The observed paucity of halo blue stars in comparison with the predictions of the Bahcall-Soneira (B&S) model of the Galaxy is referred to here at the "halo blue-star mystery". We reexamine the basic assumptions of the model, especially the luminosity function adopted by B&S for evolved halo stars. We suggest that the halo blue-star mystery can be resolved by adopting a steeper luminosity function than the one adopted by B&S, viz., one nearer to those observed in M 92, M 13, and the Hartwick field function. With this modification we show that good agreement can be obtained between predicted and observed counts for halo field giants, blue horizontal-branch stars, and RR Lyraes in the south galactic pole, provided a Hess diagram similar to that of M 3 or M 5 is adopted for stars with MV <∼+1.5. There is thus little evidence that the galactic halo field in the range Z ∼ 5 to 20 kpc suffers an extreme second parameter effect, i.e., has a Hess diagram corresponding to such clusters as NGC 7006, Pal 13, or Pal 4 as had been proposed earlier (Kraft 1984).