AbstractCollisionless shocks in astrophysical plasmas are important thermalizers, converting some of the incident flow energy into thermal energy, and non‐thermalizers, partitioning that energy in unequal ways to different particle species, subpopulations thereof, and field components. This partition problem, or equivalently the shock equation of state, lies at the heart of shock physics. Here, we employ systematically a framework to capture all the incident and downstream energy fluxes at two example traversals of the Earth's bow shock by the Magnetospheric Multiscale Mission. Here and traditionally, such data has to be augmented by information from other spacecraft, for example, to provide more accurate measurements of the cold solar wind beam. With some care and fortuitous choices, the total energy flux is conserved, including instantaneous measurements through the shock layer. The dominant incident proton ram energy is converted primarily into downstream proton enthalpy flux, the majority of which is actually carried by a small fraction of suprathermal protons. Fluctuations include both real and instrumental effects. Separating these, resolving the solar wind beam, and other considerations point the way to a dedicated mission to solve this energy partition problem across a full range of plasma and shock conditions.
