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In solar wind, magnetohydrodynamic (MHD) discontinuities are ubiquitous andoften found to be at the origin of turbulence intermittency. They may also playa key role in the turbulence dissipation and heating of the solar wind. Thetangential (TD) and rotational (RD) discontinuities are the two most importanttypes of discontinuities. Recently, the connection between turbulenceintermittency and proton thermodynamics has been being investigatedobservationally. Here we present numerical results from three-dimensional MHDsimulation with pressure anisotropy and define new methods to identify and todistinguish TDs and RDs. Three statistical results obtained about the relativeoccurrence rates and heating effects are highlighted: (1) RDs tend to take upthe majority of the discontinuities along with time; (2) the thermal statesembedding TDs tend to be associated with extreme plasma parameters orinstabilities, while RDs do not; (3) TDs have a higher average T as well asperpendicular temperature $T_\perp$. The simulation shows that TDs and RDsevolve and contribute to solar wind heating differently. These results willinspire our understanding of the mechanisms that generate discontinuities andcause plasma heating.

the astrophysical journal. letters

Occurrence Rates and Heating Effects of Tangential and Rotational  Discontinuities as Obtained from Three-dimensional Simulation of  Magnetohydrodynamic Turbulence