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Spacecraft observations showed that electron heat conduction in the solarwind is probably regulated by whistler waves, whose origin and efficiency inelectron heat flux suppression is actively investigated. In this paper, wepresent Particle-In-Cell simulations of a combined whistler heat flux andtemperature anisotropy instability that can operate in the solar wind. Thesimulations are performed in a uniform plasma and initialized with core andhalo electron populations typical of the solar wind. We demonstrate that theinstability produces whistler waves propagating both along (anti-sunward) andopposite (sunward) to the electron heat flux. The saturated amplitudes of bothsunward and anti-sunward whistler waves are strongly correlated with their {\itinitial} linear growth rates, $B_{w}/B_0\sim (\gamma/\omega_{ce})^{\nu}$, wherefor typical electron betas we have $0.6\lesssim \nu\lesssim 0.9$. Thecorrelations of whistler wave amplitudes and spectral widths with plasmaparameters (electron beta and temperature anisotropy) revealed in thesimulations are consistent with those observed in the solar wind. Theefficiency of electron heat flux suppression is positively correlated with thesaturated amplitude of sunward whistler waves. The electron heat flux can besuppressed by 10--60% provided that the saturated amplitude of sunward whistlerwaves exceeds about 1% of background magnetic field. Other experimentalapplications of the presented results are discussed.

Particle-In-Cell Simulations of Sunward and Anti-sunward Whistler Waves in the Solar Wind