latitude indicates that the heavy element content of the high latitude wind may be similar to that observed in the ecliptic. It was then shown that solar wind heavy ion observations at high latitudes allow a determination of the electron temperature at heights which bracket the nominal location of the coronal temperature maximum thus providing information concerning the magnitude and extent of mechanical dissipation in the intermediate corona.

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