The energetics of the slow solar wind
L. Ofman
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. I will present recent
results of three-fluid numerical models of the slow solar wind heating
and acceleration in coronal streamers. I will discuss the possible heating
mechanisms of electrons, protons, and heavy ions in the slow wind,
and the formation of open flux in streamers. I will show the relation
of the numerical results to past observations by SOHO, and Ulysses
spacecraft, and future observations with Solar B.
Correspondence
Leon Ofman (leon.ofman@gsfc.nasa.gov), Catholic University of America
presentation
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