Open AccessKinetic and Hydrodynamic Models of the Solar Wind and Polar Wind: A Focus Group of the Solar‐Terrestrial Interactions From Microscale to Global Models (STIMM‐2) Workshop; Sinaia, Romania, 13 and 15 June 2007
Author(s) -
Lemaire J. F.,
Echim M.
Publication year - 2008
Publication title -
eos, transactions american geophysical union
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 0.316
H-Index - 86
eISSN - 2324-9250
pISSN - 0096-3941
DOI - 10.1029/2008eo090006
Subject(s) - solar wind , polar wind , magnetopause , kinetic energy , physics , microscale chemistry , corona (planetary geology) , coronal mass ejection , atmospheric sciences , meteorology , environmental science , plasma , astrobiology , classical mechanics , mathematics education , mathematics , quantum mechanics , venus
Following the publication of the first hydrodynamic models of the “solar wind” (supersonic neutral outstream of solar charged particles) in 1958, and the “solar breeze” (the evaporation of solar particles with a subsonic mean velocity) in 1960, scientists for decades have debated about which description most accurately models the acceleration of particles leaving the solar corona. This debate tends to pit magnetohydrodynamic oriented scientists against holders of a more kinetic description, particularly regarding the mechanisms by which ions and electrons evaporate from the solar corona. A rather similar controversy started in 1969 about hydrodynamic and kinetic modeling of the “polar wind,” which streams out from the terrestrial polar caps.