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Magnetic reconnection is often invoked to explain the non-thermal radiationof relativistic outflows, including jets of active galactic nuclei (AGN).Motivated by the largely unknown plasma composition of AGN jets, we studyreconnection in the unexplored regime of electron-positron-proton (pair-proton)plasmas with large-scale two-dimensional particle-in-cell simulations. We covera wide range of pair multiplicities (lepton-to-proton number ratio$\kappa=1-199$) for different values of the all-species plasma magnetization($\sigma=1,3$ and 10) and electron temperature ($\Theta_e\equivkT_e/m_ec^2=0.1-100$). We focus on the dependence of the post-reconnectionenergy partition and lepton energy spectra on the hot pair plasma magnetization$\sigma_{e,h}$ (i.e., the ratio of magnetic to pair enthalpy densities). Wefind that the post-reconnection energy is shared roughly equally betweenmagnetic fields, pairs, and protons for $\sigma_{e,h}\gtrsim 3$. We empiricallyfind that the mean lepton Lorentz factor in the post-reconnection regiondepends on $\sigma, \Theta_e$, and $\sigma_{e,h}$ as $\langle \gamma_e-1\rangle\approx \sqrt{\sigma}(1+4\Theta_e)\left(1+\sigma_{e,h}/30\right)$, for$\sigma\ge1$. The high-energy part of the post-reconnection lepton energydistributions can be described by a power law, whose slope is mainly controlledby $\sigma_{e,h}$ for $\kappa \gtrsim 3-6$, with harder power laws obtained forhigher magnetizations. We finally show that reconnection in pair-proton plasmaswith multiplicities $\kappa \sim 1-20$, magnetizations $\sigma \sim 1-10$, andtemperatures $\Theta_e \sim 1-10$ results in particle power law slopes andaverage electron Lorentz factors that are consistent with those inferred inleptonic models of AGN jet emission.

Relativistic Magnetic Reconnection in Electron-Positron-Proton Plasmas: Implications for Jets of Active Galactic Nuclei