The Energetics of the Slow Solar Wind

Details The Energetics of the Slow Solar Wind The Energetics of the Slow Solar Wind

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aspc..369..569o&link_type=abstract

New Solar Physics with Solar-B Mission ASP Conference Series, Vol. 369, proceedings of the conference held 8-11 November, 2005 a

Physics

1

Scientific paper

Observations and numerical models show that the slow solar wind is associated with coronal streamers. However, the exact heating and acceleration mechanism of the slow wind is unknown. Moreover, the energization mechanism is likely to be different for electrons, protons, and heavy ions. Some of the main objectives of Solar-B is to understand the opening of magnetic field and heating of the coronal plasma that forms the solar wind. Recent results of three-fluid numerical models of the slow solar wind heating and acceleration in coronal streamers are shown. The possible heating mechanisms of electrons, protons, and heavy ions in the slow wind, and the formation of open flux in streamers is discussed. The relation of the numerical results to past observations by SOHO, and Ulysses spacecraft, and future observations with Solar-B is discussed.

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