# Summary

**Title**: Impact of the Extended Ionosphere

**Full Title**: Impact of the Extended Ionosphere on the Present and
Future Magnetosphere

**Summary**:

We propose to use existing published data sets, single particle
trajectory tracing, bounce-averaged kinetic theory, and multifluid
magnetodynamic simulations to incorporate a realistic description of the
extended ionosphere within a multifluid magnetospheric global
circulation model. We will include separately the *photothermal*
ionospheric light ion outflow at all latitudes (including within the
plasmasphere), and the *induced* ionospheric heavy ion plasma outflow
from regions energized by the solar wind interaction. The latter
outflows will respond to energy inputs from the solar wind via the
global simulation inner boundary.

The resultant global simulation will allow us to evaluate the impact of
the extended ionosphere on magnetospheric processes and dynamics in
response to solar wind variations, under current conditions, where
ionospheric impact may be highly dependent on the form and degree of
solar wind excitation of the magnetosphere-ionosphere system. We will
also simulate and predict the behavior of the terrestrial magnetosphere
through the upcoming geomagnetic field reversal, when the importance of
ionospheric plasma is expected to increase substantially as the main
field dipole moment weakens and rotates and the magnetopause standoff
distance shrinks.

Given the tools, we believe it is incumbent upon us to predict and
anticipate the expected changes in space weather on longer space climate
time scales. The need for this was highlighted by the 2003 Hollywood
movie, "Core", which took many liberties with the facts, exploited
public gullibility concerning the Sun-Earth connection, and spread
numerous falsehoods. We believe it is imperative to correct this
situation through a research study of the actual expectations for a
field reversal, followed by education and public outreach efforts to
enhance public awareness of the scientific realities.

Our studies of future magnetospheric behavior will be validated through
comparisons of relevant reversal states with existing observations and
models of terrestrial planet magnetospheres, including Mercury (reduced
dipole moment), Mars (irregular field), and Venus (negligible dipole
moment). They will also be relevant to planning for future visits, for
example Discovery Missions, to these and other planets, as called for by
the Sun Earth Connections Roadmap and the National Academy of Sciences
Decadal Strategy Study. On a somewhat longer time scale of a few hundred
years, they will become critically relevant to the Earth of the future,
as the current dipole reduction unfolds into a reversal.

#  

Summary [i](#summary)

SCIENTIFIC, TECHNICAL, AND MANAGEMENT SECTION
[1](#scientific-technical-and-management-section)

Background [1](#background)

Extended Ionosphere [1](#extended-ionosphere)

Geodynamo [3](#geodynamo)

Recent Progress [3](#recent-progress)

Mercury Ion Dynamics [3](#mercury-ion-dynamics)

Venus/Mars Solar Wind Interaction [5](#venusmars-solar-wind-interaction)

Dayside Reconnection [6](#dayside-reconnection)

MFMD Simulation of a 90˚ Tilt Magnetosphere
[7](#mfmd-simulation-of-a-90-tilt-magnetosphere)

Science Objectives [8](#science-objectives)

The Extended Ionosphere [8](#the-extended-ionosphere)

Magnetospheric Impact [9](#magnetospheric-impact)

Reconnection Impact [10](#reconnection-impact)

Plasma Sheet and Energetic Particles
[11](#plasma-sheet-and-energetic-particles)

Proposed Approach [12](#proposed-approach)

Multi-fluid MagnetoDynamic and MHD Models
[12](#multi-fluid-magnetodynamic-and-mhd-models)

Outer Magnetosphere Full Particle Model
[12](#outer-magnetosphere-full-particle-model)

Inner Magnetosphere Kinetic Particle Model
[13](#inner-magnetosphere-kinetic-particle-model)

Work Plan [13](#work-plan)

Closure and Relevance [14](#closure-and-relevance)

Management and Cost [15](#management-and-cost)

Responsibilities of Key Personnel
[15](#responsibilities-of-key-personnel)

Appendix 1. REFERENCES [16](#appendix-1.-references)

Appendix 2: CURRICULUM VITAE [18](#appendix-2-curriculum-vitae)

Dominique C. Delcourt, Research Scientist
[18](#dominique-c.-delcourt-research-scientist)

Selected Publications [18](#selected-publications)

Mei-Ching Fok, Astrophysicist [19](#mei-ching-fok-astrophysicist)

Gary A Glatzmaier, Professor of Earth Sciences
[20](#gary-a-glatzmaier-professor-of-earth-sciences)

Thomas E. Moore, Branch Head [21](#thomas-e.-moore-branch-head)

Nikolai Tsyganenko, Senior Research Scientist
[22](#nikolai-tsyganenko-senior-research-scientist)

Appendix 3: CURRENT AND PENDING SUPPORT
[23](#appendix-3-current-and-pending-support)

Mei-Ching Fok [23](#mei-ching-fok)

Thomas E. Moore [23](#thomas-e.-moore)

Nikolai Tsyganenko [23](#nikolai-tsyganenko)

Appendix 4: BUDGET SUMMARY for RESEARCH PROPOSAL
[24](#appendix-4-budget-summary-for-research-proposal)

Budget Details and Notes [24](#budget-details-and-notes)

Appendix 5: FINAL PROGRESS REPORT
[25](#appendix-5-final-progress-report)

Appendix 6: STATEMENTS OF COMMITMENT
[26](#appendix-6-statements-of-commitment)

# 

# SCIENTIFIC, TECHNICAL, AND MANAGEMENT SECTION

## Background

### Extended Ionosphere

30 years of theory, beginning with Banks and Holzer \[1968\]; and
observations, beginning with Shelley et al. \[1972\], have led to the
recognition that the ionosphere is an extended plasma region that
dominates not only the plasmasphere, but also the hot near-Earth plasma
sheet and ring current regions, especially during times of geomagnetic
disturbances \[Moore and Delcourt, 1995 and references therein\].
Traditionally, magnetosphere-ionosphere coupling has been modeled by
taking the entire ionosphere as a thin layer described by its
height-integrated characteristics. However, more recently \[e.g.
Winglee, 1998\], it has become clear that the presence of the ionosphere
throughout much of the magnetosphere mass loads the system and may
actually enable the creation of the ring current, the principal
manifestation of geomagnetic storms \[Moore et al., 2001\].

Current global simulations that describe the ionosphere as an extended
region within the magnetosphere impose boundary plasma densities rather
than fluxes \[e.g. Winglee 1998\]. Then all ionospheric outflows are
driven by pressure distributions inside the simulation space rather than
by ionospheric processes. Such models do a good job on the polar wind
light ion outflows but do not yet realistically incorporate the low
latitude *photothermal* plasmasphere, or the *induced* heavy ion
outflows driven by structured sources of energy in the auroral zone. Low
latitude outflows that fill the plasmasphere are eventually freed up to
circulate through the entire magnetosphere during geomagnetically active
periods as drainage plumes, as has been amply demonstrated in recent
studies \[Goldstein et al., 2003; Su et al., 2001; Foster et al., 2002;
Chandler et al., 2003\]. The auroral induced sources are strongly
influenced by both electromagnetic (Poynting) and kinetic energy fluxes
\[Strangeway et al., 2000; Strangeway et al,. 2002\] imposed by
structured magnetospheric convection and precipitation.

![](media/image1.png){width="3.4756944444444446in"
height="3.9604166666666667in"}**Figure 1**. We are now in a position to
include both photothermal and induced outflows in global simulation
models, and need only translate empirical relationships into suitable
code modules for their implementation within a suitable (multifluid)
simulation code.

While the ionosphere is known to be important in the dynamics of our
current magnetosphere, especially during active times, it will become
much more important \[Vasyliunas, 2003 during periods of reduced dipole
moment such as that which will prevail during the geomagnetic reversal
that we have for some centuries been entering \[Cox, 1969\]. Since
biblical times, the dipole moment is has halved, and the rate of change
is accelerating in recent decades \[Merrill, 1999\], such that
extrapolation suggests a reversal minimum in a few 100 years. With the
proposed attention to realistic modeling of the extended ionosphere, our
tools will have reached a state of readiness to be tested on a wider
range of parameters with greater ionospheric importance and impact. We
propose here to investigate the behavior of the geomagnetosphere during
a magnetic field reversal, for which this capability will be enabling.

Siscoe et al. \[1976\] conjectured that only the dipole moment is
reduced during a reversal, concluding that the higher multipoles would
be sufficient to prevent the Earth from reaching a Venus like state with
direct interaction of the solar wind and ionosphere. Siscoe and
coworkers \[1976; 1979, 1980\] also considered the auroral zone shapes
that would result. Neverthless, it is clear that the magnetosphere will
go through stages in which it becomes more similar to the magnetospheres
of other terrestrial planets, which in general have smaller dipole
moments than that of the Earth, in absolute or relative terms. If the
dipole moment drops sufficiently below its present value, the
magnetosphere will more closely resemble that of Mercury, where the
upstream standoff distance is \< 1.5 planetary radii. If it drops even
lower than that, it will more closely resemble the Martian interaction
with the solar wind, with higher multipole moments imparting a local
structure not unlike the local crustal magnetization features of Mars
\[Curtis and Ness, 1988; Acuna et al., 2001\]. If the higher multipole
moments drop as well, Earth will resemble Venus' solar wind interaction.
Thus, a consideration of space climate during a geomagnetic reversal
should encapsulate the entire study of comparative magnetospheres for
the terrestrial planets. Moreover, during a reversal period with
appreciable remanent dipole moment, as the orientation rotates through
90˚ relative to the spin axis, a magnetosphere similar to that once
expected for Uranus (before the Voyager encounter) \[Selesnick and
Richardson, 1986, Selesnick, 1988\] will briefly exist.

![](media/image2.pct){width="5.933333333333334in" height="3.78125in"}

Figure 2. Dynamo simulations, after Glatzmaier et al. \[1999\]. Cases
correspond to varying imposed patterns of radial heat flux at the
core-mantle boundary. Top row: the pattern of heat flux in projection
over the boundary with geographic north at the top-center and south pole
at bottom-center. Solid contours represent heat flux enhancements while
broken contours represent heat flux depressions relative to mean. Case e
has bands of enhancement with a polar peak, while case f is the inverse.
Case g is the isotropic case, while case h represents a more realistic
case. Second row: trajectory of the south pole of the dipole moment
spanning the times indicated in the plots below. Third row: plots of the
polar latitude of the dipole moment versus time. Fourth row: plots of
the magnitude of the dipole moment versus time. All simulations began
long before the zero times plotted.

![](media/image3.pct){width="1.5in" height="9.5in"}

### Geodynamo 

The geomagnetic field is known to exhibit quasiperiodic reversals on a
time scale of a few hundred thousand years, involving distinct flips of
polarity that occur at average frequency of about 5 per My, with longer
term modulations of frequency, as shown in the sidebar chart \[S Earle,
<http://www.mala.bc.ca/~earles/reversals.htm>\]. Extrapolation of the
current dipole evolution may not be accurate, but the geologic record
shows that future reversals are a certainty.

But do we know the character of reversal fields well enough to model the
solar wind interaction throughout the process? The answer is an
unqualified "yes". During the past decade, the theory of the geodynamo
has been substantially developed through 3D simulations that run for a
few 100 kyrs, with a resolution of \~15 days \[Glatzmaier and Roberts,
1995\]. These simulations exhibit realistic polarity reversals within
(barely) practical run times. The modeled dynamo is thermally driven,
and responds dramatically to varying assumptions concerning the
distribution of heat flow from the Earth's core to space \[Glatzmaier et
al., 1999; Roberts and Glatzmaier, 2000\]. In the realistic cases, a
reversal involves a reduction of the dipole moment of the Earth, and to
a varying degree, a turning of the residual dipole moment from one spin
pole to the other, followed by a restoration of the original dipole
moment in the opposite direction. The minimum dipole moment during a
reversal is typically \<10% of the quiescent dipole moment, but it can
be larger or smaller depending on a number of factors. **Figure 2**
illustrates a range of possibilities. Most cases exhibit behaviors that
can be described as impulsive polarity flips of the geomagnetic field.
In many cases the dipole moment dips substantially during the rotation
of the dipole orientation; in other cases it does not dip as much.

Recent simulation work has thus created a quantitative basis for
investigating the solar wind interaction during a geomagnetic reversal.
Simulation results can be used as a determination of the likely internal
field of the Earth at any stage of the reversal process. The full
coefficients for these internal fields are available on a 15 day
resolution basis for any of the events shown in Figure 2, and for many
other cases as well. G Glatzmaier will collaborate with us in this
study, supporting us with a supply of geomagnetic field descriptions
from his simulation work, exemplary of the generic states attained by
the field during the process of reversals.

It is relatively straightforward to insert an arbitrary internal field
into a magnetospheric field model or a global simulation of the solar
wind interaction. Doing so may drastically alter many of the conditions
being modeled and may require adjustments in the modeling framework.
Nevertheless, it should be clear from the discussion above that the
tools exist with which to begin the task of predicting the kinds of
magnetospheres we will have during the process of a geomagnetic
reversal, which may be underway at the present time. This is a proposal
to do just that, to first establish a realistic extended ionosphere
within a simulation of the current magnetosphere; then to simulate the
future magnetosphere at representative stages of a field reversal; then
to validate our results by comparison with observations of the
magnetospheres of the terrestrial planets Mercury, Mars, and Venus.

In the following sections of this proposal, we summarize recent progress
made under our prior support, forumulate a specific set of science
objectives for the present proposal, summarize our approach and the
specific studies we are planning. Finally, we summarize and point out
the relevance of our proposed work to the Sun-Earth Connection Geospace
Sciences program.

## Recent Progress

### Mercury Ion Dynamics

In recognition of Messenger, a NASA Discovery mission being developed
for exploration of Mercury, and Bepi Colombo, a Mercury mission being
planned by ESA, we have begun to study the character of the Hermean
magnetosphere and hermeosphere. The latter is a region dominated by
Mercury's exosphere, containing exotic materials such as sodium,
sputtered from the planetary surface.

One study \[Delcourt et al., 2002\] considered ion dynamics in the
Hermean magnetosphere, and evaluated the effects of smaller radius field
curvatures associated with the smaller overall size of this
magnetosphere. The simulations demonstrate that centrifugal effects play
a substantially more prominent role in the net particle acceleration
than in the terrestrial magnetosphere. It is found that, at Mercury, the
acceleration due to ExB drift path curvature may greatly exceed that due
to magnetic field line curvature even for moderate convection rates, a
situation which contrasts with that prevailing at Earth. At Mercury, ExB
related centrifugal effects can yield heavy ion energization of hundreds
of eV within minutes, which is at least two orders of magnitude above
that achieved in the Earth's magnetosphere.

In the second study \[Delcourt et al., 2003\], we explored the behavior
of Na^+^ ions of planetary origin at Mercury, which exhibits several
features of interest linked to the small spatial scales of the Hermean
magnetosphere. First, because of the pronounced curvature of the ExB
drift paths, significant centrifugal acceleration occurs during
transport from high to low latitudes so that the magnetospheric lobe
content is found to be significantly more energetic (several hundreds of
eV) at Mercury than at Earth. In the innermost region (typically, within
2 R~M~ radial distance), this non-adiabatic behavior is characterized by
prominent pitch angle scattering ( \~ 1) which hampers stable trapping
at low latitudes. At larger distances, quasi-adiabatic (Speiser-type)
behavior occurs together with several keV ion energization. The net
result of this non-adiabatic circulation is a quite substantial filling
of the inner tail and a thin sheet of energetic Na^+^ ions at larger
distances, as shown in **Figure 3**. Because of a less dense exosphere,
the density from planetary ions is found to be smaller at aphelion.
Also, the non-adiabatic motion of ions in the magnetotail is responsible
for a narrow band of energetic precipitation in each hemisphere at the
planet's surface. These bands, which extend over several degrees in
latitude and a wide range of longitude, should lead to additional
sputtering of planetary material. The poleward boundary of these bands
corresponds to the limit of slow gyromotion in the magnetotail and thus
depends on ion species. This latter gyroradius filter effect forms a
specific feature of the large-scale magnetic mass spectrometer at
Mercury.

![](media/image4.pct){width="2.8743055555555554in"
height="4.3694444444444445in"}![](media/image5.pct){width="2.8541666666666665in"
height="4.368055555555555in"}

*Figure 3. Color-coded curvature radii of ExB drift paths at (left)
Mercury and (right) Earth. Solid lines show representative magnetic
field lines. Dashed lines show representative ExB drift paths. After
Delcourt et al. \[2003\].*

### Venus/Mars Solar Wind Interaction

Recognizing that Venus and Mars are both candidates for further
exploration, we have also begun to study the Venusian solar wind
interaction. In this case, virtually no intrinsic field or extended
magnetosphere exists, so that the solar wind is directly incident upon
the upper atmosphere and ionosphere. Consequently, one expects a
relatively direct aeronomic interaction in which both charge exchange
and scattering collisions will be frequent with substantial emission of
fast neutral atoms and collisional dissipation resulting in sputtering
escape of upper atmospheric gases. We used the multifluid magetodynamic
simulation results of Tanaka and Murawski \[1997\] to provide a
description of the plasma and fields, along with the exospheric model of
Keating et al. \[1985\]. With the goal of estimating neutral atom
emission, we folded together the plasma and gas models to generate line
of sight integral atom fluxes, with results illustrated in **Figure 4.**
The simulations show the following: Neutral atom imaging is a useful
tool for studying the solar wind interaction with the terrestrial
planetary magnetospheres over the range of magnetization from Earth to
Venus. Significant low-energy (0 -- 10 keV) neutral atom emissions are
expected fromVenus. Venus magnetosheath emissions have similar features
and comparable intensity as those from the Earth during extreme solar
wind condition. Low-energy neutral O images from Venus can be used to
probe the location and dynamics of the ionopause.

![](media/image6.pct){width="5.345833333333333in"
height="5.384027777777778in"}

*Figure 4. Simulated Venus H (left) and O (right) ENA images for the
energy range from 2 eV to a few keV. The white circle is the rim of the
planet and the blue circle is the equator. \[Fok et al., 2003\].*

### Dayside Reconnection

Motivated by Polar observations \[Chandler et al., 1999\] we explored
dayside reconnection theoretically, with the goal of examining whether
high and low latitude reconnection might occur simultaneously \[Moore et
al., 2002\]. The result is that we find it quite plausible, and indeed
we find it to be an essential property of the dayside reconnection
X-line for typical interplanetary magnetic field clock angles near 90˚
or more northerly than that. We revisited arguments in the literature
concerning "component" reconnection and "anti-parallel" reconnection,
and developed a method for integrating the shape of the X-line across
the dayside magnetopause, thus unifying both types of reconnection.,
since in general the X line extends well away from its intersection
points with the locus of antiparallel fields.

Opinion has recently favored the limitation of reconnection primarily to
regions where the reconnecting fields are anti-parallel, as shown in
**Figure 5**, left panel. Where the fields are not anti-parallel or
nearly so, only a component of the fields is available for so-called
"component" reconnection, and the remainder of the fields is directed
along the "X-line", in the form of a so-called "guide field". However,
there is a problem with anti-parallel reconnection, in that the
direction of the X-line tends to run perpendicular to the local magnetic
fields whereas the region of anti-parallel fields tends to run parallel
to the local magnetic fields. As a result, there can be at most a very
short X-line within a given region of anti-parallel fields. Multiple
short X-lines could be invoked, but it is difficult to see how the
aggregate of a series of short parallel X-lines lying across an
antiparallel field region could add up to a significant transpolar
potential in the global picture.

As an alternative, we explored the hypothesis that an X-line forms at
the region with the largest reconnecting field components (presumably at
or near a region of antiparallel fields) but then spreads away from that
region along an X-line that is integrated from point to point along the
magnetopause like a vector streamline. The result is shown in **Figure
5**, right panel, where the X-line has been mapped across the
magnetopause for several different clock angles. Boundary layer flows
were calculated according to the procedure of Cowley and Owen \[1989\].

![](media/image7.jpeg){width="2.8520833333333333in"
height="3.89375in"}![](media/image8.jpeg){width="2.75in"
height="3.9305555555555554in"}

Figure 5. Comparison of antiparallel reconnection sites (left) with the
dayside reconnection X-line (right) calculated by integrating the
component reconnection X- line (white curve) away from regions of
maximal reconnecting component, for selected clock angles. Vectors
emanating from the X-line indicate boundary layer flow. \[Moore et al.,
2002\].

### MFMD Simulation of a 90˚ Tilt Magnetosphere

We also initiated a collaboration with R. M. Winglee of U. Washington,
who has developed an innovative multifluid magntodynamic (MFMD) global
simulation code that tracks separately solar wind ions, ionospheric ions
of multiple species, and electrons. We are running this code at GSFC and
have assigned staff to analyze the code and refine it where possible,
with the goal of parallelization for accelerated performance on
massively parallel processor facilities. To gain experience with the
code our initial efforts have focused on preliminaries to the work
proposed here. To simulate a case of interest for geomagnetic reversals,
we reduced the terrestrial dipole moment to one half its current value,
and tilted it so that the north magnetic pole points toward the sun. The
results are illuminating and fascinating. **Figure 6** illustrates some
salient characteristics of the resultant "pole-on" magnetosphere.

With one pole toward the sun, there is only a single cusp, and only a
single magnetotail lobe. Dayside reconnection links interplanetary field
lines into the sunward facing pole, and extends azimuthally about half
way around the sun-Earth line, encircling the dayside cusp and centered
on the azimuth where the IMF is anti-parallel with the local geomagnetic
field. A more or less semi-cylindrical plasma sheet forms, wrapped
around the single tail lobe, and offset toward the sun-Earth line
azimuth that is opposite to that of the peak dayside reconnection. The
single lobe contains outflows of cold ionospheric plasma, while the
plasma sheet contains Earthward flows of hot ionospheric and solar
plasma. The solar hydrogen density minimizes in the plasma sheet, while
the ionospheric hydrogen density maximizes there.

Our initial results compare well with earlier work on high tilt (Uranus)
magnetospheres by Wu, \[1984\], and Walker et al. \[1989\]. Those
earlier efforts had zero IMF magnitude, resulting in near-perfect
symmetry, whereas ours is highly asymmetric owing to reconnection with
the IMF. In our case, the dipole also rotates diurnally, such that the
pole will in 6 hours be pointing duskward, returning the global
magnetosphere to a more normal two-cusp, two-lobe configuration, albeit
one that still has its magnetic poles at the equator. Then the pole will
rotate to the tail, through dawn, and back to the orientation shown
here. It should be apparent at this point that a magnetosphere like this
one will generate an auroral light show like none in recorded history.

![](media/image9.pct){width="3.2256944444444446in"
height="3.0625in"}![](media/image10.pct){width="3.422222222222222in"
height="3.301388888888889in"}

*Figure 6. Left -- X-Y and X-Z slices with color contoured total
pressure and vector flow. A Y-Z slice at right is offset to X=-12.5.
Reconnection flows are visible in the upper left magnetopause region.
Right -- Similar slices but zoomed out, with color contoured solar wind
pressure in the ecliptic plane and representative magnetic field lines
in the upper box, showing offset plasma sheet formation.*

## Science Objectives

The following objectives are set for their significance to the space
physics community at large and because they are addressable using the
tools we have developed and extended in our previous studies:

1.  Develop a global model of the current magnetosphere with a realistic
    extended ionosphere including photothermal and induced outflows, and
    use it to investigate common space weather events.

2.  Consider and investigate the long term behavior of the magnetosphere
    using the global simulation for cases ranging through all phases of
    a simulated geomagnetic reversal.

3.  Investigate the kinetic behavior of particles in the simulated
    present and future magnetospheres using kinetic simulations in
    global simulation fields, over the relevant energy range.

4.  At phases of geomagnetic reversal for which the Earth's
    magnetosphere closely resembles those of the other terrestrial
    planets, compare results with relevant observations and tailored
    simulations.

### The Extended Ionosphere

An important aspect of the proposed work is the specification of the
ionospheric boundary conditions, both as lower boundary conditions for
the multi-fluid code, and as source distributions for phase space
density weighting of single particle trajectories. To do this, we will
use outflow observations and modeling results from the literature,
especially results that have been obtained from the FAST mission by R J
Strangeway and coworkers \[Strangeway et al., 2000; 2003\], as well as
similar work being done on the Polar spacecraft data set \[Zheng et al.,
2003\]. Representative results illustrating the two main parameters from
the latter study are illustrated in **Figure 7,** Here the the DC
Poynting flux and the precipitating electron density were confirmed as
the most powerful drivers of total outflow flux.
![](media/image11.png){width="3.3652777777777776in"
height="2.2104166666666667in"}![](media/image12.png){width="3.3055555555555554in"
height="2.1666666666666665in"}

*Figure 7. Results from a Polar Mission study of the local influences on
ionospheric outflow using perigee pass data (\~5000 km altitude) from 19
events. The two parameters that emerged as the strongest determinants of
outflow flux were the DC Poynting Flux and the precipitating electron
density (strongly weighting low enery electrons around 3-100 eV), in
agreement with FAST results reported by Strangeway et al. \[2002\].*

Following suggestions made during discussions at the annual NSF-GEM
workshops, we will develop a boundary module for outflow response to
local conditions to be supplied to the multi-fluid code, to assure a
degree of self-consistency and responsiveness to system feedback. We
will scale the heavy ion outflow with the important energy fluxes into
the ionosphere implied by multi-fluid conditions of density,
temperature, and electric field, representing both the electromagnetic
(Poynting) flux and the particle precipitation energy flux, or a
suitable proxy for each. This relationship will be presumed to depend
only on solar conditions and to be independent of all other parameters.

The induced heavy ion outflow flux will be superposed upon a pervasive
photothermal light ion outflow flux, assumed to fill the plasmasphere
and exist everywhere outside of it. The magnitude of this outflow flux
will depend only on solar zenith angle \[Su et al., 1998\] and high
altitude pressure buildup. A steady state model will therefore create a
plasmasphere as an intrinsic feature of the model. When simulating
dynamic storm events, the resultant plasmasphere will respond
self-consistently to the global convection pattern, producing the
observed drainage plumes that supply light ion plasma to the dayside
magnetopause region \[Chandler et al., 2003\].

### Magnetospheric Impact

Winglee et al. \[TBD\] have shown that the clearest impact of
ionospheric plasma on the magnetosphere is mass loading of convection,
with substantial reduction of the transpolar potential reaching the
ionosphere. This corresponds to the absorbtion of energy by acceleration
and heating of extended ionospheric plasma in the lobes, plasma sheet,
and ring current regions. Essentially, energy dissipation (**JE** \> 0)
becomes much more widely distributed rather than being limited to the
ionosphere proper. With our improved, realistic description of the
extended ionosphere, we will revisit the impact of ionospheric plasmas
and their energy absorbing capabilities, looking for new modes of
behavior as well as other, more subtle and-or quantitative changes in
magnetospheric dynamics stemming from the presence of an extended
ionosphere.

Recent observations and modeling results have made it clear that, even
during relatively quiet times (except for northward IMF periods), the
photothermal outflows of lobal winds supply the plasma sheet with a
substantial amount of plasma, while at the same time, evidence has been
found that solar wind plasmas present in the more distant tail, beyond
about 30 RE, have very little opportunity to be transported back to the
near-Earth region. Our suspicion is that a serious modeling effort to
include a realistic extended ionosphere, such as we propose, will
suggest that the principal energy flow in the magnetosphere is from the
solar wind to the extended ionosphere, and thence into the ionosphere
proper, with relatively little re-energization of solar wind plasmas
that have been slowed down by their interaction with the dayside or
flank magnetopause regions. If this is borne out, it will force a
substantial revision of the current paradigms of magnetospheric physics.

The impact of the extended ionosphere will only increase as the Earth
progresses further into the current geomagnetic field reversal. To study
this quantitatively, we will be rebuilding our simulations with selected
typical snapshots of the geomagnetic field from the simulations of
Glatzmaier and Roberts \[1995\]. For example, in case g of Figure 2, the
magnetic field magnitude is substantially depressed from our present
field, and is dominated by the higher multipoles, as illustrated in
**Figure 8.**

![](media/image13.png){width="3.3333333333333335in"
height="3.3333333333333335in"}![](media/image14.png){width="3.3333333333333335in"
height="3.3333333333333335in"}

*Figure 8. A comparison of the size of the 30 nT isosurface for the IGRF
(2002 geomagnetic field; mainly dipolar on this scale) and for the
Glatzmaier et al. \[1999\] field during a simulated geomagnetic minimum
during a reversal event (case g of Figure 2). It is irregular, with a
prominent lumps and dimples.*

It is clear from Figure 8 that Earth will have a much smaller
magnetosphere than at present, and that it will have many unfamiliar
features, including weak field regions such as the dimple there. It is
clear tha the magnetosphere will be substantially less effective as a
shield from external radiation, and that it's patterns of convection,
auroral formation, and energetic particle acceleration will be
substantially different as well. All of these things can be calculated
and evaluated using the tools we propose to develop. A major determinant
of the behaviors of such a magnetosphere is the occurrence of
reconnection that links it with the external solar wind medium.

### Reconnection Impact

**Figure 9** is a sketch of the qualitative nature of a high-tilt
magnetosphere as it would be realized if a geomagnetic field reversal
passes through a state with the dipole axis normal to the spin axis. The
view is in the ecliptic plane of the average Parker spiral
interplanetary field. The planetary rotation phase is captured here at
the moment when the dipole axis points sunward, a real simulation for
which was described in the previous section (albeit with opposite pole
orientation).

It is immediately apparent that the concept of magnetic local time in
such a system will lose its usual meaning. The magnetic tilt of such a
magnetosphere will undergo a diurnal cycle over the full range of
possible values. The aurora will become a mid to low (geographic)
latitude phenomenon, favoring certain geographic longitudes, depending
on the reduction of the dipole moment. Moreover, the aurora will also
undergo a diurnal cycle in which it twice a day assumes forms that are
familiar from our present magnetosphere (apart from their geographic
distribution), with both dusk and dawn ovals exhibiting dayside and
nightside parts that are distinct from each other. During the
intervening UT quadrants like the one shown in Figure 9, when the ovals
are centered near noon and midnght, the entire dayside auroral zone
should more closely resemble our present dayside auroras, while the
entire nightside auroral zone should more closely resemble our present
day nightside auroras.

Using field configurations as given by geodynamo simulations, we will
build a corresponding series of global magnetospheric simulations that
support determination of a quantitative form of the magnetosphere,
including its circulation and energy flow patterns.

![](media/image15.png){width="3.3979166666666667in"
height="2.6430555555555557in"}![](media/image16.png){width="3.2881944444444446in"
height="2.5409722222222224in"}

*Figure 9. A sketch showing (left) the qualitative nature of a high-tilt
magnetosphere with an IMF, as the ecliptic plane projection of magnetic
field lines and flows. The axis of rotation remains near normal to this
plane. The right panel shows the expected ionospheric convection pattern
from two perspectives as indicated.*

The very high tilt (90˚) cases will provide an invaluable exploration of
the effects of IMF orientation over a wider range than we have
previously seen or simulated, testing our ideas concerning the
distribution and operation of dayside reconnection. The sketch in Figure
9 has been drawn based upon our recent results in this area \[Moore et
al., 2002\]. In three dimensions, we expect that the reconnection X-line
will form at the dipolar magnetic longitude where the IMF and dipole
field are anti-parallel, and radiate away from that site along a curve
that will circumnavigate in some fashion the single sunward cusp, the
reconnection rate having a significant peak where the fields are
anti-parallel, and lower rates elsewhere along the X-line. This
reconnection will drive a convective flow across the dayside polar cap
from the dipole longitude of anti-parallel fields to the dipole
longitude of parallel fields. Our first simulation efforts, as reported
above, are qualitatively consistent with this description, though
details remain to be studied. On the nightside a neutral sheet will be
created as roughly a half cylinder shape, dividing sunward from tailward
directed field, and reconnecting in such a way as to return flux to the
inner part of the magnetosphere. As strange as this magnetosphere
appears, it still will have some familiar features and functions.

The past two years have brought a revolution in our appreciation for the
reality of storm-time plasmaspheric erosion \[Sandel et al. 2001; Su et
al., 2001; Foster et al., 2002\] and its impacts on the dayside
magnetopause region, as well as the other regions downstream in
magnetospheric circulation. Supporting these remote sensing observations
are an increasing number of reports \[Sauvaud et al., 2001; Chandler and
Moore, 2003; Chen and Moore, 2003\] showing that relatively cold
ionospheric plasma is a substantial component of the outer dayside
magnetosphere, just inside the magnetopause.

The implications of these newly discovered facts include a potential
impact on dayside reconnection, since the amount of ionospheric plasma
varies broadly from less than 0.1 cm-3 to over 50 cm-3 at the subsolar
magnetopause, depending on the history of convection. This implies a
similar variation of the Alfvén speed and the limiting rate of
reconnection in that region. Thus, we have the prospect that
magnetospheric circulation driven by dayside reconnection should be
self-limiting when it draws a substantial part of the plasmasphere out
to the subsolar region, depressing the local Alfvén speed. With a much
smaller, possibly complex magnetosphere during a reversal, extended
ionospheric plasma transport will be increasingly prominent in the
magnetopause region.

### Plasma Sheet and Energetic Particles

We will investigate the non-adiabatic kinetics that occur in the field
reversal magnetosphere, including particle acceleration to plasma sheet,
ring current, and radiation belt energies by processes known to be
important in the present day magnetosphere. The pervasive features of
inner magnetospheric circulation will include the induced
oxygen-enhanced cleft plasma fountain and high latitude photothermal
flows (referred to here as "lobal winds"), hot outflows from the auroral
zones ("auroral winds"), bidirectional streaming distributions, and
resultant hot isotropic distributions of plasma.

![](media/image17.png){width="4.095833333333333in"
height="2.6944444444444446in"}![](media/image18.png){width="2.5236111111111112in"
height="2.5625in"}

*Figure 10. A kinetic simulation of the magnetosphere based on polar
wind H^+^ trajectories in empirical model fields (Tsyganenko 89, level
2, modified Stern-Volland with appropriate transpolar potential \~25kV),
using the full motion code of Delcourt. Based on 20000 particles emitted
from all local times and latitudes above 55˚ invariant, velocity space
distributions have been integrated in 1 RE cubes to derive the plasma
pressure.*

The study will begin with electromagnetic fields within which the test
particles will travel, determined from the multifluid magnetodynamic
simulations. Next, particle weightings and trajectory initial conditions
will be set based on the global simulated lobal and auroral wind
properties and spatial distributions. A large number of particle
trajectories will be launched with random spacing across the range of
parameters indicated by the observations, in both velocity space and
physical space. A prototypical example of the resultant trajectory
database is shown in **Figure 10**, where we have used empirical
photothermal light ion outflow results and empirical field models to
exercise the trajectory simulation and database codes. We have populated
space with over 20000 particles here, so that their distribution can be
examined within relevant parcels to investigate the opening hypotheses.
It can be seen in Figure 10 that a clear plasma sheet is formed as the
particles are compressed nonadiabatically in preparation for Earthward
transport, and accelerated substantially. The eventual pressures in the
inner magnetosphere approach 1 nPa, comparable with moderate ring
current pressures. Other plots (not shown) of parallel flows demonstrate
the formation of a layered plasma sheet boundary region of nested
tailward and Earthward flows. Perpendicular flows are largely random but
a clear westward drift emerges in the inner plasma sheet and the entire
ring current region torus.

This preliminary effort must be complemented by similar studies of
entering solar wind particles, as well as induced ionospheric outflows
of heavy ions. We will investigate these energetic particle populations
in the current and future magnetosphere in these and other ways using
the tools described below.

## Proposed Approach

We propose a coupled test particle and kinetic 3D magnetospheric
simulation effort, using global multi-fluid magnetodynamic MFMD
simulations to create the field and plasma source context within which
we will study localized departures from adiabaticity.

### Multi-fluid MagnetoDynamic and MHD Models

We have successfully developed a kinetic particle interface with the
Lyon Fedder Mobarry single fluid MHD code, and thereby demonstrated the
feasibility of this work with a single fluid model. It will be
relatively straightforward to carry this over to a multi-fluid code
having similar computation grid.

The multi-fluid magnetodynamic code we will use was developed and
reported by R. M. Winglee \[1998, 2000\], to which the reviewer is
referred for substantial details, which include a description of the
partial inclusion of parallel pressure gradient and magnetic drift
effects, albeit at the thermal speed only. This remains the only model
of which we are aware that currently includes a separate fluid (or
fluids) representing ionospheric outflows. However, this statement may
no longer be valid by the time this work begins, as other simulation
efforts are picking up on this practice. One of our top priorities will
be to compare specific cases with and without substantial photothermal
ionospheric outflows, and with and without substantial induced heavy ion
outflows. This will substantiate the effects of an extended ionospheric
fluid within the simulation space, which is also relevant to comparisons
with other magnetospheres such as that of Mercury, where the ionospheric
source is much less important dynamically, or Venus, where it is much
more important.

### Outer Magnetosphere Full Particle Model

Our test particle model has been described extensively elsewhere \[e.g.
Delcourt et al., 1993, and references therein\]. Empirical 3D models of
magnetospheric magnetic and electric fields have been used extensively
as a basis. For each time step, the fields can be locally evaluated by
tracing a triad of field lines to the ionosphere to map the electric
field model to the particle position. This technique compensates with
accuracy for what it gives up in computational efficiency, as
demonstrated by our test of reversibility in connection with exploration
of the plasma sheet source groove \[Moore et al., 2000\].

The software interfaces we have recently added now allow the use of any
available model that returns the required fields from positional inputs,
within practical computational time scales.

In this model, ensembles of particles are initiated from appropriate
source locations with characteristic initial conditions, and advanced in
the model fields using the full equations of motion. We have the choice
of whether to use empirical analytic fields expressed in the ionosphere
or local specification of the electric field by a 3D simulation. An
interpolation scheme is used to obtain the field at points within an
global computational grid, with acceptable loss of accuracy, limiting to
some degree the long-range accuracy of the trajectories.

We also propose to extend the use of this particle model to investigate
the acceleration of electrons in the plasma sheet, looking for the
effects that result in their relatively low temperature as compared with
the co-located ions. This will require us to work with global simulation
fields rather than empirical ionospheric convection patterns.

### Inner Magnetosphere Kinetic Particle Model

The inner magnetosphere model we will use in this work is the Fok
kinetic model that solves a Boltzmann initial/boundary value problem
with specified electric and magnetic fields, including the effects of
charge exchange losses, wave particle diffusion effects, and Coulomb
drag on energetic particles interacting with hydrogen geocorona and the
plasmasphere, respectively. Rather than tracking particles trajectories
in detail, a bounce-averaged approach is taken. A full description of
this ring current model is given in Fok et al. \[1995, 1996, 2001a\].

The Fok kinetic model has recently been combined with the Rice
convection model (RCM) to provide self-consistent electrodynamic
coupling with the ionosphere proper (Comprehensive RCM or CRCM). To
couple with the Fok model, the RCM algorithm for calculating Birkeland
current has been generalized to arbitrary pitch angle distribution \[Fok
et al., 2001b\]. Given a specified ionospheric conductance and initial
ring current distribution, the RCM component of the CRCM computes the
ionospheric electric field and currents. The Fok model then advances the
plasma distribution using the electric field computed by the RCM and at
the same time calculates particle losses along drift paths. The updated
distributions are then returned to the CRCM to complete the computation
cycle. Input models required for running the CRCM include a magnetic
field model, transpolar potential, an ionospheric conductance model, and
the plasma sheet distribution function at the equator at the CRCM outer
boundary.

Overall, the global fields and plasma inputs to the magnetotail will be
produced using the Winglee MFMD, based on a physical-empirical model of
ionospheric outflows and their response to fluid conditions at the inner
boundary of the multi-fluid simulation. The plasma sheet effects on
inflowing plasmas will be included using the Delcourt 3D particle motion
code. The effects within the inner magnetosphere will be included using
the CRCM, which includes ionospheric electrodynamics coupling. The
combination of these models provides the best of all worlds by including
self-consistent fields both globally and within the inner magnetosphere,
while tracking important non-adiabatic effects where they are important.

### Work Plan

Year 1

-   Implement photothermal outflows and corotation to generate a
    simulated plasmashere and polar wind. Test the impact of these
    outflows on the present magnetosphere using reference events.

-   Implement induced auroral heavy ion outflows in response to energy
    inputs from the global simulation. Test the impact of these outflows
    on the present magnetosphere.

-   Complete a study of the high tilt magnetosphere with revised
    photothermal and induced outflows.

-   Extend these results to reveal diurnal dynamics of a high tilt
    magnetosphere.

Year 2

-   Replace the MFMD dipole field with a multipole expansion, set by
    geodynamo simulation, beginning with the present magnetosphere.

-   Simulate the magnetosphere using reference events, for
    representative phases of geomagnetic reversals, from the present
    field to the dipole moment minimum of a reversal.

-   Perform test particle studies of nonadiabatic behavior and particle
    acceleration for each phase.

-   Identify baseline behavior and response to solar wind variability
    for each phase.

Year 3

-   Adapt the resultant code to Mercury by scaling back the extended
    ionosphere; and compare behavior with Mariner 10 observations,
    remote observations, and other simulation efforts.

-   Adapt the resultant codes to Mars and compare behavior with
    observations and other efforts.

-   Adapt kinetic inner magnetosphere code for each phase, and compute
    energetic particles for each phase.

-   Adapt the resultant codes to Venus and compare behavior with
    Pioneer-Venus and other efforts.

## 

## 

## 

## Closure and Relevance

The proposed work will:

-   Incorporate ubiquitous photothermal and induced ionospheric
    outflows, with dependence on local conditions, into a global
    simulation, and determine the impact of the ionospheric plasma.

-   Predict behaviors of the ionospheric-dominated magnetosphere during
    geomagnetic field reversals, particular auroral and storm plasma
    formation at various stages of reversal.

-   Explore the heliospheric interaction with other terrestrial planets,
    Mercury, Mars and Venus, including evaluations of production of
    escaping fast neutral atoms.

The proposed work falls within the areas known as "magnetospheric
physics" and \"comparative magnetospheres\", and supports NASA missions
with objectives in these areas. The NAS Decadal Research Strategy in
Solar and Space Physics recognizes this area thusly (p.11): \"The
comparative study of planetary ionospheres and magnetospheres is a
central theme of solar and space physics research.\" The SEC 2002
Roadmap (p.29) states that SEC missions traditionally fall into one or
more of the four broad disciplines: solar, heliospheric, magnetospheric
(including comparative magnetospheres), and
ionospheric-thermospheric-mesospheric (ITM).\"

While it is clearly impossible to plan now for a NASA mission to the
terrestrial magnetosphere at the time of minimum field intensity, all
magnetospheric missions are inherently planned for a field reversal
period, insofar as the decline of the dipole moment is known to have
accelerated markedly during the past 10-30 years. The following missions
in the SEC Roadmap are specifically targeted toward comparative
magnetospheric study of other solar system bodies that are in states
resembling the terrestrial magnetosphere during a field reversal
episode: Bepi-Colombo (Mercury), Mars Aeronomy Probe, Solar Connections
Observatory for Planetary Environments (SCOPE), and Venus Aeronomy
Probe.

Moreover, the SEC Roadmap (p.64-65) addresses the means for the study of
comparative magnetospheres, stating: \"while (Discovery) missions focus
upon planetary themes, NASA and the planetary community should remain
open to including Discovery missions that address comparative planetary
environments.\"\....\"Historically, the major advances in both
heliospheric physics and comparative magnetospheres resulted from
collaboration between the Sun-Earth Connection and Solar System
Exploration.\" The Decadal Research Strategy makes a specific
recommendation that \"The scientific objectives of the NASA Discovery
Program should be expanded to include those frontier space plasma
physics research topics that could not otherwise be accommodated by
other spacecraft opportunities.\"

The recommended missions cannot be conducted effectively without the
proposed Geospace community effort to anticipate and predict the
environments that will be encountered at other planets. Such efforts
must be based upon knowledge gained in the terrestrial space environment
as embodied in our best simulation models of this system. The proposed
effort to compare simulations with planetary observations will lead to
high confidence in the credibility of our predictions for those planets
as well as the field reversal magnetosphere of our own planet.

This work extends the SEC study of geospace response (to the solar and
geomagnetic variability) to the longer time scales of "space climate".
Beyond the solar cycle and its minima lie the geomagnetic field
reversals, with time scales of a few 100 yrs to a few 100 kyr, with
minima resembling those of the solar cycle extending to 100 Myr and
possibly longer. By addressing geological time scales and events with
possible biological impacts \[e.g., Reid et al., 1975\], this study will
enhance linkages between the Sun Earth Connections, Planetary Origins,
and Structure and Evolution of the Universe themes. The proposed work
supports existing efforts to model and simulate global geospace
circulation by extending them to conditions beyond the range for which
typical codes have been developed and tested. It will make use of
existing and future observations of terrestrial planets to validate the
predictions made, provide robust improvements in the generality of space
environment simulations, and extend the state of the art in
magnetospheric simulation.

## 

## 

## Management and Cost

This modeling effort will make use of established cooperative agreements
between the Goddard Space Flight Center and the Universities Space
Research Association in Greenbelt MD. This agreement allows incremental
funding of research efforts, and the onsite housing of research
associates within Goddard Space Flight Center. It is anticipated that a
part of the support requested in this proposal will be applied to the
salary of USRA research associates who may support this and other tasks.

## Responsibilities of Key Personnel

Dr. T. E. Moore, principal investigator, will guide the overall science
effort goals and implementation of the investigation, assuring that
priority is placed upon the best tradeoff between attainability and
scientific importance. He will participate directly in planning and
executing the simulation work including development of suitable model
inputs from observations, validation of the results obtained, the
comparison of the results with appropriate data sets, and the
presentation and publication of the results.

Dr. M.-C. Fok, coinvestigator, is a research scientist with the GSFC
Interplanetary Physics Branch, and is the principal architect of the
kinetic energetic particle simulation model used in this work. She is
also responsible for the modification of the test particle code to use
global simulation fields rather than empirical model fields. She will
participate in the proposed work on a day-to-day basis.

Dr. N. Tsygananko, coinvestigator, is a research scientist with USRA,
Greenbelt MD. He will assist in the definition of the internal magnetic
field for the simulation model, based on the Glatzmaier geodynamo
simulation.

Dr. D. C. Delcourt, collaborator, is the architect of the 3D particle
simulation code. He will participate in the definition of scientific
goals and in the development of appropriate physical model and code
features, and in the execution and interpretation of model run results,
via network communications and teleconferencing, as well as periodic
meeting attendance and visits.

Dr. G Glatzmaier, collaborator, is professor at the University of
Southern California and director of the institute for... He will supply
us with multipole expansions of the geodynamo fields produced in his
simulations for selected states or phases of the reversal process, as
necessary.

Dr. R. M. Winglee, collaborator, is the principal architect of the
multifluid magnetodynamic simulation code. He will support and review
adaptations of his code, for use in specifying self-consistent fields
within which test particle motions will be computed, as well as for
specifying flux inputs into critical regions of the magnetosphere.

Dr. M. Hesse, collaborator, is the director of the GSFC Community
Coordinated Modeling Center. He will support independent validation runs
using CCMC public codes, specifically the BatsRUS global MHD simulation,
as validation and for comparison with the results from the multifluid
magnetodynamic simulation.

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# Appendix 2: CURRICULUM VITAE

## Dominique C. Delcourt, Research Scientist

Centre d\'etudes des Environnements Terrestre et Planetaires (CETP), 4,
Avenue de Neptune,

94107 - Saint Maur des Fosses. France

Dr. Delcourt received the M.S. in Physics from Universite de Paris XI,
Orsay, France, in 1981, and the Ph.D in Astronomy and Space Technics
from University Paul Sabatier, Toulouse, France, in 1985. Dr. Delcourt
was awarded a National Research Council Research Associateship in 1986,
for research on the interpretation of Dynamics Explorer data on the
basis of three dimensional particle trajectory calculations. He spent
two years with the Space Science Laboratory, Marshall Space Flight
Center, working with the Retarding Ion Mass Spectrometer (RIMS) science
team in data analysis and interpretation. This work has led to the first
quantitative global description of ionospheric plasma transport within
the magnetosphere \[Delcourt et al., 1989\]. He was a research fellow of
the Space Science Department of ESA/ESTEC from 1988 to 1991, and has
extended his modeling efforts to include dynamic phenomena in the
magnetosphere, particularly with regard to the particle acceleration
effects of transient electric fields induced by the substorm dynamics of
the magnetotail. Dr. Delcourt was awarded his Habilitation (to supervise
student research) by the University Paul Sabatier (Toulouse III),
Toulouse, France, in December, 1989. In 1991 he joined the research
staff of the Universities Space Research Association, Huntsville, AL,
working at the Marshall Space Flight Center on magnetospheric plasma
transport. In 1992, he joined the research staff of CRPE (now CETP)
which is a CNRS laboratory dedicated to the study of Earth and planetary
environments. He is continuing his study of magnetospheric plasma
transport and energization using a combination of in-situ measurements
and numerical simulations.

## Selected Publications 

Delcourt, D. C., C. R. Chappell, T. E. Moore, and J. H. Waite Jr., A
three-dimensional numerical model of ionospheric plasma in the
magnetosphere, J. Geophys. Res., vol. 94, p. 11893, 1989.

Delcourt, D. C., J.-A. Sauvaud, and A. Pedersen, Dynamics of
single-particle orbits during substorm expansion phase, J. Geophys.
Res., vol. 95, p. 20853, 1990.

Delcourt, D. C., J.-A. Sauvaud, and T. E. Moore, Cleft contribution to
ring current formation, J. Geophys. Res., vol. 95, p. 20937, 1990.

Delcourt, D. C., and T. E. Moore, Precipitation of ions induced by
magnetotail collapse, J. Geophys. Res., vol. 97, p. 6405, 1992.

Delcourt, D. C., T. E. Moore, J.-A. Sauvaud, and C. R. Chappell,
Non-adiabatic transport features in the outer cusp region, J. Geophys.
Res., vol. 97, p. 16833, 1992.

Delcourt, D. C., J.-A. Sauvaud, and T. E. Moore, Polar wind ion dynamics
in the magnetotail, J. Geophys. Res., vol. 98, p. 9155, 1993.

Delcourt, D. C., T. E. Moore, and C. R. Chappell, Contribution of
low-energy ionospheric protons to the plasma sheet, J. Geophys. Res.,
vol. 99, p. 5681, 1994.

Delcourt, D. C., R. F. Martin Jr., J.-A. Sauvaud, and T. E. Moore,
Centrifugal trapping in the magnetotail, Annales Geophys., vol. 13, p.
242, 1995.

Delcourt, D. C., J.-A. Sauvaud, R. F. Martin Jr., and T. E. Moore, On
the nonadiabatic precipitation of ions from the near-Earth plasma sheet,
J. Geophys. Res., vol. 101, p. 17409, 1996.

Delcourt, D. C., G. Belmont, J.-A. Sauvaud, T. E. Moore, and R. F.
Martin Jr., Centrifugally-driven phase bunching and related current
sheet structure in the near-Earth magnetotail, J. Geophys. Res., vol.
101, p. 19839, 1996.

Delcourt, D. C., J.-A. Sauvaud, and T. E. Moore, Phase bunching during
substorm dipolarization, J. Geophys. Res., vol. 102, p. 24313, 1997.

Delcourt, D. C., and G. Belmont, Ion dynamics at the earthward
termination of the magnetotail current sheet, J. Geophys. Res., vol.
103, p. 4605, 1998.

Delcourt, D. C., and J.-A. Sauvaud, Recirculation of plasma sheet
particles into the high-latitude boundary layer, J. Geophys. Res., vol.
103, p. 26521, 1998.

Delcourt, D. C., and R. F. Martin Jr., Pitch angle scattering near
energy resonances in the geomagnetic tail, J. Geophys. Res., vol. 104,
p. 383, 1999.

## Mei-Ching Fok, Astrophysicist

NASA Goddard Space Flight Center, Code 692, Greenbelt, MD 20771

Dr. Mei-Ching Fok received the B. S. degree in Physics from the Chinese
University of Hong Kong (CUHK) in 1980. She spent the year after in the
Physics Department at CUHK as a teaching assistant. From 1981-1985, she
taught Physics and Mathematics in a high school in Hong Kong. In the
summer of 1985, she came to the United States with her husband to pursue
graduate studies. In 1987, Dr. Fok received the M. S. degree in Physics
from the Eastern Michigan University. In the following year, she was
admitted to the Ph. D. program in the Department of Atmospheric, Oceanic
& Space Sciences at the University of Michigan and received her Ph. D.
degree in August 1993. Three months later, she was awarded an NAS/NRC
Resident Research Associateship at NASA/Marshall Space Flight Center. In
1995 after she left the NRC program, she joined the Universities Space
Research Association (USRA) at MSFC. In August 1997, Dr. Fok was
transferred within USRA to the Goddard Space Flight Center to follow her
NASA sponsor, Dr. Thomas E. Moore. She became a NASA employee in May
2001.

During her doctoral study, she performed statistical studies on the
subauroral electron temperature enhancement, using measurements from
AE-C and DE 2 satellites. Dr. Fok also developed a kinetic model to
study the dynamics of the storm time ring current ions and the
associated effects on the plasmasphere-ionosphere system. Her model is
the first ring current model that incorporates a time-dependent
plasmasphere model and thus resolves the instantaneous coupling between
the energetic and thermal plasmas. At the Marshall Space Flight Center,
Dr. Fok extended her ring current model into 3 dimensions and included
realistic magnetic field configurations. Her model has been used to
simulate the energetic neutral atom (ENA) emissions in the inner
magnetosphere in support the IMAGE mission. She continues her work at
GSFC on global modeling through wide collaborations with the modeling
group at the Rice University, the MHD group at the University of
Michigan, and scientists at CETP, France.

Selected Publications:

Fok, M.-C., R. A. Wolf, R. W. Spiro, and T. E. Moore, Comprehensive
computational model of the Earth\'s ring current, *J. Geophys. Res.,
106*, 8417-8424, 2001.

Fok, M.-C., T. E. Moore, and W. N. Spjeldvik, Rapid enhancement of
radiation belt electron fluxes due to substorm dipolarization of the
geomagnetic field, *J. Geophys. Res., 106*, 3873-3881, 2001.

Fok, M.-C., T. E. Moore, and D. C. Delcourt, Modeling of inner plasma
sheet and ring current during substorms, *J. Geophys. Res.*, *104*,
14,557-14,569, 1999.

Fok, M.-C., and T. E. Moore, Drift-shell splitting in an asymmetric
magnetic field, in *Geospace Mass and Energy Flow: Results From the ISTP
Program*, *Geophys.* *Monogr. Ser.*, *vol. 104*, edited by J. L. Horwitz
et al., pp. 327-331, AGU, Washington, D. C., 1998.

Fok, M.-C., and T. E. Moore, Ring current modeling in a realistic
magnetic field configuration, *Geophys. Res. Lett.*, *24*, 1775-1778,
1997.

Fok, M.-C., T. E. Moore, and M. E. Greenspan, Ring current development
during storm main phase, *J. Geophys. Res.*, 101, 15,311, 1996.

Fok, M.-C., T. E. Moore, J. U. Kozyra, G. C. Ho, and D. C. Hamilton,
Three-dimensional ring current decay model, *J. Geophys. Res.*, *100*,
9619, 1995.

Fok, M.-C., J. U. Kozyra, A. F. Nagy, C. E. Rasmussen, and G. V.
Khazanov, Decay of equatorial ring current ions and associated
aeronomical consequences, *J. Geophys. Res.*, *98*, 19,381, 1993.

Fok, M.-C., J. U. Kozyra, A. F. Nagy, and T. E. Cravens, Lifetime of
ring current particles due to Coulomb collisions in the plasmasphere,
*J. Geophys. Res.*, *96*, 7861, 1991.

## Gary A Glatzmaier, Professor of Earth Sciences

University of California, Santa Cruz

Dr. Gary A Glatzmaier received a Bachelor of Science degree, magna cum
laude, from Marquette University in 1971 and then served four years as
an officer in the U.S. Navy teaching nuclear reactor physics. In 1980 he
he received a Ph.D. in Physics from the University of Colorado. After
two post doctoral positions, he spent 16 years at the Los Alamos
National Laboratory developing three-dimensional time-dependent computer
models to study the internal structure and dynamics of planets and
stars. In 1998 he became a Professor of Earth Sciences at the University
of California, Santa Cruz. In his studies of the Earth he developed
separate models that simulate the global circulation and convection in
the Earth\'s atmosphere, mantle and core. He produced the first
successful computer simulations of the geodynamo, the mechanism in the
Earth\'s fluid outer core that maintains the geomagnetic field. He has
been an associate editor of the Geophysical and Astrophysical Fluid
Dynamics journal since 1990 and has served on scientific committees for
the AGU, SEDI, NRC, NSF, NASA, and DOE. He is a Fellow of the Los Alamos
National Laboratory and of the American

Geophysical Union and in 1996 won IEEE Sydney Fernbach Award for his
geodynamo simulations. He is currently the Director of the Center for
the Origin, Dynamics and Evolution of Planets within the Institute of
Geophysics and Planetary Physics at UC Santa Cruz.

Glatzmaier, G.A. (2002) Geodynamo simulations - How realistic are they?
Ann. Rev. Earth Planet. Sci., 30, 237-257.

Roberts, P.H. and Glatzmaier, G.A. (2000) Geodynamo theory and
simulations, Rev. Mod. Phys. 72, 1081-1123.

Glatzmaier, G.A., Coe, R.S., Hongre, L. and Roberts, P.H. (1999) The
role of the Earth\'s mantle in controlling the frequency of geomagnetic
reversals, Nature 401, 885-890.

Glatzmaier, G.A. and Roberts, P.H. (1997) Simulating the geodynamo,
Contemp. Physics, 38, 269-288.

Glatzmaier, G.A. and Roberts, P.H. (1996) Rotation and magnetism of
Earth\'s inner core, Science, 274, 1887-1891.

Glatzmaier, G.A. and Roberts, P.H. (1995) A three-dimensional
self-consistent computer simulation of a geomagnetic field reversal,
Nature, 377, 203-209.

Glatzmaier, G.A., Schubert, G. and Bercovici, D. (1990) Chaotic,
subduction-like downflows in a spherical model of convection in the
Earth\'s mantle, Nature 347, 274-277.

Hart, J.E., Glatzmaier, G.A. and Toomre, J. (1986) Space-laboratory and
numerical simulations of thermal convection in a rotating hemispherical
shell with radial gravity, J. Fluid Mech. 173, 519-544.

Glatzmaier, G.A. (1984) Numerical simulations of stellar convective
dynamos. I. The model and method, J. Comp. Phys., 55, 461-484.

## Thomas E. Moore, Branch Head

Interplanetary Physics Branch, NASA Goddard Space Flight Center,
Greenbelt, MD USA 20771

[Thomas E. Moore]{.underline} earned the B.S. in Physics in 1970, and
the M.A. in 1971, from the University of New Hampshire. He received the
Ph.D. in Astrogeophysics from the University of Colorado, Boulder in
1978. Returning to the University of New Hampshire, he worked on the
dynamics of the plasma environment at geosynchronous orbit, pioneering
the use of multiple spacecraft to resolve the space-time structure of
magnetospheric substorm injections. He also was active in the
observation of plasma and energetic particles above auroral displays
from sounding rocket platforms, and developed the first model of solar
EUV and acceleration effects on the composition of ionospheric outflows.

Dr. Moore joined NASA at Marshall Space Flight Center in 1983 as a
member of the science team for the Retarding Ion Mass Spectrometer on
the Dynamics Explorer Satellite. He has worked actively on the
acceleration and outflow of ionospheric plasma, the resulting source of
plasma for the magnetosphere, and the acceleration of ionospheric plasma
by magnetospheric circulation and substorm phenomena. He supplied
instrumentation for the TOpside Probe of the Auroral Zone (TOPAZ) series
of sounding rocket payloads, the ARCS series of active experiment
payloads, and the SCIFER and CAPER cusp payloads. At MSFC, he became the
principal investigator for the Thermal Ion Dynamics Experiment and
Plasma Source Instrument for the ISTP POLAR spacecraft, and originated
the concept of the geopause, within which the Earth is the dominant
supplier of matter.

Dr. Moore joined the Goddard Space Flight Center in May 1997, to serve
as project scientist for the IMAGE mission, lead coinvestigator for the
Low Energy Neutral Atom imager on IMAGE, and to pursue broader interests
in the heliospheric plasma dynamics and heating. He pursues an active
interest in numerical modeling of space plasmas, and in data
acquisition, manipulation and visualization technologies. He has served
as secretary and program committee member of the American Geophysical
Union, Space Physics and Aeronomy section, and as a member of the Solar
Probe science definition team, and the NASA Sun-Earth Connection Roadmap
Committee. He currently serves as project study scientist for the
Magnetotail Constellation Mission of the Solar Terrestrial Probes
Program, and as a co-chair of the NSF Geospace Environment Modeling
working group on M-I coupling via ionospheric plasma outflows.

**[Selected Publications:]{.underline}**

Moore, T. E., M.-C. Fok, and M. O. Chandler, The dayside reconnection X
line, J. Geophys. Res., 107(A10), 10.1029/2002JA009381, p.SMP 26, 2002.

Moore, T. E., et al., Low Energy Neutral Atoms in the Magnetosphere,
Geophys. Res. Lett. 28, p.1143, 15 March 2001.

Moore, T. E., et al., The Low Energy Neutral Atom Imager for the IMAGE
Mission, Space Sci. Revs, 91(1-2), p.155, 2000.

Moore, T. E., et al., Ionospheric mass ejection in response to a CME,
Geophys. Res. Lett., 26(15), p.2339, 1 Aug. 1999.

Moore, T. E., C. J. Pollock, and D. T. Young, Kinetic core plasma
diagnostics, in Geophysical Monograph #102, p.105, Am. Geophys. Un.,
Washington, DC, 1998.

Moore, T. E. et al., High-altitude observations of the polar wind,
Science, 277, p.349, 1997.

Moore, T. E., et al., Plasma heating and flow in an auroral arc, J.
Geophys. Res. 101, p.579, 1996.

Moore, T.E., and D.C. Delcourt, The Geopause, Revs. Geophys., 33(2), p.
175, 1995.

Moore, T.E., et al., The Thermal Ion Dynamics Experiment and Plasma
Source Instrument, Space Sci. Revs, 71, p.409, 1995.

Moore, T. E., Origins of Magnetospheric Plasma, Rev. Geophys.,
Supplement, p.1039, 1991.

## Nikolai Tsyganenko, Senior Research Scientist

Universities Space Research Association,

**Professional preparation:**

M.S. (1970) and Ph.D. (1974) in Geophysics, from the Dept. of Physics,
University of St.-Petersburg, Russia.

**Positions:**

Aug. 2001 - present Universities Space Research Association Senior
Research Scientist

Feb. 1994 - Aug. 2001 Raytheon ITSS (formerly Hughes STX) Chief
Scientist

Feb. 1992 - Feb. 1994 NASA Goddard SFC / NAS Senior NRC Associate

Mar. 1973 - Feb. 1992 State University of St.-Petersburg, Junior
(1973-77) and Senior (1977-92)

Institute of Physics Staff Scientist

**Research/expertise area:** Space physics/magnetospheric modeling;
authored 75 papers and a monograph.

**Selected recent publications:**

Tsyganenko, N.A., Quantitative models of the magnetospheric magnetic
field: Methods and results, Space Sci. Rev., **54**, 75-186, 1990.

Tsyganenko, N. A., D. P. Stern, and Z. Kaymaz, Birkeland currents in the
plasma sheet, J. Geophys. Res., **98**, 19,455-19,464, 1993.

Tsyganenko, N. A., and M. Peredo, Analytical models of the magnetic
field of disk-shaped current sheets, J. Geophys. Res., **99**, 199-206,
1994.

Tsyganenko, N. A., Modeling the Earth\'s magnetospheric magnetic field
confined within a realistic magnetopause, J.Geophys.Res., **100**,
5599-5612, 1995.

Tsyganenko, N. A., and D.P. Stern, Modeling the global magnetic field of
the large-scale Birkeland current systems, J.Geophys.Res., **101**,
27,187-27,198, 1996.

Tsyganenko, N. A., Modeling of twisted/warped magnetospheric
configurations using the general deformation method, J. Geophys. Res.,
**102**, 23,551-23,564, 1998.

Tsyganenko, N. A., S. B. P. Karlsson, S. Kokubun, T. Yamamoto, A. J.
Lazarus, K. W. Ogilvie, C. T. Russell, and J. A. Slavin, Global
configuration of the magnetotail current sheet as derived from GEOTAIL,
WIND, IMP-8, and ISEE-1/2 data, J. Geophys.Res., **102**, 6827-6841,
1998.

Tsyganenko, N. A., and C. T. Russell, Magnetic signatures of the distant
polar cusps: Observations by POLAR and quantitative modeling, J.
Geophys.Res., **104**, 24,939-24,955, 1999.

Tsyganenko, N. A., Modeling the inner magnetosphere: The asymmetric ring
current and Region 2 Birkeland currents revisited, J. Geophys.Res.,
**105**, 27,739-27,754, 2000.

Tsyganenko, N. A., A model of the near magnetosphere with a dawn-dusk
asymmetry 1.Mathematical structure, and 2. Parameterization and fitting
to observations, J. Geophys. Res., v.107 (A8), doi: 10.1029/2001JA000219
and 10.1029/2001JA000220, 2002a,b.

Tsyganenko, N. A., and T. Mukai, Tail plasma sheet models derived from
Geotail particle data, J. Geophys. Res., v.108 (A3), 1136, doi:
10.1029/2002JA009707, 2003.

Tsyganenko, N. A., H. J. Singer, and J. C. Kasper, Storm-time distortion
of the inner magnetosphere: How severe can it get ? J. Geophys. Res.,
v.108 (A5), 1209, doi: 10.1029/2002JA009808, 2003.

# Appendix 3: CURRENT AND PENDING SUPPORT

## Mei-Ching Fok

##### Agency/Contact Brief Title Period:Funding: Commit

NASA R&A/J. Sharber Plasma Transport & Energization FY02: 0k\$ 20%

NASA IMAGE/J. Spann Low Energy Neutral Atom Imager MO&DA FY02: 10k\$
-FY04 20%

NASA IMAGE/J. Spann IMAGE Theory and Modeling FY02: 27k\$ -FY04 30%

MSFC NSSTC/G. Khazanov UPOS: Radiation Belt Environment FY02: 100k\$ -
FY03 30%

NASA R&A/J. Peterson Modeling of ENA Imagery FY03: 80k\$ -FY05 30%

Pending Support:

NASA EP/M. Mellott SMEX/COMPASS FY04: tbdk\$ - FY08 20%

## 

## Thomas E. Moore

##### Agency/Contact Brief Title Period:Funding Commit

NASA GGS/W. Peterson POLAR/TIDE-PSI MO&DA FY03: 420k\$ -FY04 20%

NASA R&A/W. Peterson Plasma Transport & Energization FY03: 42k\$ 20%

NASA IMAGE/W. Peterson Low Energy Neutral Atom Imager MO&DA FY02: 482k\$
-FY04 20%

NASA IMAGE/W. Peterson IMAGE Mission Scientist FY02: 0k\$ -FY03 20%

NASA STP/W. Peterson Magnetospheric Constellation Study FY02: 0k\$ -
FY12 20%

Pending Support:

NASA EP/M. Mellott Magnetospheric Multiscale Mission FY04: 26k\$ - FY10
20%

NASA EP/M. Mellott SMEX/COMPASS FY04: 67k\$ - FY09 20%

NASA EP/M. Mellott SMEX/IBEX FY04: 26k\$ - FY09 20%

## Nikolai Tsyganenko

##### Agency/Contact Brief Title Period:Funding: Commit

NASA LWS / D. Sibeck Global Modeling of Geomagnetic Field FY03: \$83K -
FY05 40%

NSF / K. Baker Storms in the Inner Magnetosphere FY03: \$65K -FY05 32%

NSF / K. Baker Data-Based Open Magnetosphere FY03: \$36K - FY05 18%

Pending support:

NASA SEC/GI/ W.Peterson Plasma Sheet Based on Geotail Data FY04 -FY06
10%

# Appendix 4: BUDGET SUMMARY for RESEARCH PROPOSAL

## Budget Details and Notes

**Budget Notes**

This proposal budget has been prepared using NASA GSFC guidance for full
cost accounting practices. These practices are incorporated into a
template budget form that has been used as the basis for all rates and
overhead computations in this budget. The budget summary sheets break
out direct civil service labor and "other" cost categories, which
correspond roughly to the new costs associated with full cost accounting
and the "old" costs normally reported for NASA SR&T proposals,
respectively.

# Appendix 5: FINAL PROGRESS REPORT

This report consists of two parts: the section entitled "Recent
Progress" in the main section of the proposal to which this is attached
(not repeated here), and the following section summarizing publication
activity:

**Publications attributed to current SR&T support:**

Cladis, J. B, H. L. Collin, O. W. Lennartsson, T. E. Moore, W. K.
Peterson, and C. T. Russell, Observations of centrifugal acceleration
during compression of the magnetosphere, Geophys. Res. Lett., 27(7),
p.915, 2000. This paper established that centrifugal flinging motions of
field lines can effect substantial acceleration of heavy ions,
especially when the motion is impulsive as in response to the shock
leading a CME.

Cowley, S.W.H., and C. J. Owen, A simple illustrative model of open flux
tube motion over the dayside magnetosphere, Planet. Space Sci., 37(11),
p.1461, 1989.

Delcourt, D.C., T. E. Moore, B. L. Giles, and M.-C. Fok, Quantitative
Modeling Of Modulated Ion Injections Observed By Polar-Tide In The Cusp
Region, J. Geophys. Res., 25(A11), p.25191, 2000. This study shows that
the entry of solar wind plasma is modulated by nonadiabatic effects
owing to the sharp and variable curvature of open field lines connecting
the heliosphere to the geosphere.

Delcourt, D. C. , T. E. Moore, S. Orsini and A. Millilo, J.-A. Sauvaud,
Centrifugal Acceleration Of Ions Near Mercury, Geophys. Res. Lett.,
29(12), p.32-1, 15 June, 2002. This is an initial exploration of
nonadiabatic particle behavior in a much smaller magnetosphere, in which
such behavior is made more pervasive by the small scales of the
structures.

Delcourt, D. C., S. Grimald, F. Leblanc, J.-J. Berthelier, A. Millilo,
A. Mura, S. Orsini, and T. E. Moore, A quantitative model of the
planetary Na^+^ contribution to Mercury's magnetosphere, Ann. Geophys.,
in press, 2003. This paper is discussed in the main body of this
proposal.

Fok, M.-C., T. E. Moore and W. N. Spjeldvik, Rapid enhancement of
radiation belt electron fluxes due to substorm dipolarization of the
geomagnetic field, J. Geophy. Res. 106(A3), p.3873, 2001a. This is our
first exploration into the involvement of substorm dipolarizations in
the acceleration of relativistic radiation belt electrons.

Fok, M.-C., R. A. Wolf, R. W. Spiro, and T. E. Moore, Comprehensive
computational model of the Earth\'s ring current, J. Geophys. Res.,
106(A5), p.8417, 2001b. This effort demonstrated the extension of the
Rice Convection Model to include pitch angle distributions and
conservation of the higher magnetic moments. It has proven immediately
useful in the understanding IMAGE ring current observations.

Fok, M.-C., T. E. Moore, and D. C. Delcourt, Modeling of inner plasma
sheet and ring current during substorms, J. Geophys. Res., 104,
14,557-14,569, 1999. This is the paper, based on empirical field models,
with which our more recent simulations of substorm dipolarization in MHD
fields have been compared.

Fok, M-C, T E Moore, G R Wilson, J D Perez, X Zhang, P C:son Brandt, D G
Mitchell, E C roelof, J-M Jahn, C J Pollock, and R A Wolf, Global ENA
IMAGE simulations, Space Science Revs., in press, 2003.

Horwitz, J. L., and T. E. Moore, Core Plasmas in Space Weather Regions,
IEEE Trans, vol. 28, 6, pp. 1840-1853, December 2000. This a review
paper summarizing the role of low energy geogenic plasmas in space
weather throughout the magnetosphere.

Moore, T E, M O Chandler, D C Delcourt, B L Giles, W K Peterson, C T
Russell, J Wygant, Ionospheric Incorporation into the Plasma Sheet, EOS
Trans. AGU, Spring Meeting Supplement, 2002. This is the initial report
of our Fall 2001 equatorial data set, which will be the basis for our
proposed study of ionospheric incorporation in the plasma sheet.

Moore, T. E., M.-C. Fok, and M. O. Chandler, The dayside reconnection X
line, J. Geophys. Res., 107(A10), p.SMP 26, 2002. (DOI:
10.1029/2002JA009381). This paper unifies the antiparallel and component
descriptions of reconnection, and is concerned mainly with macroscopic
distribution issues. It shows that reconnection extends well away from
the sites of antiparallel reconnection along X lines that traverse the
global dayside magnetopause.

Moore, T.E., M.O. Chandler, M.-C. Fok, B.L. Giles, D.C. Delcourt, J.L.
Horwitz, C.J. Pollock, Ring Currents and Internal Plasma Sources, Space
Science Reviews, 95(1-2): 555-568, January 2001. This is a Space Science
Reviews "challenge" paper arguing that strong ring currents such as we
have in the terrestrial magnetosphere can only occur where there are
substantial internal sources of plasma.

Moore, T. E., B. L. Giles, D. C. Delcourt, and M.-C. Fok, The plasma
sheet source groove, J. Atmos. Solar Terr. Phys., 62(6), p.505, 2000.
This is our study of polar wind trajectory reversibility showing that
ionospheric outflows can never be identified as a source of the plasma
sheet by backward trajectory tracing from the plasma sheet (and also
that the plasma sheet should be intrinsically unstable owing to velocity
space structuring.

Moore, T.E., R. Lundin, et al., Plasma source processes in the high
latitude ionosphere, IN "Sources and Losses of Magnetospheric Plasmas",
ed. by B. Hultqvist, G. Paschmann, and M. Øeroset, Kluwer, Dordrecht,
1999. This is our review chapter on ionospheric outflows, which has been
widely cited, though insufficiently taken to heart by the global
simulation community, to date.

Moore, T.E., et al., Heliosphere-Geosphere Interactions Using Low Energy
Neutral Atoms, Space Science Reviews, Special Issue, in press, 2003.
This paper makes use of modeling results from this study in support of
the interpretation of low energy neutral atom images of the Earth.

Perez, J. D., M.-C. Fok, and T. E. Moore, Deconvolution of energetic
neutral atom images of the Earth\'s magnetosphere, Space Sci. Revs.,
91(1-2), p.421, 2000. This paper is part of the IMAGE mission handbook
issue of SSR. Deconvolution methods were tested against our ring current
simulations in anticipation of the real IMAGE data set.

Strangeway, R. J., C. T. Russell, C. W. Carlson, J. P. McFadden, R. E.
Ergun, M. Temerin, D. M. Klumpar, W. K. Peterson, T. E. Moore, Cusp
Field-Aligned Currents and Ion Outflows, J. Geophys. Res. 105(A9),
p.21129, 2000. This paper initiated the study of local ionospheric
outflow response to local magnetospheric and solar wind energy inputs.

# Appendix 6: STATEMENTS OF COMMITMENT