Identifying Compressive Fluctuations In Inertial Range Solar Wind
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Identifying Compressive Fluctuatio In Inertial Range Solar Wind K.G. Klein 1 , G.G. Howes 1 , S.D. Bale 2 , C.H.K. Chen 2 , C.S. Salem 2 , J.M. TenBarge 1 1 University of Iowa 2 University of California, Berkeley • C(δn, δB || ) from ~1.2x10 5 WIND data intervals is ~-1 • Correlation implies that a preponderance of the compressive energy is due to slow waves • Lack of fast waves may have implications for in dissipation range SHINE session: The Dissipation of Solar Wind Turbulence Correlation of density and parallel magnetic fluctuations: Points from WIND data, Lines from synthetic data model.
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Identifying Compressive Fluctuations In Inertial Range Solar Wind. K.G. Klein 1 , G.G. Howes 1 , S.D. Bale 2 , C.H.K. Chen 2 , C.S. Salem 2 , J.M. TenBarge 1. 1 University of Iowa 2 University of California, Berkeley. SHINE session: The Dissipation of Solar Wind Turbulence. - PowerPoint PPT Presentation
Transcript of Identifying Compressive Fluctuations In Inertial Range Solar Wind
Identifying Compressive Fluctuations In Inertial Range Solar WindK.G. Klein1, G.G. Howes1, S.D. Bale2, C.H.K. Chen2, C.S. Salem2, J.M. TenBarge1 1University of Iowa 2University of California, Berkeley
• C(δn, δB||) from ~1.2x105 WIND data intervals is ~-1
• Correlation implies that a preponderance of the compressive energy is due to slow waves
• Lack of fast waves may have implications for in dissipation range
SHINE session: The Dissipation of Solar Wind Turbulence
Correlation of density and parallel magnetic fluctuations:Points from WIND data, Lines from synthetic data model.