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We calculate the severe radiative energy losses which occur at the base ofblack hole jets using a relativistic fluid jet model, including in-situacceleration of non-thermal leptons by magnetic reconnection. Our resultsdemonstrate that including a self-consistent treatment of radiative energylosses is necessary to perform accurate MHD simulations of powerful jets andthat jet spectra calculated via post-processing are liable to vastlyoverestimate the amount of non-thermal emission. If no more than 95% of theinitial total jet power is radiated away by the plasma travels as it travelsalong the length of the jet, we can place a lower bound on the magnetisation ofthe jet plasma at the base of the jet. For typical powerful jets, we find thatthe plasma at the jet base is required to be highly magnetised, with at least10,000 times more energy contained in magnetic fields than in non-thermalleptons. Using a simple power-law model of magnetic reconnection, motivated bysimulations of collisionless reconnection, we determine the allowed range ofthe large-scale average reconnection rate along the jet, by restricting thetotal radiative energy losses incurred and the distance at which the jet firstcomes into equipartition. We calculate analytic expressions for the cumulativeradiative energy losses due to synchrotron and inverse-Compton emission alongjets, and derive analytic formulae for the constraint on the initialmagnetisation.

Using radiative energy losses to constrain the magnetisation and magnetic reconnection rate at the base of black hole jets