tokens: cut through the current sheet in turbulence, the parameters depend on time due to the turbulent interaction of larger scale magnetic eddies, so wide variation in parameters across different current sheets and at different times is expected. 7 DISCUSSION AND CONCLUSIONS As a result of the weak collisionality of many space and astrophysical plasmas, several physical processes can locally contribute to the dissipation of energy and the heating of the plasma. During magnetic reconnection, magnetic energy is efficiently converted to directed plasma flows, thermal energy, and energetic particles (Burch et al. 2016 ; Torbert et al. 2018 ). During turbulence in a magnetized plasma, the cascade provides the global amount of energy needed for fluctuations to be dissipated at small scales (Marino et al. 2008 ). However, which dissipative mechanisms are dominant and under which conditions is still not sufficiently understood (Vaivads et al. 2016 ). Therefore, a multiplicity of dissipation surrogates have been adopted in the literature to identify potential sites of dissipation. Owing to the strongly non-linear dynamics and the importance of physics at kinetic scales in such systems, numerical simulations of the Vlasov–Maxwell system (or, including collisions, the Boltzmann–Maxwell system) are the decisive tool to address the long-standing issue of plasma heating and energy dissipation in magnetized plasmas, e.g. Parashar et al. ( 2009 ). For example, the ‘turbulence dissipation challenge’ (Parashar et al. 2015 ) motivated numerical work to compare different algorithms on the solution of similar problems to assess the nature of the dissipation in magnetized turbulence (e.g. Pezzi et al. 2017 ; Perrone et al. 2018 ; González et al. 2019 ). In the same spirit, we have conducted a survey of a number of dissipation surrogates with three different kinetic plasma codes – the fully kinetic particle-in-cell vpic , the fully kinetic Eulerian Vlasov–Maxwell Gkeyll , and the Eulerian Hybrid Vlasov–Maxwell codes – to perform numerical simulations of two important physical phenomena in plasma physics. The first class investigates reconnection in an isolated current sheet, and the second concerns plasma turbulence at kinetic scales. We have calculated and compared eight distinct dissipation proxies, delineated in Section 2 . For the sake of clarity, we have categorized them in terms of (i) energy-based parameters, whose definition describes energy transfer and conversion; and (ii) VDF-based parameters, that are directly related to kinetic signatures in the particle VDF. Energy-based parameters considered here are the power density by electromagnetic fields on charged particles (Zenitani et al. 2011 ), the pressure–strain interaction (Yang et al. 2017a ), and a local proxy of the turbulent energy transfer (Sorriso-Valvo et al. 2018a ). The VDF-based parameters are the local pressure agyrotropy (Swisdak 2016 ) and three measures describing how different a local
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