Solar wind observations show that suprathermal electrons (70 eV $lesssim$ Energy $lesssim$ 1 keV) of the magnetic-field-aligned "strahl" component have broader pitch-angle distributions than are predicted by adiabatic theories of solar wind expansion. Magnetosonic-whistler fluctuations propagating toward the Sun at k ¿ B o = 0 (where B o is the background magnetic field) have a strong cyclotron resonance with suprathermal electrons propagating in the anti-Solar direction along B o . This resonance enables strong pitch-angle scattering; thus whistlers are a likely source of the observed strahl broadening. Particle-in-cell simulations in a magnetized, homogeneous, collisionless plasma of electrons and protons are used to study the response of a strahl-like electron component to whistler fluctuation spectra. If the whistler anisotropy instability is excited via the initial application of T $perp$ /T $parallel$ > 1 to the electron core component, the resulting electron scattering leads to strahl pitch-angle distributions which decrease in width as electron energy increases. In contrast, if a power spectrum of whistler fluctuations proportional to k -3 is initially applied to the simulations, the resulting electron scattering leads to strahl pitch-angle distributions which increase in width as electron energy increases.