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We investigate the impact of a mean field model for the $\alpha\Omega$-dynamopotentially active in the post-merger phase of a binary neutron starcoalescence. We do so by deriving equations for ideal general relativisticmagnetohydrodynamics (GRMHD) with an additional $\alpha-$term, which closelyresemble their Newtonian counterpart, but remain compatible with standardnumerical relativity simulations. We propose a heuristic dynamo closurerelation for the magnetorotational instability-driven turbulent dynamo in theouter layers of a differentially rotating magnetar remnant and its accretiondisk. As a first demonstration, we apply this framework to the early stages ofpost-merger evolution ($\lesssim 50\, \rm ms$). We demonstrate that dependingon the efficacy of the dynamo action, magnetically driven outflows can bepresent with their amount of baryon loading correlating with the magnetic fieldamplification. These outflows can also contain precursor flaring episodesbefore settling into a quasi-steady state. For the dynamo parameters exploredin this work, we observe electromagnetic energy fluxes of up to $10^{50}\, \rmerg/s$, although larger amplification parameters will likely lead to strongerfluxes. Our results are consistent with the expectation that substantial dynamoamplification (either during or after the merger) may be necessary forneutron-star remnants to power short gamma-ray bursts or precursors thereof.

Impact of a mean field dynamo on neutron star mergers leading to magnetar remnants