Observations of energetic (1.5 - 300 keV/e) medium-to-high charge stat
e (+3 less-than-or-equal-to Q less-than-or-equal-to +7) solar wind ori
gin C and O ions made in the quasi-trapping region (QTR) of Earth's ma
gnetosphere are compared to ion trajectories calculated in model equat
orial mapetospheric magnetic and electric fields.. These comparisons i
ndicate that solar wind ions entering the QTR on the nightside as an e
nergetic component of the plasma sheet exit the region on the dayside,
experiencing little or no charge exchange on the way. Measurements ma
de by the CHarge Energy Mass (CHEM) ion spectrometer on board the AMPT
E/CCE spacecraft at 7 < L < 9 from September 1984 to January 1989 are
the source of the new results contained herein: quantitative long-term
determination of number densities, average energies, energy spectra,
local time distributions, and their variation with geomagnetic disturb
ance level as indexed by Kp. Solar wind primaries (ions with charge st
ates unchanged) and their secondaries (ions with generally lower charg
e states produced from primaries in the magnetosphere via charge excha
nge) are observed throughout the QTR and have distinctly different loc
al time variations that persist over the entire 4-year analysis interv
al. During Kp greater-than-or-equal-to 3(o) intervals, primary ion (e.
g., O+6) densities exhibit a pronounced predawn maximum with average e
nergy minimum and a broad near-local-noon density minimum with average
energy maximum. Secondary ion (e.g., O+5) densities do not have an id
entifiable predawn peak, rather they have a broad dayside maximum peak
ed in local morning and a nightside minimum. During Kp less-than-or-eq
ual-to 2- intervals, primary ion density peaks are less intense, broad
er in local time extent, and centered neu midnight, while secondary io
n density local time variations diminish. The long-time-interval basel
ine helps to refine and extend previous observations; for example, we
show that ionospheric contribution to O+3 is negligible. Through compa
rison with model ion trajectories, we interpret the lack of pronounced
secondary ion density peaks colocated with the primary density peaks
to indicate that: (1) negligible charge exchange occurs at L > 7, that
is, solar wind secondaries are produced at L < 7, and (2) solar wind
secondaries do not form a significant portion of the plasma sheet popu
lation injected into the QTR. We conclude that little of the energetic
solar wind secondary ion population is recirculated through the magne
tosphere.