Solar Wind Turbulence Around Mars: Relation Between The Energy Cascade Rate And The Proton Cyclotron Waves Activity. (arXiv:2007.09476v2 [physics.space-ph] UPDATED)
<a href="http://arxiv.org/find/physics/1/au:+Andres_N/0/1/0/all/0/1">Nahuel Andr&#xe9;s</a>, <a href="http://arxiv.org/find/physics/1/au:+Romanelli_N/0/1/0/all/0/1">Norberto Romanelli</a>, <a href="http://arxiv.org/find/physics/1/au:+Hadid_L/0/1/0/all/0/1">Lina Z. Hadid</a>, <a href="http://arxiv.org/find/physics/1/au:+Sahraoui_F/0/1/0/all/0/1">Fouad Sahraoui</a>, <a href="http://arxiv.org/find/physics/1/au:+DiBraccio_G/0/1/0/all/0/1">Gina DiBraccio</a>, <a href="http://arxiv.org/find/physics/1/au:+Halekas_J/0/1/0/all/0/1">Jasper Halekas</a>

The first estimation of the incompressible energy cascade rate at
magnetohydrodynamic (MHD) scales is obtained in the plasma upstream of the
Martian bow shock, using MAVEN observations and an exact relation derived for
MHD turbulence. The energy cascade rate is computed for events with and without
proton cyclotron wave (PCW) activity, for time intervals when MAVEN was in the
solar wind with no magnetic connection to the bow shock. It is shown that the
nonlinear cascade of energy at the MHD scales is slightly amplified when PCWs
are present in the plasma. The analysis of the normalized cross helicity and
residual energy for the turbulent fluctuations shows the presence of Alfv’enic
and non-Alfv’enic fluctuations in a magnetic dominant regime for the majority
of the cases.

The first estimation of the incompressible energy cascade rate at
magnetohydrodynamic (MHD) scales is obtained in the plasma upstream of the
Martian bow shock, using MAVEN observations and an exact relation derived for
MHD turbulence. The energy cascade rate is computed for events with and without
proton cyclotron wave (PCW) activity, for time intervals when MAVEN was in the
solar wind with no magnetic connection to the bow shock. It is shown that the
nonlinear cascade of energy at the MHD scales is slightly amplified when PCWs
are present in the plasma. The analysis of the normalized cross helicity and
residual energy for the turbulent fluctuations shows the presence of Alfv’enic
and non-Alfv’enic fluctuations in a magnetic dominant regime for the majority
of the cases.

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