  Recent reanalyses of HIPPARCOS parallax data confirm a previously noted
discrepancy with the Pleiades distance modulus estimated from main-sequence
fitting in the color-magnitude diagram. One proposed explanation of this
distance modulus discrepancy is a Pleiades He abundance that is significantly
larger than the Hyades value. We suggest that, based on our theoretical and
observational understanding of Galactic chemical evolution, nitrogen abundances
may serve as a proxy for helium abundances of disk stars. Utilizing
high-resolution near-UV Keck/HIRES spectroscopy, we determine N abundances in
the Pleiades and Hyades dwarfs from NH features in the 3330 Ang region. While
our Hyades N abundances show a modest 0.2 dex trend over a 800 K Teff range, we
find the Pleiades N abundance (by number) is 0.13+/-0.05 dex lower than in the
Hyades for stars in a smaller overlapping Teff range around 6000 K; possible
systematic errors in the lower Pleiades N abundance result are estimated to be
at the <0.10 dex level. Our results indicate [N/Fe]=0 for both the Pleiades and
Hyades, consistent with the ratios exhibited by local Galactic disk field stars
in other studies. If N production is a reliable tracer of He production in the
disk, then our results suggest the Pleiades He abundance is no larger than that
in the Hyades. This finding is supported by the relative Pleiades-Hyades C, O,
and Fe abundances interpreted in the current context of Galactic chemical
evolution, and is resistant to the effects on our derived N abundances of a He
abundance difference like that needed to explain the Pleiades distance modulus
discrepancy. A physical explanation of the Pleiades distance modulus
discrepancy does not appear to be related to He abundance.
