2017/10/31 by Lina Hadid, Fouad Sahraoui, Sebastien Galtier +1 · 2 citations
Physics and Astronomy · #physics.space-ph #astro-ph.EP #astro-ph.SR
paper · pdf · doi:10.1103/physrevlett.120.055102
published as Phys. Rev. Lett. 120, 055102 (2018)
arxiv created 2017/12/19 · arxiv updated 2018/02/07
The first estimation of the energy cascade rate |εC| of magnetosheath turbulence is obtained using the CLUSTER and THEMIS spacecraft data and an exact law of compressible isothermal magnetohydrodynamics turbulence. |εC| is found to be of the order of 10-13 J.m3.s-1, at least two orders of magnitude larger than its value in the solar wind (order of 10-16 J.m3.s-1 in the fast wind). Two types of turbulence are evidenced and shown to be dominated either by incompressible Alfvénic or magnetosonic-like fluctuations. Density fluctuations are shown to amplify the cascade rate and its spatial anisotropy in comparison with incompressible Alfvénic turbulence. Furthermore, for compressible magnetosonic fluctuations, large cascade rates are found to lie mostly near the linear kinetic instability of the mirror mode. New empirical power-laws are evidenced and relate |εC| to the turbulent Mach number and the internal energy. These new finding have potential applications in distant astrophysical plasmas that are not accessible to in situ measurements.