Scaling laws in solar wind MHD turbulence

Details Scaling laws in solar wind MHD turbulence Scaling laws in solar wind MHD turbulence

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010eguga..1214850m&link_type=abstract

EGU General Assembly 2010, held 2-7 May, 2010 in Vienna, Austria, p.14850

Computer Science

Scientific paper

Incompressible and isotropic magnetohydrodynamic turbulence in plasmas can be described by an exact relation for the energy flux through the scales. This Yaglom-like scaling law has been recently observed in the fast solar wind above the solar poles, where the turbulence is in an Alfvénic state, as well as in the ecliptic by separating fast (Alfvénic) and slow (non Alfvénic) stream. The results provides insights on the nature of solar wind turbulence, on its implications for energy transfer and heating, and on the role of Alfvénicity in the formation of the magnetohydrodynamic turbulent cascade.

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