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Accretion disks formed in binary neutron star mergers play a central role inmany astrophysical processes of interest, including the launching ofrelativistic jets or the ejection of neutron-rich matter hosting heavy elementnucleosynthesis. In this work we analyze in detail the properties of accretiondisks from 44 ab initio binary neutron star merger simulations for a large setof nuclear equations of state, binary mass ratios and remnant fates, with theaim of furnishing reliable initial conditions for disk simulations and acomprehensive characterization of their properties. We find that the disks havea significant thermal support, with an aspect ratio decreasing with the massratio of the binary from $\sim 0.7$ to 0.3. Even if the disk sample spans abroad range in mass and angular momentum, their ratio is independent from theequation of state and from the mass ratio. This can be traced back to therotational profile of the disc, characterized by a constant specific angularmomentum (as opposed to a Keplerian one) of $3-5 \times 10^{16} \rm ~cm^2~s^{-1}$. The profiles of the entropy per baryon and of the electronfraction depend on the mass ratio of the binary. For more symmetric binaries,they follow a sigmoidal distribution as a function of the rest mass density,for which we provide a detailed description and a fit. The disk propertiesdiscussed in this work can be used as a robust set of initial conditions forfuture long-term simulations of accretion disks from binary neutron starmergers, posing the basis for a progress in the quantitative study of theoutflow properties.

Geometric and thermodynamic characterization of binary neutron star accretion discs