Coronal heating is clearly related to the coronal magnetic field. This may
be due to a passive role of the magnetic held in modifying wave propagation
and dissipation or to an active role resulting from the liberation of magn
etic energy by reconnection or in some other way. The purpose of this artic
le is to examine the consequences of reconnection at the chromospheric leve
l rather than in the corona. We note that the chromosphere is indeed a favo
rable site for reconnection to occur, since the resistivity is greatest in
that region-specifically at the temperature-minimum location. Chromospheric
reconnection can lead to coronal heating by Joule heating, by the generati
on and subsequent dissipation of high-frequency Alfven and magnetacoustic w
aves, or by the response of the coronal magnetic field to a sudden change i
n connectivity. The second process could also contribute to heating of the
solar wind, since high-frequency Alfven waves can be absorbed by cyclotron
damping. We note also that chromospheric reconnection could inject sufficie
nt chromospheric gas into the corona to balance the known steady downflow o
f coronal gas through the transition region. It is also possible that chrom
ospheric reconnection plays a role in the first ionization potential effect
.