Understanding kinetic dissipative processes in the solar wind is an important endeavor required to improve our global solar wind models. The candidate dissipative processes must be collisionless in nature and should produce the observed signature of perpendicular anisotropy for protons. Many processes have been proposed e.g. wave-particle interactions, energization at intermittent coherent structures and stochastic heating. We will discuss two efforts related to this line of research:
1) Turbulent Dissipation Challenge: A community driven effort that aims to better quantify the relative contributions of various dissipative processes in the solar wind.
2) Effect of electron equation of state on the kinetics of protons.