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Momentum transfer from solar wind to interplanetary field enhancements inferred from magnetic field draping signatures
Author(s) -
Lai H. R.,
Russell C. T.,
Jia Y. D.,
Wei H. Y.,
Angelopoulos V.
Publication year - 2015
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 - 10.1002/2015gl063302
Subject(s) - interplanetary magnetic field , solar wind , physics , magnetopause , field line , bow shock (aerodynamics) , computational physics , mercury's magnetic field , magnetic field , magnetic cloud , plasma , coronal mass ejection , field (mathematics) , interplanetary spaceflight , geophysics , astrophysics , mechanics , shock wave , nuclear physics , mathematics , quantum mechanics , pure mathematics
Characterized by a cusp‐shaped enhancement in the magnetic field strength, the magnetic structure in the solar wind, called an interplanetary field enhancement (IFE), has been investigated since its discovery. To understand its three‐dimensional magnetic field geometry, we study an IFE detected by five spacecraft simultaneously. Field lines are seen draping around in the upstream region and rotating in the ambient convection electric field direction in the downstream region. Earlier studies suggest that IFEs are created when the solar wind accelerates newly formed dust clouds. Both signatures found in our study support this hypothesis: the field line draping is caused by dust‐solar wind momentum exchange, while the field line rotation is a typical signature of dusty plasma pickup. The force that exchanges the momentum is approximately 10 6 N. This study illustrates the nature of the interaction between two flowing plasmas of very different mass‐to‐charge ratio.