  Empirical birthrate estimates for pulsar binaries depend on the fraction of
sky subtended by the pulsar beam: the pulsar beaming fraction. This fraction
depends on both the pulsar's opening angle and the misalignment angle between
its spin and magnetic axes. Previous estimates use the average value for only
two pulsars, i.e. PSRs B1913+16 and B1534+12. We explore how birthrate
predictions depend on assumptions about opening angle and alignment, using
empirically-motivated distributions to define an effective beaming correction
factor, f_{b,eff}. For most known pulsars, we expect f_{b,eff} to be less than
6. We also calculate f_{b,eff} for PSRs J0737-3039A and J1141-6545, applying
the currently available constraints for their beam geometry. Our median
posterior birthrate predictions for tight PSR-NS binaries, wide PSR-NS
binaries, and tight PSR-WD binaries are 89/Myr, 0.84/Myr, and 34/Myr,
respectively. For pulsars with spin period between 10 ms and 100 ms, we
marginalized our posterior birthrate distribution P(R) over a range of
plausible beaming correction factors. Our predictions are robust, changing
little between several alternative misalignment angle distribution models.
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