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Black widows (BWs) are millisecond pulsars ablating their companion stars.The out-flowing material from the companion can block the radio emission of thepulsar, resulting in eclipses. In this paper, we construct a model for theradio eclipse by calculating the geometry of the bow shock between the winds ofthe pulsar and companion, where the shock shapes the eclipsing medium but hadnot been described in detail in previous works. The model is further used toexplain the variations of the flux density and dispersion measure (DM) of threeBW pulsars (i.e., PSR B1957$+$20, J2055$+$3829, and J2051$-$0827) detected bythe Five-hundred-meter Aperture Spherical radio Telescope (FAST). Consequently,we constrained the parameters of the three BW systems such as the inclinationangles and true anomalies of the observer as well as the mass-loss rates andwind velocity of the companion stars. With the help of these constraints, it isexpected that magnetic fields of companion stars and even masses of pulsarscould further be determined as some extra observation can be achieved in thefuture.

Constraining the orbital inclination and companion properties of three black widow pulsars detected by FAST