  We model the observed charge states of the elements C, O, Mg, Si, and Fe in
the coronal mass ejections (CMEs) ejecta. We concentrate on "halo" CMEs
observed in situ by ACE/SWICS to measure ion charge states, and also remotely
by STEREO when in near quadrature with Earth, so that the CME expansion can be
accurately specified. Within this observed expansion, we integrate equations
for the CME ejecta ionization balance, including electron heating parameterized
as a fraction of the kinetic and gravitational energy gain of the CME. We also
include the effects of non-Maxwellian electron distributions, characterized as
a kappa function. Focusing first on the 2010 April 3 CME, we find a somewhat
better match to observed charge states with kappa in the range 2-4, close to
the theoretical minimum value of kappa = 3/2, implying a hard spectrum of
non-thermal electrons. Similar, but more significant results come from the 2011
February 15 event, although it is quite different in terms of its evolution. We
discuss the implications of these values, and of the heating required, in terms
of the magnetic reconnection Lundquist number and anomalous resistivity
associated with CME evolution close to the Sun.
