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The evolution of the electron heat flux in the solar wind is regulated by theinterplay between several effects: solar wind expansion, that can potentiallydrive velocity-space instabilties, turbulence and wave-particle interactions,and, possibly, collisions. Here we address the respective role played by thesolar wind expansion and the electron firehose instability, developing in thepresence of multiple electron populations, in regulating the heat flux. Wecarry out fully kinetic, Expanding Box Model simulations and separately analyzethe enthalpy, bulk and velocity distribution function skewness contributionsfor each of the electron species. We observe that the key factor determiningelectron energy flux evolution is the reduction of the drift velocity of theelectron populations in the rest frame of the solar wind. In our simulations,redistribution of the electron thermal energy from the parallel to theperpendicular direction after the onset of the electron firehose instability isobserved. However, this process seems to impact energy flux evolution onlyminimally. Hence, reduction of the electron species drift velocity in the solarwind frame appears to directly correlate with efficiency for heat fluxinstabilities

Collisionless heat flux regulation via electron firehose instability in presence of a core and suprathermal population in the expanding solar wind