  A Chandra spectrum of the moderately active nearby F6 V star Pi3 Ori is used
to study the coronal properties of mid-F dwarfs. We find that Pi3 Ori's coronal
emission measure distribution is very similar to those of moderately active G
and K dwarfs, with an emission measure peak near $\log T=6.6$ seeming to be
ubiquitous for such stars. In contrast to coronal temperature, coronal
abundances are known to depend on spectral type for main sequence stars. Based
on this previously known relation, we expected Pi3 Ori's corona to exhibit an
extremely strong "FIP effect," a phenomenon first identified on the Sun where
elements with low "First Ionization Potential" (FIP) are enhanced in the
corona. We instead find that Pi3 Ori's corona exhibits a FIP effect essentially
identical to that of the Sun and other early G dwarfs, perhaps indicating that
the increase in FIP bias towards earlier spectral types stops or at least slows
for F stars. We find that Pi3 Ori's coronal characteristics are significantly
different from two previously studied mid-F stars, Procyon (F5 IV-V) and Tau
Boo (F7 V). We believe Pi3 Ori is more representative of the coronal
characteristics of mid-F dwarfs, with Procyon being different because of
luminosity class, and Tau Boo being different because of the effects of one of
two close companions, one stellar (Tau Boo B: M2 V) and one planetary.
