Solar Wind Turbulence around Mars: MAVEN observations

We estimate for the first time the signed incompressible energy cascade rate (direct and inverse) at magnetohydrodynamic (MHD) scales in the pristine solar wind, upstream from Mars' bow shock. For this, we apply third-moment theory for fully developed turbulence to more than five years of Mars Atmosphere and Volatile EvolutioN (MAVEN) magnetic field and plasma observations. From our statistical results, we also conclude that the incompressible energy cascade rate decreases as the Martian heliocentric distance increases, for each of the three explored Martian years. We also suggest that the presence of proton cyclotron waves, associated with the extended Martian hydrogen exosphere, do not have a significant effect on the nonlinear cascade of energy at the MHD scales.