Open AccessAcceleration of the fast solar wind by the emergence of new magnetic flux
Author(s) -
Fisk L. A.,
Schwadron N. A.,
Zurbuchen T. H.
Publication year - 1999
Publication title -
journal of geophysical research: space physics
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 1.67
H-Index - 298
eISSN - 2156-2202
pISSN - 0148-0227
DOI - 10.1029/1999ja900256
Subject(s) - nanoflares , physics , corona (planetary geology) , solar wind , coronal mass ejection , coronal radiative losses , coronal cloud , magnetic reconnection , coronal loop , photosphere , computational physics , interplanetary magnetic field , magnetic flux , magnetic energy , acceleration , magnetic field , astrophysics , classical mechanics , magnetization , quantum mechanics , astrobiology , venus
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.