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Dark matter in the form of compact objects with mass $M_{\rm co} \gtrsim 10M_{\odot}$ can be constrained by its dynamical effects on wide binary stars.Motivated by the recent interest in Primordial Black Hole dark matter, werevisit the theoretical modelling involved in these constraints. We improve onprevious studies in several ways. Specifically, we i) implement a physicallymotivated model for the initial wide-binary semi-major axis distribution, ii)include unbound binaries, and iii) take into account the uncertainty in therelationship between semi-major axis and observed angular separation. Theseeffects all tend to increase the predicted number of wide binaries (for a givencompact object population). Therefore the constraints on the halo fraction incompact objects, $f_{\rm co}$, are significantly weakened. For the wide binarysample used in the most recent calculation of the constraints, we find thefraction of halo dark matter in compact objects is $f_{\rm co} < 1$ for $M_{\rmco} \approx 300 \, M_{\odot}$, tightening with increasing $M_{\rm co}$ to$f_{\rm co} < 0.26$ for $M_{\rm co} \gtrsim 1000 \, M_{\odot}$.

Modelling uncertainties in wide binary constraints on primordial black holes