We propose that the supersoft x‐ray spectra observed in CAL 83, CAL 87, and RX J0527.8‐6954 can be explained as a result of near‐Eddington accretion onto neutron stars. Our model is consistent with a recently proposed unified model for the low‐mass x‐ray binaries (LMXRB). If the luminosity of the source is within 10% of the Eddington value, what determines whether the source appears as a supersoft x‐ray source or as a ‘‘canonical’’ LMXRB is the nature of the accretion flow and its extend. If the radial flow is subsonic and extends toatleasta few thousand neutron star radii the source behaves like a supersoft one. If on the other hand the flow is supersonic and extends toatmosta few hundred neutron star radii, the source exhibits the characteristics of a ‘‘canonical’’ LMXRB. ©1994 American Institute of Physics.