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Implications of the Stagnation Line Model for energy input through the dayside magnetopause
Author(s) -
Pudovkin Mikhail I.,
Semenov Vladimir S.,
Heyn Martin F.,
Biernat Helfried K.
Publication year - 1986
Publication title -
geophysical research letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.007
H-Index - 273
eISSN - 1944-8007
pISSN - 0094-8276
DOI - 10.1029/gl013i003p00213
Subject(s) - magnetopause , physics , solar wind , magnetosphere , interplanetary magnetic field , magnetosheath , geophysics , flux (metallurgy) , computational physics , mechanics , magnetic field , materials science , quantum mechanics , metallurgy
Based on the formation of a stagnation line at the magnetopause the electromagnetic energy transport from the solar wind into the dayside magnetosphere is analyzed. The resulting energy flux is proportional to v ∞ B ∞ ² sin² (θ ∞ ‐ ϕ ∞ ), where v ∞ and B ∞ are the solar wind speed and magnetic field and θ ∞ ‐ ϕ ∞ is the angle between the IMF and the stagnation line projected into the interplanetary space. A stagnation line parallel to the separator gives approximately the sin 4 (θ ∞ /2) energy flux dependence of Akasofu's ε‐index.