WY Cancri is a short-period ( P =0.829 d ) eclipsing RS Canum Venaticorum stars , and both components are late-type stars .
Recently , observations provided by photometric observations and light time minima show that the orbital period of WY Cancri is experiencing a secular decrease at a rate of { d } P / { d } t = -1.2 \times 10 ^ { -7 } d~ { } yr ^ { -1 } .
In this Letter , we attempt to investigate if the period change of WY Cancri can originate from the angular momentum loss .
In calculation , we assume that this source has a high wind loss rate of \sim 10 ^ { -10 } ~ { } M _ { \odot } ~ { } yr ^ { -1 } .
To account for the observation , magnetic braking demands a strong surface magnetic field of \gtrsim 10000 G like Ap/Bp stars .
Furthermore , if this source may be surrounded by a circumbinary disk , and 6 % of the wind loss feeds the disk , tidal torque between the disk and the binary can offer the observed angular momentum loss rate .
Such a strong magnetic field or an extremely high wind input fraction seem to be highly unlikely .