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Helium white dwarfs (HeWDs) are thought to form from low-mass red giant starsexperiencing binary interaction. Because the helium core mass of a red giantstar is closely related to the stellar radius, there exists well-known relationbetween the orbital period ($P_{\rm orb}$) and the mass ($M_{\rm WD}$) of theHeWDs, which is almost independent of the type of the companion star.Traditional derivation of the $M_{\rm WD}$-$P_{\rm orb}$ relation generallyneglected the effect of wind mass loss from the red giants, while observationsshow that wind mass loss from red giants in binary systems is systematicallyhigher than that from isolated stars. In this work, we calculate binaryevolution with tidally enhanced stellar wind (TEW) and find that it causessignificantly scatter of the traditional $M_{\rm WD}$-$P_{\rm orb}$ relation.The TEW can prevent the red giants from overflowing their Roche lobes and slowdown the growth of the helium core, leaving a lower-mass HeWD for given orbitalperiod. This scenario may account for some of the HeWD binaries that deviatefrom the traditional $M_{\rm WD}$-$P_{\rm orb}$ relation. However, we point outthat observations of more HeWD binaries in wide orbits are needed to test theTEW model and to constrain the enhanced wind factor.

The White Dwarf Mass-Orbital Period Relation Under Wind Mass Loss