  Halo initial mass functions (IMFs), heavily-biased toward white dwarf (WD)
precursors (i.e. 1->8 M_sun), have been suggested as a suitable mechanism for
explaining microlensing statistics along the line of sight to the LMC. Such
IMFs can apparently be invoked without violating the observed present-day WD
luminosity function. By employing a simple chemical evolution argument, we
demonstrate that reconciling the observed halo Population II dwarf abundances
(i.e. [C,N/O]=-0.5), with that expected from the postulated ``WD-heavy'' IMF
(i.e. [C,N/O]=+0.5), is difficult.

Astrophysics