**A summary of WIND magnetic clouds for years 1995-2003: model-fitted
parameters, associated errors and classifications **

*R.P. Lepping, D.B. Berdichevsky, C.-C. Wu, A. Szabo, T. Narock, F. Mariani,
A. J. Lasarus, and A.J. Quivers *

**Abstract:**

Interplanetary magnetic clouds (MCs) have been identified for the first 8.6
years of the WIND mission, and their magnetic field structures have been parameter-fitted
by a static, force free, cylindrically-symmetric model (Lepping et al., 1990)
with various levels of success. This paper summarizes various aspects of the
results of the model fitting by providing: seven estimated model fit-parameter
values for each of the 82 MCs found, their objectively determined quality estimates,
closest approach vectors (in two coordinate frames), fit-parameter *errors*
for the cases of acceptable quality (50 cases, or 61%), axial magnetic fluxes,
axial current densities, and total axial current - as well as some examples
of MC profiles for various conditions and "categories" for each case
(e.g. B_{z}: N→S or S→N, etc.). MC quality is estimated
from a quantitive consideration of a large set of parameters, such as the chi-squared
of the model fit, degree of asymmetry of the B profile, and a comparison of
two means of estimating radius. This set of MCs was initially identified by
visual inspection of relevant field and plasma data. Each resulting MC candidate
is then tested through the use of the MC parameter model, for various adjusted
durations to determine the best fit, which helps to refine the boundary-times.
The resulting MC set is called Set 1. Another, larger, set (Set 2) of MCs is
identified through an automated program whose criteria are based on general
MC plasma and field characteristics at 1 AU determined through past experience.
Set 1 is almost fully contained within Set 2, whose frequency of occurrence
better matches that of the sunspot cycle than Set 1. The difference-set (Set
2-Set 1) is referred to as the magnetic cloud-like (MCL) set, whose members
do not very well represent good flux ropes through modeling. We present a discussion
of how a MC's front boundary is specifically identified in terms of multi-parameter
considerations (i.e. any one or more of: increase in B, directional discontinuity,
magnetic hole in B, drop in proton plasma beta, B-fluctuation level change,
proton temperature drop, etc.) as well as through the application of the flux
rope model. Also presented are examples of unusual MCs, as well as some commonly
occurring relationships, such as the existence and frequency (approx. 1/2 the
time) of upstream interplanetary shocks, and less frequent internal shocks.

Annales Geophysicae, 24, 1-31, 2006, SRef-ID: 1432-0576/ag/2006-24-1, European Geosciences Union 2006, submitted, 2006