Physics
Scientific paper
Sep 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999jgr...10419765f&link_type=abstract
Journal of Geophysical Research, Volume 104, Issue A9, p. 19765-19772
Physics
55
Interplanetary Physics: Solar Wind Plasma, Interplanetary Physics: Mhd Waves And Turbulence, Interplanetary Physics: Sources Of The Solar Wind
Scientific paper
Recent observations have shown that small magnetic loops are continuously emerging within supergranules in the solar photosphere. The subsequent reconnection of this emerging flux with field lines which open into the corona should define the Poynting's vector and mass flux into the corona. These two quantities uniquely determine the final energy flow and speed of the steady, fast solar wind. It is also pointed out that if the consequence of the emergence of new flux and its reconnection is lateral displacements of coronal magnetic field lines, this process should increase the magnetic field energy in the corona in a definable manner. The resulting dissipation of this energy, by work done on the plasma or by Joule heating, defines the spatial distribution for the heating of the corona. A simple model is constructed that yields profiles for the acceleration of the fast solar wind and for coronal temperatures that are reasonable.
Fisk Len A.
Schwadron Nathan A.
Zurbuchen Thomas H.
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