Particle acceleration processes on auroral field lines during major geomagnetic storms
C. Cattell, P.I.
Table of Contents
1. Scientific/Technical Management Section
pg. 2
2. References
pg. 17
3. Summary of Personnel and Work Efforts
pg. 23
4. Facilities and Equipment
pg. 24
5. Budget Justification
pg. 25
6. Biographical Sketches
pg. 26
7. Co-I and/or Collaborator Commitments
pg. 30
8. Current and Pending Support
pg. 33
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1. Scientific/Technical/Management Section
A. Objectives and significance to NASA’s strategic goals
Major geomagnetic storms affect the magnetosphere of the earth dramatically in a
number of ways. These include intensification of the radiation belts, ionospheric heating and
latitudinally extensive, extremely intense aurora, causing significant energy dissipation (Baker et
al., 2001). Additionally, in the largest storms, magnetospheric activity becomes directly driven
by the solar wind (e.g. Siscoe et al., 2002; Lopez et al., 2004) resulting in magnetospheric
conditions that are significantly different than at other times. Understanding of the various
processes occurring during such events is important for several reasons. First, these events result
in acceleration of high energy particles which are a hazard to instruments and humans in space.
Secondly, this alternate state of the magnetosphere is effectively an additional laboratory,
complete with a good number of existing instruments, for the study of natural plasma processes
in space. And third, such storms are the most extreme examples of space weather that affect
near-earth space resulting in substantial energy transfer from the sun to the earth. Although most
studies of major storms have focused on the ring current and radiation belts, one of the first
storm phenomenon to be observed was the ‘great red aurora.’ Acceleration processes associated
with auroral and cusp field lines have, therefore, also received attention. There are a number of
electron features that have been identified, including stable auroral red (SAR) arcs and low
latitude broadband electrons (which may produce great red aurora). Several recent studies have
examined the strong outflow of ionospheric ions (Moore et al., 1999; Strangeway et al., 2000)
that occurs near the polar cap boundary on the dayside. With the notable exception of studies of
ionospheric sources of ring current particles (Daglis et al., 1993; McFadden et al., 2003),
however, the role of particle acceleration on auroral field lines in the dynamics and evolution of
major geomagnetic storms (‘superstorms’) has been largely unexplored. Recent studies of the
largest storms have suggested that ionospheric particles and acceleration processes may play an
important and here-to-for unrecognized role in storm dynamics (Kozyra et al., 2004b). There is
evidence for strong coupling between ionospheric particles, auroral acceleration, the ring current,
radiation belts and the atmosphere. Our primary science goal is to determine the mechanisms
that energize electrons and ions on low latitude auroral field line during major storms and to
establish their role in the dynamics and evolution of major storms, including energy deposition.
The extension of FAST data acquisition to low latitudes, in conjunction with Polar and Cluster
observations of particles and MHD waves on these field lines at higher altitudes and
geosynchronous observations of possible source regions, provide a unique opportunity to obtain
closure on these questions.
One particular phenomenon associated with these major storms is low-latitude broadband
electron signatures with sufficient energy flux to produce visible aurora. Shiokawa et al. (1996;
1997) first reported such signatures using DMSP data, conjecturing that they may be the cause of
red aurora observed at mid-latitude ground stations. Similar electron events have also been
observed by the FAST satellite (Dombeck 2005; Dombeck et al., 2005b; Nakajima et al., 2005).
The electron signatures in these events are distinct from both SAR arc events (e.g. Kozyra et al.,
1993; Shiokawa et al., 2001) and diffuse auroral electrons (e.g. Chen et al. 2005b), which are
also observed during storms. SAR arc electron events result from energy transfer from ring
current ions to cold electrons and have an upper energy limit of ~100 eV (Kozyra et al., 1997),
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while diffuse auroral electrons result from plasma sheet electrons convecting to lower L-shell
during a storm and have an energy spectra which is peaked around a few keV. The low-latitude
broadband electron events, by contrast, generally have a non-peaked energy spectra ranging up
to several keV. The acceleration mechanism for these intense, low-latitude broadband electrons
observed during major storms has not yet been determined. There are, however, similarities
between the signatures of these events and those of broadband electrons near the polar cap
boundary which are accelerated by Alfvén waves on the plasma sheet boundary layer (PSBL)
(e.g. Chaston et al., 2002; Dombeck et al., 2005a ). One goal of the proposed study is to
understand the acceleration mechanism for low-latitude broadband electron events observed
during major storms and the differences and similarities to broadband electrons seen during
other geomagnetic conditions.
Although most storm research has focused on electrons, including those that produce
SAR arcs and great red aurora, there are unusual signatures in the ions that are often seen
coincident with these electron signatures. An example of these new discoveries is the banded
ions with energies from 10s to 1000s of eV, which are observed during many superstorms,
including the “Halloween” 2003 storms (Cattell et al., 2004b; Thomsen et al., 2004). Although
energy banded ions in the auroral zone have been previously reported (Hirahara et al., 1997;
Boehm et al., 1999), the observations during the Halloween storms last much longer (more than
12 hours), have more bands, the O+ and H+ bands are at the same energies, the bands are seen
on the both the dayside and nightside, and band structure is more complex. They are also
extensive in latitude (~50º-75º on the dayside). These bands are new phenomenon associated
with all superstorms and possibly many storms and are not readily interpreted using previous
models. The banded ions are associated with but occur equatorward of intense ion outflow on the
dayside and equatorward of the region of discrete aurora on both the day and night sides. The
distributions are peaked in the perpendicular direction (locally mirroring). At the same time, long
lasting intervals of field-aligned energy dispersed ions from ~100 eV to 40 keV are seen in the
LANL geosynchronous satellites, primarily on the dayside and after magnetosheath encounters
(i.e. highly compressed magnetosphere). Although the geosynchronous ions have energy
dispersion consistent with time-of-flight, the FAST bands only show such dispersion within an
individual band and not across bands or latitude. The second goal of the proposed work is to
determine the source population, acceleration mechanisms and ultimate fate of the banded ions.
At this time, we can only speculate about the role of banded ions in superstorms. They
may provide an important energy source for extreme SAR arcs and great red aurora. They occur
coincident with the MLAT extent of the electron temperature peak on the dawnside and thus may
provide an additional heat source for plasmaspheric electrons by Coulomb collisions (Kozyra et
al., 2004b). The banded ions are also often seen in the same regions as the broadband electrons.
The source of the banded ions has not yet been identified. An ionospheric source may be
indicated by the association with intense ion outflow on the dayside; a boundary layer or
ionospheric source may be indicated by the association of the geosynchronous injections with
magnetospheric compressions (Thompsen et al., 2004); or they may be related to the usual
dawnside ring current source. Recent Cluster observations when Cluster was within ~30º of the
equatorial plane at ~4 RE during the Halloween storms (Engebretson et al., 2005) showed Pc1
and 2 waves, which are the frequencies to interact strongly with these ions. During one interval,
there was a power minimum at the O+ cyclotron frequency. The final goal of our proposed
research is to understand whether there is any relationship between the electron and ion
acceleration processes, the role of the banded ions in SAR and great red aurora, and the role of
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acceleration and loss processes on low latitude auroral field lines in storm dynamics and
evolution.
One of the strategic goals of NASA and its Science Mission Directorate and part of the
particular focus of the Heliophysics Research Program is to understand how solar activity affects
the space environment of the earth (goal 3B). Since the most intense and direct coupling of solar
activity to the near earth environment occurs during major geomagnetic storms, and particle
energization is both a means by which solar wind energy is ultimately transferred to earth and
constitutes a change to the environment itself, understanding these energization processes is
necessary for achieving NASA’s goals.
Our proposal describes a research program designed to examine particle acceleration on
low latitude auroral field lines. The primary goals are to: (1) understand the acceleration (as well
as transport and loss) of low latitude broadband electrons observed during major storms and the
differences and similarities to broadband electrons seen during other geomagnetic conditions; (2)
determine the source population, acceleration mechanisms and ultimate fate of the banded ions;
and (3) understand whether there is any relationship between the electron and ion acceleration
processes, the role of the banded ions in SAR arcs and great red aurora, and the role of
acceleration on low latitude auroral field lines in storm dynamics and evolution. The specific
science questions and approach to answering these questions will be detailed in Section C.
The University of Minnesota and the proposed project team are ideally suited to conduct
the study of these important, and not yet well studied, magnetic storm processes. In addition to
having successfully completed studies using similar techniques on FAST particle data (Cattell et
al., 2003, 2004a, 2006), the team has done preliminary and published studies, advancing the
understanding of the likely closely related process of PSBL broadband electron/Alfven wave
events and low latitude events (Dombeck 2005; Dombeck et al., 2005a, 2005b, 2006). The
University of Minnesota also has the computer expertise, computing tools, and data available in
house to efficiently conduct the proposed project. All of the FAST electron CDF files as well as
all Polar full resolution data are stored online at the University of Minnesota. All FAST, Polar
and Cluster full resolution data is also available online or on CD at the University, while
necessary ACE, Wind and geomagnetic index data are readily available online through webservices for which automated access routines already exist at the University. In addition, the PI
has ongoing grants of time on the supercomputers of the Minnesota Supercomputer Institute that
will be used for particle tracing codes. The PI of the proposed project is a Co-I on FAST, and the
Polar and Cluster electric field instruments. Note that she does not receive project funding for
Polar or Cluster studies and that her FAST funds are currently for TIMED/FAST comparisons.
The group has ongoing collaborations with the Polar particle teams and the Cluster magnetic
field and particle teams, and software installed and running to provide analysis of full resolution
Polar particle data, Cluster magnetic and particle data. Collaborator Dr. M. Thomsen has
expertise in the analysis of the LANL geosynchronous data and has worked with the PI on
preliminary studies of banded ions. Collaborator Dr. J. Kozyra has expertise in theory and data
analysis on SAR arcs, great red aurora, superstorms and coupling processes.
B. Impact of proposed work and relevance to NASA goals
Our research addresses NASA’s strategic goal, 3B, “Understand the Sun and its effects
on Earth and the solar system.” Specifically, as called out in 3B.1, we will provide “progress in
understanding the fundamental physical processes of the space environment…” that will
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ultimately allow the development of a predictive capability. We will provide science results to
address several research focus areas from the 2005 Roadmap, including F2- “ Understand the
plasma processes that accelerate and transport particles and F3 -“Understand the role of plasma
and neutral interactions in nonlinear coupling of regions throughout the solar system”, as well as
H2 - “Determine how changes in the Earth’s magnetosphere, ionosphere, and upper atmosphere
change in order to enable specification, prediction, and mitigation of their effects.”
Our proposed work contributes directly to the goal of the Heliophysics Guest Investigator
program to fully utilize the data sets from operational missions to meet NASA strategic goals. In
particular, the proposed study is a data analysis and interpretation science project that uses data,
from various spacecraft of the Geospace Mission, in particular FAST, with additional analysis of
data from Polar and Cluster. ACE and WIND data will be used to specify the solar wind drivers.
C. Technical Approach and Methodology
While a few major storm related low-latitude broadband electron events (Shiokawa 1996,
1997; Dombeck et al., 2005a,b; Nakajima et al., 2005) and banded ion events (Cattell et al.,
2004b; Thomsen et al., 2004) have been reported on a case study basis, they have not yet been
studied as classes of events. Neither process is yet understood, either observationally or
theoretically. FAST is particularly well suited, in orbit, mission duration and instrumentation, for
its data to play the primary role in a comprehensive study of these events. Its ten year mission
duration to date covers nearly an entire solar cycle allowing observation of a statistically
significant number of major storms, >20, and its 133 minute, highly elliptical, polar orbit and
extremely fast data rate for both particles and fields provides the temporal and spatial coverage at
high resolution necessary to investigate these rare events. Further, FAST data has already been
utilized for preliminary results on case studies of these and similar events (Cattell et al., 2004b;
Dombeck 2005; Dombeck et al., 2005a,b; Nakajima et al., 2005). Combining FAST data with
data from the Polar, Cluster, and LANL geosynchronous satellites, with Wind and ACE
providing solar wind monitoring, will allow for a comprehensive understanding of these
phenomena and their role in sun-earth coupling during major storms.
The complete methodology for our study is detailed below, but a brief overview is as
follows: The first stage of the study will be to study a small statistical sample of both broadband
electron and banded ion events (~10) for detailed initial analysis for use in providing preliminary
results, determining the viability of the various acceleration mechanisms, and developing
automated identification algorithms. These algorithms will then be used to compile a database of
events from the entire FAST mission, which will include the relevant characteristics of each
event from the FAST data, plus the relevant conditions of the solar wind and magnetosphere
from WIND, ACE, Polar and Cluster data and global indices such as Dst, AE and Kp. This
database will be used to determine characteristics and correlations for events and conditions, for
comparison to the various theoretical generation mechanism and to provide constraints/input
parameters to related simulations. Finally, detailed analysis of both the FAST data and related
Polar, Cluster and LANL data will be used to refine and further test understanding of these
processes and their role in storm dynamics and evolution.
Low-latitude downgoing broadband electrons during major storms were first reported by
Shiokawa et al. (1996; 1997) using DMSP data. These broadband electron signatures were
significantly different than those associated with diffuse, inverted-V and SAR arc aurora, having
a very broad energy range, from ~30 eV to 30 keV and sharply defined latitudinal extents.
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Preliminary FAST results, shown in Figure 1
which plots the downward energy spectra for
a variety of cases, indicate that events that
can be described as low-latitude broadband
electrons during major storms are observed at
many different local times and have a variety
of signatures. These include intense,
latitudinally limited events, events that extend
throughout much of the auroral zone, events
that have maximum energies below 1 keV,
ones with energies up to 10 keV, isolated
broadband populations and ones that are
concurrent with inverted-V, diffuse or SAR
arc auroral populations. Further, clear cut
differences in properties to classify these
various signatures into “types” are not readily
apparent. Therefore, these events may be the
result of a single mechanism operating under
different conditions or a variety of different
mechanisms, possibly occurring
simultaneously, that result in similar electron
signatures. Preliminary FAST analysis does
provide some insight in that the basic
properties of many of the low-latitude
broadband electron events are similar to
broadband electron events more commonly
observed on field lines mapping to the PSBL.
Also, low-latitude broadband electron events
have been observed to occur on similar field
lines and in storms that also contained banded
ions, although a complete correlative study of
these two phenomena has not yet been done.
Therefore these low-latitude broadband
electron events may be related to a process
similar to the PSBL events, i.e. Alfven waves
at higher altitude, a process related to the
banded ions or to some other process. The
proposed study will investigate these
possibilities. The low-latitude broadband
electrons are also sometimes observed
concurrently and on the same field lines as
SAR arc electron populations. The
broadband signatures are distinct from the
SAR arc ones, having higher energy
components and sharp latitudinal extents.
These population distinctions and the fact
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Figure 1. Sample downward electron energy spectra
from FAST passes through the auroral zone showing
a variety of examples of low latitude broadband
electron events during major geomagnetic storms.
Note that the bottom three passes are equator to pole
while the others are pole to equator.
that broadband events are observed at times without SAR arc populations indicate that these two
processes are likely unrelated. This conjecture will be specifically tested as a part of the
proposed study, with the assistance of Collaborator Dr. J. Kozyra.
Broadband electron events on PSBL field lines, which are observed both during major
storms and during substorms, have been more extensively studied than the low-latitude variety
and are observed coincident with small scale Alfven waves at FAST. They are consistent with
being powered by Alfven waves on the PSBL observed at 4-9 RE (Wygant et al., 2000,2002a;
Chaston et al., 2002, 2003). This theory is supported by various simulations (e.g. Chaston et al.,
2002; Su et al., 2004; Chen et al., 2005a) which indicate that Alfven waves at 4-9 RE result in a
broadband electron spectra at FAST altitudes, and has recently been confirmed by a study of a
simultaneous Polar and FAST PSBL crossing (Dombeck et al., 2005a). Similar findings have
also been reported on dayside cusp field lines (Chaston et al. 2005). Figure 2 (Dombeck et al.,
2005b) shows data from a FAST pass during the recovery phase of a major storm on 21 October
1999 with both PSBL and low-latitude broadband electron events. Panel a and b are the electron
energy and pitch angle spectra, while panels c and d show the earthward directed Poynting flux
and dE/dB ratio in two different frequency bands, red (blue) 10 to 100 mHz (1 to 4 Hz). dE/dB
ratios are only plotted for times of significant Poynting flux (>0.04 ergs cm-2s-1 when mapped to
the ionosphere). Intense
broadband electrons can be
observed at ‘B’, on PSBL
field lines, and at low
latitude (~60º ILat), e.g. ‘A’,
with less intense broadband
signatures at intermediate
latitudes. The dE/dB ratios
indicate that the lower
frequency Poynting flux
(red) is consistent with quasistatic structures coupling to
the ionosphere through
Pederson currents, while the
high frequency Poynting flux
(blue) is Alfvénic in nature.
The broadband electrons at
both ‘A’ and ‘B’, along with
some of those observed at
mid-latitude, occur
coincident with small scale
(high frequency) Alfvénic
activity. Panels d and e show
electron energy flux
Figure 2. A sample FAST pass during a major storm showing both
distributions at ‘A’ and ‘B’
low latitude (A) and PSBL (B) broadband electron signatures.
respectively. Such
Panels a and b plot the electron energy and pitch angle spectra,
similarities between the lowwhile panels c and d plots Alfvénic Poynting flux and dE/dB ratio
for two different frequency bands. Panels e and f are sample
latitude and PSBL broadband
electron energy flux distributions for the broadband electron events.
electron observations
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indicate that the two processes may be similar. Further support to this conjecture is provided by
preliminary analysis (Dombeck 2005; Dombeck et al., 2005b) which indicates that during at least
one major storm Polar likely observed intense earthward Alfvénic Poynting flux at ~6 RE
concurrent with a low-latitude broadband electron event observed by the DMSP F14 satellite.
To understand these low-latitude broadband electron events observed during major
storms and their role in the solar wind/magnetosphere coupling, several specific science
questions will be addressed. 1) What are the characteristics of these events and are there distinct
‘types’? 2) How are these events related to/controlled by solar wind drivers and magnetospheric
conditions? 3) Are these events caused by the same mechanism as the PSBL events, how do the
low-latitude Alfven waves differ from those on the PSBL and how do they relate to major
storms? 4) Are additional mechanisms required to account for all of the observed events, and if
so what are those mechanisms? The proposed research project will address these questions in
several steps, utilizing in situ particle and fields data from FAST, Cluster and Polar.
The first step will be to choose ~10 FAST events which include ones with and without
concurrent SAR arc populations and banded ions (if possible) from varying phases of major
storms. These events will be used for detailed initial analysis, including particle distribution and
Alfven wave analysis, as well as relationship to solar wind and magnetospheric conditions. This
study will provide detailed initial investigation of the physics of these events addressing all four
science questions and will facilitate development of an automated event identification algorithm.
This algorithm development will combine the expertise developed in the previous University of
Minnesota database studies with newer data mining techniques (e.g. Karimabadi et al., 2006) to
produce a robust, efficient algorithm for the identification and classification of these events with
their widely varying signatures. Particular attention will be given in this first stage to providing
preliminary answers to questions 3 and 4 by conducting detailed analysis of the event particle
distributions and comparing them and Alfven wave characteristics to those of FAST events on
PSBL field lines. The methodology for Alfven wave analysis has been described in Dombeck
(2005) and Dombeck et al. (2005a, 2006).
The second step will be to use the identification algorithm on the entire FAST data set as
was done in the University of Minnesota FAST electron beam study (Cattell et al., 2004a; 2006)
to create an event database, to provide definitive answers to science questions 1 and 2 on a
statistical level and a sufficient empirical context to understand the physics of questions 2, 3 and
4. The entire FAST dataset will be used rather than just concentrating on major storms since part
of the proposed study is to determine how the events are related to solar wind/magnetospheric
conditions and storms. For each event, the database will store the characteristics of the event,
e.g. characterization of the electron distribution and moments and their variability during the
event, event spatial and temporal extent and location, along with FAST field data for Alfven
wave summary analysis, as has been done for PSBL events (Dombeck et al., 2005a, 2006), and
various characteristics of the solar wind and magnetospheric conditions surrounding the time of
the event, e.g. solar wind velocity, dynamic pressure and composition, IMF magnitude, direction
and variability, magnetospheric composition, and AE, Dst indices. These latter solar wind and
magnetospheric conditions and characteristic will be obtained ACE, Wind, Polar, Cluster data,
when available, from the CDAWeb and the World Data Center for Geomagnetism, Kyoto.
These data will be obtained through automated download routines similar to those used for
previous University of Minnesota correlative studies (Cattell et al., 2004a; Dombeck et al.,
2006). Before running the automated database routines on the entire FAST dataset, it will be
8
tested on a few month’s worth of data when several major storms occurred to tune the automated
algorithms and provide preliminary results.
The third step of the investigation of low-latitude broadband electron events will be to
investigate the properties of the plasma sheet mapping to the regions of these events during the
times that these events are observed. This region generally corresponds to the plasma sheet
between 3 and 6 RE to provide definitive answers to science questions 3 and 4. Wygant et al
(2001, 2002b) have presented a number of cases of strong Alfvénic waves deep within the
plasma sheet during major storms. Further study of this region and events of this type will
clarify the role of Alfvénic acceleration in these events. The analysis in this stage of the study
will utilize Polar, Cluster, and to a lesser extent LANL geosynchronous satellite data, and will
incorporate two methods of analysis. The first method will search for conjunctions between
Polar or Cluster and FAST during FAST observations of low-latitude broadband electrons.
Similar analysis has been done for the PSBL and cusp broadband electron events (Dombeck et
al., 2005a; Chaston et al., 2005). LANL geosynchronous satellites conjunctions will be
somewhat common but their lack of field measurements will limit the utility of such
conjunctions, particularly if the energy at these higher altitudes is primarily in waves, as in the
case of Alfven waves. Without knowing the occurrence frequency of the low-latitude broadband
electron events, it is difficult to estimate the likely number of Polar or Cluster and FAST
conjunctions. However, a rough estimate can be determined from visual data inspection that
indicates that there are generally ~10 to 15 orbits per major storm with prominent events. Polar’s
~18 hour orbit means that it should be latitudinally conjunct with FAST during one or two of
those orbits per storm. Polar has been operational for the duration of the FAST mission.
However, the latitudinal precession of Polar’s perigee means that is would be conjunct in the ~3
to 6 RE mapping altitude only perhaps 10% of the time, leading to an expectation of ~2 to 4
conjunction events. Cluster, having only been available for roughly half of the FAST mission
duration, having a ~54 hour orbit, but passing through the ecliptic at ~4 RE each orbit of it
mission also has an expectation of ~2 to 4 conjunctions. The challenge during such Polar and
Cluster orbits will be to determine accurate mapping since active storm times require
topographical mapping, and the low-latitude broadband electron events map to the central
plasma sheet which does not easily facilitate such mapping. However, indirect arguments can be
made for mapping of such events, as has been done for the preliminary analysis of the
Polar/DMSP F14 low-latitude broadband electron event (Dombeck 2005; Dombeck et al.,
2005b). These conjunction studies will provide confirmation and allow investigation of the
details of the electron acceleration mechanism(s) and the energy transfer process.
The second method of investigating the region of the plasma sheet mapping to the lowlatitude broadband electron events that will be utilized in the proposed study will be to use the
conditions during which such events occur to determined stage 2 of the study and then
investigate the Polar and Cluster passes through regions that would map to such events when
FAST is not in direct conjunction. When available DMSP satellite data will be used to confirm
that low-latitude broadband electron events do occur during these Polar and Cluster passes. This
method of study will provide enough samples of plasma sheet conditions for statistical
understanding of the region during the events. Combining the results of this method of study
with the direct conjunction events will provide sufficient data for confirmation of the accuracy of
understanding of the electron acceleration mechanism(s) responsible for these events and their
coupling to major storm processes.
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These three steps of analysis will facilitate the answering of all four specific science
questions in regard to the low-latitude broadband electron events during major storms. In
addition to providing characterization of the events and their ‘types’, determining how these
events relate to the PSBL and cusp broadband electron and Alfven wave events, and
investigating how these events are related to major storm conditions and sun-earth energy
transfer, questions 1, 3 and 2 respectively, these steps will also answer whether and how these
events are related to other processes, question 4, such as banded ions and SAR arcs or here-to-for
unknown processes.
Banded ions have previously been reported on auroral field lines at low altitudes (FAST,
DMSP and DE-2), intermediate altitudes (DE-1, Akebono) and at high altitudes (Polar). In the
low altitude auroral zone, energy dispersed discrete bands, which lasted for a few hours and had
equal O+ and H+ velocities, were reported during quiet times. Two interpretations for the
observed structures were proposed: (1) convective drift dispersion from an ionospheric heating
source (Hirahara et al., 1997); and time-of-flight dispersion from equatorial acceleration event
(Boehm et al., 1999). Both models predict that O+ and H+ ions will have the same velocity,
energy bands have ratios dependent on latitude (field line length) and that energy increases with
latitude. The equatorial source model assumes an impulsive acceleration process that is broad in
latitude, as described by Mauk (1986). The observed energy dispersion with latitude depends on
the length of the field line squared and results in bands with ratios of .25, .75, 1.25, etc. In the
ionospheric acceleration model, the latitude dispersion depends on the ExB drift and results in
bands with ratios of 1,2,3 … or 1.5, 2.5, 3.5, etc.. Boehm et al. (1999) concluded that both their
observations and those of Hirahara et al. were most consistent with the equatorial acceleration
mechanism.
Using DE data ( at low and mid-altitudes), Frahm et al. (1986) and Winningham et al.
(1984) described energy dispersed ion bands, within the region of diffuse aurora, from few eV to
a few keV and peaked at a pitch angle of 0º. In contrast to the Boehm et al. and Hirahara et al.
observations, these occurred primarily during the main phase of storms. Similar to Hirahara et
al., the bands were interpreted as being the result of convective dispersion from an ionospheric,
auroral source.
At higher altitudes, Polar observations of multiple energy dispersed bands (~1-100s of
keV) were reported by Fennell et al. (1998) and Peterson et al. (1998). These events had O+ and
H+ at same energy, and were weakly peaked at 90º pitch angle. They extended from L~3-8, were
most often seen from ~6-18 MLT, and in quiet times following substorms. Three different
explanations have been proposed: (1) convection of time variable discrete ion sources in the
plasma sheet (Peterson et al., 1998); (2) time-of-flight following prompt energization in an
electric field pulse associated with substorm dipolarization with bands depend on ion grad B
drift time (Li et al., 2000); and (3) time-varying ExB convection of a tail source population for
energies >~1keV and an ionospheric source for energies <~1keV (Fennell et al., 1998). A recent
particle tracing simulation (Ebihara et al., 2003) concluded that the Fennell et al. mechanism was
most likely with the bands being a result of enhanced convection (during the substorm) followed
by reduced convection.
Note that are other band-like features that have been observed and modeled, including
the ion ‘gaps’ (see, for example, Kovrazkhin et al., 1999), ‘wedge’-type dispersion (Ebihara et
al., 2001) and velocity-dispersed ions at the plasma sheet boundary (Ashour-Abdalla et al.,
1992,2005; Bosqued et al., 1993). McFadden et al. (2001) described low energy FAST
observations of ring current injections and low energy ring current dawn-dusk asymmetry.
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Figure 3. Six dayside (MLT ~8 to 11) auroral passes on 10/31/03 from 01:54-13:06 UT. The left hand
panels are ions with downgoing pitch angles, the middle panel plots perpendicular pitch angles and the
right panels are the upgoing ions.
These have all been sometimes observed during the events with ion banding, but are very
different phenomena and will not be discussed further.
The ion bands that have been observed during superstorms by FAST (Cattell et al.,
2004b; Thomsen et al., 2004) are distinctly different from the ion bands reported previously and
described above. The ion bands often last for periods greater than 10 hours, have more bands
than previously seen, have equal O+ and H+ energies, and energy-latitude dispersion
characteristics that depend on local time and are sometimes very complex. They are a new
phenomenon associated with all superstorms and many storms, and they are not readily
explained using previous models.
An example from the superstorm of Halloween 2003 is shown in Figure 3, which plots
the dayside (MLT of ~8 to 11) auroral passes on 10/31/03 from 01:54-13:06 UT. The left hand
panels are ions with downgoing pitch angles, the middle panels plot perpendicular pitch angles
and the right panels are the upgoing ions. For more than 12 hours on the dayside, FAST observed
H+ and O+ bands at discrete energies from ~30 eV to ~10 keV, over a wide range of latitudes
from ~50º-75º (more commonly 56º-72º). The ion fluxes peak near 90º, with almost no upgoing
ions, consistent with mirroring close to the satellite altitude. Although the relative flux varies
from peak to peak, the O+ and H+ bands are at same energy; therefore, the banding can not be
time-of-flight, velocity dispersion from a common source, as proposed by Boehm et al. for their
quiet time banding events. In addition, there is very little energy dispersion with latitude. There
is no evidence for the energy band ratios predicted by either mechanism discussed by Boehm et
al. During some orbits, there is evidence for modification of the band energy, possibly due to
local potential drops. Time-of-flight dispersion is visible in the distribution functions within an
individual energy band, i.e. the relation between the pitch angles and the energy of particles
within a given band. Note that FAST observed very intense ion outflow (of both H+ and O+),
11
Figure 4. The same six passes as Fig. 3 with perpendicular ions (left) and downgoing electrons (right).
peaking at >1010 ions/cm2 s throughout this interval.
The association between downgoing electrons and
the banded ions is shown in Figure 4, which plots
the perpendicular ions (left side) and downgoing
electrons (right side) for the same passes as Figure
3. The banded ions are observed primarily
equatorward of the main auroral zone, although in
some passes (see top two passes), they extend to
latitudes where the injected cusp ions are observed.
The perpendicular ion heating and ion outflow occur
in the cusp and auroral zone in association with both
‘inverted-V’ and broadband electron acceleration
associated with the cusp and PSBL.
The banding seen on the nightside is often
more complex and intermittent than on the dayside,
as can be seen in Figure 5, which plots the
perpendicular ions for six adjacent auroral passes
during the Halloween storm. In contrast to the
dayside, there is often energy dispersion with
latitude (higher energies at higher latitudes-see 2nd
panel from the top) and the ion bands only rarely
occur at latitudes above ~65º. However, as on the
dayside, the bands are equatorward of the primary
auroral electron acceleration (not shown). When
12
Figure 5. Perpendicular ions from six
nightside auroral passes on 10/31/03 14:55
- 11/1/2003 02:30.
considering mechanisms to produce the
bands, the relevant timescales must be
examined. For L~6-10, only ions with
E>~1.5 keV will see the effect of grad
B drift. For lower energies, co-rotation
dominates. The drift times are long.
Bounce periods are also long compared
to the duration of a FAST pass, ~50
minutes for a 100 eV proton at L=10
and ~20 minutes for 1 keV O+.
During the Halloween storm
interval, the LANL geosynchronous
satellites observed broad regions of
energy dispersed field-aligned ions
from ~100 eV to 40 keV. Examples are
shown in Figure 6, which plots a 1 hour
interval including the time of the first
FAST pass in Figure 4. The ions
occurred primarily on the dayside and
Figure 6. Data from one LANL satellite at the time of the
often in association with
first FAST pass in Figure 4 showing the field-aligned
magnetospheric compressions.
dispersed ions going north and south.
Although most of the ion bursts fit a
time-of-flight dispersion; in some
cases, it was for an ionospheric source and, in some, for an equatorial source, with multiple
source injection times (Thomsen et al., 2004). Note that, for some bursts, multiple bounces are
required to fit the dispersion, but not all the intermediate bounces are observed. Comparison
between the energy spectra observed at geosynchronous and simultaneously at the same L value
at FAST was not definitive for the few cases done. Note that strong PC5 modulation was
observed in the LANL data during part of these events and the possible role of these waves will
be examined.
The preliminary comparison of the FAST banded ions and the geosynchronous data
during the Halloween storm raised more questions than it answered about the mechanism
producing the banded ions. There is evidence in the FAST data and the LANL data for an
ionospheric source, as well as for a plasma sheet source. The LANL data shows clear evidence
for an equatorial dayside source associated with magnetospheric compressions, likely the
boundary layer. The equatorial source observations are consistent with Mauk (1986) and Quinn
and McIlwain (1979), as well as with the source characteristics inferred by Boehm et al..
Although the LANL data are consistent with time-of-flight dispersion, the FAST data do not
appear to be, since the O+ and H+ bands have the same energies (not velocities).
More detailed analysis of both data sets, and the addition of other observations at higher
altitudes, is needed address our science goal to: determine the source population, acceleration
mechanisms and ultimate fate of the banded ions. The first step is to fully characterize the
banded ions. As discussed above, initially a set of events will be studied in detail to provide
examples for algorithm development. Among the properties that must be determined are the
energy and flux of the bands vs. latitude, and the ratio of the O+/H+ energy and flux for each
13
band. This will allow us to determine whether the same bands persist for many orbits and
whether there are consistent ratios between the energies of adjacent bands.
For a subset of events, the LANL geosynchronous data will be examined, as was done for
some intervals during the Halloween storm, to determine whether there are energy dispersed ions
and, if so, what source locations and injection mechanisms are consistent with them. In addition
to examining the LANL data which are available continuously, we will also identify storm
periods with banded ions for which either Polar or Cluster was on the same L-shells as FAST.
These data sets afford a complementary view of the high altitude processes and, in addition,
provide diagnostics on low frequency waves that can interact with the ions (Hudson et al, 1995),
and on the convection electric field and its variability. For example, recent Cluster observations
when Cluster was within ~30º of the equatorial plane at ~4 RE during the Halloween storms
(Engebretson et al., 2005) showed Pc1 and 2 waves, which are the frequencies to interact
strongly with these ions. During one interval, there was a power minimum at the O+ cyclotron
frequency. The reported ion banding observed on Polar is more consistent with the FAST
observations at low altitudes that other banded observations, so we anticipate that conjunctive
studies with Polar will yield useful constraints on source, acceleration and loss mechanisms.
Using the characteristics determined from the low altitude (FAST) and high altitude
(LANL, Polar and Cluster) data, we can test possible mechanisms for producing the ion bands
using a particle tracing code that we have implemented at the Minnesota Supercomputer Institute
(Cattell et al., 1995; Streed et al., 2000a,b). This code allows us to trace the motion of H+ and
O+ ions in a dipole magnetic field or any of the Tsygenenko model fields. In addition, we can
specify wave electric and magnetic fields and the convection electric field. The detailed
specification of the properties of the banded ions and their associations with high altitude
distributions and with magnetic activity, and the complementary high altitude particle data from
geosynchronous and Polar and Cluster and wave data from Polar and Cluster will result in a
detailed and complete observational picture of this phenomenon. The comparison to the results
of particle tracing codes, and to models presented for other banded ions, will allow us to
determine the source population, acceleration mechanisms and ultimate fate of the banded ions.
Figure 6 shows the relationship between storm phase (Dst in the bottom panel), banded
ions (red banded intervals) and broadband electrons (purple banded intervals) for one major
storm on Nov. 20-21, 2003. Banded ions and broadband electrons are both seen throughout the
storm for this event. It should be noted that this storm occurred after a long interval of major
activity and may not be typical of an isolated storm. Figure 4 provides an illustration of some
relationships that are observed. An electron signature (maximum energy ~70 eV) consistent with
an SAR arc can be seen at ~-61 in the second panel in association with intense banded ions. In
the third panel at ~-70, broadband electrons up to ~1keV occur with strong ion banding. The
final goal of our proposed work is to understand whether there is any relationship between the
electron and ion acceleration processes, the role of the banded ions in SAR and great red
aurora, and the role of acceleration and loss processes on low latitude auroral field lines in
storm dynamics and evolution.
We will examine a number of specific questions using the conclusions reached about
goals 1 and 2 and the detailed correlative databases to determine the role of these processes in
major storms. Here we discuss a few representative examples. (1) Are the banded ions an
important or contributing energy source for extreme SAR arcs/great red aurora? A hint that the
ions may be important in SAR arcs is that the intense ions are sometimes coincident with the
electron temperature peak on dawnside. They may provide an additional heat source for
14
plasmaspheric electrons by Coulomb collisions. (2) Do the ion bands represent a loss mechanism
for ring current ions? Are the ion bands related to large, penetrating variable electric fields seen
during superstorms? The relationship to storm phase and to observed injection into the ring
current will help answer this question, as will particle tracing including observed MHD waves.
(3) What is the energy input into the ionosphere via the broadband electrons and the banded
ions? How significant is it in the storm energy budget? (4) Is there evidence that the banded ions
interact with the Alfven waves that accelerate electrons?
D. Plan of Work and Management
The software required to access and analyze FAST, Polar and Cluster data is installed and
operating at the University of Minnesota, as are the routines to automatically access the public
web data services for WIND and ACE data and the geomagnetic indices. Alfvén wave analysis
programs are also available and have been used for previous studies using both Polar and FAST
data, and the University of Minnesota has experience converting its Polar analysis programs for
use with Cluster data. Other than development of the event identification algorithms that are
specific to the proposed project almost all of the software required for the proposed research,
including the particle tracing code, is already functional. Therefore the project team will be able
to devote most of their time to science questions.
Year 1: Sample events will be selected from the FAST data and analyzed in detail
including particle distributions, wave data and relations to storm, solar wind and magnetospheric
conditions to provide preliminary results, determine the viability of the various acceleration
mechanisms, and develop the automated identification algorithms. Initial comparisons to LANL,
Polar and Cluster data will be made for select events. The preliminary results from this phase of
the research including the viability of the various acceleration mechanisms and comparison with
PSBL and cusp Alfvén wave events will be presented. Later in the year, the existing database
creation software will be modified to incorporate the new identification algorithms and tested on
data spanning 3 months of active storms.
Year 2: The database software will be fine tuned and then run on the entire FAST
dataset. The initial science results from the first three months of data will also be presented at
this time. Once the database is complete, the results, including correlations with storms, solar
wind and magnetospheric conditions, will be presented, and Polar and Cluster conjunction events
with FAST will be identified for study. Test runs of the particle tracing code will be done for
comparison of ion bands and geosynchronous data.
Year 3: The Polar/Cluster conjunction events with FAST will be studied in detail along
with other Polar and Cluster passes through the region of interest, 3 to 6 RE, during times which
correspond to conditions for low-latitude broadband electron and ion banding events as
determined from the database phase of the project to confirm and refine understanding of the
acceleration mechanism(s) and the superstorm energy transfer processes. Final work on the
particle tracing code will be done to test source mechanisms, etc. for banded ions.
E. Personnel Responsibilities
The PI, Cynthia Cattell, will have overall responsibility for the management of the
proposed work and will coordinate the efforts of the research team. She will oversee the analysis
of the FAST ion data sets by the University of Minnesota graduate student and the FAST, Polar
15
and Cluster analysis by the postdoctoral researcher, John Dombeck. She will work on
interpretation of the banded ions and their roles in storms. She will lead the particle tracing
effort.
Co-Investigator, Dr. John Dombeck, will take the lead in analysis of the FAST electron
and fields data, in identifying Polar and Cluster intervals of interest and analysis of the Polar and
Cluster fields data sets for MHD waves.
Collaborator Dr. Michelle Thomsen will assist in the analysis of the LANL
geosynchronous data for comparison to models for sources of banded ions and comparison of the
geosynchronous plasma data to the broadband electrons. Collaborator Dr. Janet Kozyra will
provide assistance in the interpretation of multiple data sets and comparison to models and
simulations. She will also provide expertise in SAR arcs and great red aurora and superstorm
coupling.
All team members will participate in the interpretation of the science results and in their
presentation in the literature and at scientific meetings.
16
2. References
Ashour-Abdalla, M., L. M. Zelenyi, J. M. Bosqued, and R. A. Kovrazhkin (1992), Precipitation
of fast ion beams from the plasma sheet boundary layer, Geophys. Res. Lett., 19(6), 617–620.
Ashour-Abdalla, M., J. M. Bosqued, M. El-Alaoui, V. Peroomian, L. M. Zelenyi, R. J. Walker,
and J. Wright (2005), A stochastic sea: The source of plasma sheet boundary layer ion structures
observed by Cluster, J. Geophys. Res., 110, A12221, doi:10.1029/2005JA011183.
Baker, D. N., N. E. Turner, and T. I. Pulkkinen (2001), Energy transport and dissipation in the
magnetosphere during geomagnetic storms, J. Atmos. Sol.-Terr. Phys., 63, 421.
Boehm, M. et al. (1999), FAST observations of bouncing ion distributions: Fieldline length
measurements, J. Geophys. Res., 104, 2343.
Bosqued, J. M., M. Ashour-Abdalla, M. El Alaoui, V. Peroomian, L. M. Zelenyi, and C. P.
Escoubet (1993), Dispersed ion structures at the poleward edge of the auroral oval: Low-altitude
observations and numerical modeling, J. Geophys. Res., 98(A11), 19,181.
Cattell, C., M. Linton and I. Roth (1995), The effects of low frequency waves on ion trajectories
in the earth’s magnetotail, Geophys. Res. Lett., 22, 3445.
Cattell C., J. Dombeck, W. Peria, R. Strangeway, R. Elphic, and C. Carlson (2003), Fast Auroral
Snapshot observations of the dependence of dayside auroral field-aligned currents on solar wind
parameters and solar illumination, J. Geophys. Res., 108(A3), 1112, doi:10.1029/2001JA000321.
Cattell, C. J. Dombeck, W. Yusoff, C. Carlson and J. McFadden (2004a), FAST observations of
the solar illumination dependence of upflowing electron beams in the auroral zone, J. Geophys.
Res., 109, A02209, doi:10.1029/2003JA010075.
Cattell, C. A , M. F. Thomsen, Janet Kozyra, B. Lavraud, J. Borovsky, and J. Dombeck (2004b),
Energized Banded Ions During Large Geomagnetic Storms: Comparisons of Observations at
Geosynchronous and Low Altitudes, COSPAR04-A-02925.
Cattell, C., J. Dombeck, C. Carlson, and J. McFadden (2006), FAST observations of the solar
illumination dependence of downgoing auroral electron beams: Relationship to electron energy
flux, J. Geophys. Res., 111, A02201, doi:10.1029/2005JA011337.
Chaston, C. C., J. W. Bonnell, L. M. Peticolas, C. W. Carlson, and J. P. McFadden (2002),
Driven Alfven waves and electron acceleration: A FAST case study, Geophys. Res. Lett., 29,
1535, doi:10.1029/2001GL013842.
Chaston, C. C., J. W. Bonnell, C. W. Carlson, and J. P. McFadden (2003), Properties of smallscale Alfvén waves and accelerated electrons from FAST, J. Geophys. Res., 108, 8003,
doi:10.1029/2002JA009420.
17
Chaston C. C., et al. (2005), Energy deposition by Alfvén waves into the dayside auroral oval:
Cluster and FAST observations, J. Geophys. Res., 110, A02211, doi:10.1029/2004JA010483.
Chen, L.-J., C. A. Kletzing, S. Hu, and S. R. Bounds (2005a), Auroral electron dispersion below
inverted-V energies: Resonant deceleration and acceleration by Alfvén waves, J. Geophys. Res.,
110, doi:10.1029/2005JA011168.
Chen, M. W., Schulz, M., Lyons, L. R., and Gorney, D. J. (1993), Storm time transport of ring
current and radiation belt ions, J. Geophys. Res., 98, 3835.
Chen, M. W., M. Schultz, P. C. Anderson, G. Lu, G. Germany, and M. Wüest (2005b), Storm
time distributions of diffuse auroral electron energy and X-ray flux: Comparison of drift-loss
simulations with observations, J. Geophys. Res., 110, doi:10.1029/2004JA010725.
Daglis, I. A., E. T. Sarris, and B. Wilken (1993), AMPTE/CCE CHEM observations of the ion
populations at geosynchronous altitudes, Ann. Geophys.,11, 685.
Dombeck, J. P. (2005), Properties of Alfvén waves in the magnetotail below 9 RE and their
relation to auroral acceleration and major geomagnetic storms, Ph.D. Thesis, University of
Minnesota, Minneapolis, Minnesota.
Dombeck, J., C. Cattell, J. R. Wygant, A. Keiling, and J. Scudder (2005a), Alfvén waves and
Poynting flux observed simultaneously by Polar and FAST in the plasma sheet boundary layer, J.
Geophys. Res., 110, A12S90, doi:10.1029/2005JA011269.
Dombeck, J. P., C. Cattell, J. Wygant, A. Keiling, M. Thompsen, and J. Scudder (2005b), Intense
Alfven waves well within the plasma sheet during the main phase of the 21 October 1999 major
storm and comparison of major storm to non-storm substorm PSBL alfven waves, SA13B-05,
Fall AGU.
Dombeck, J., C. Cattell, and J. Wygant (2006) Alfvén wave properties in the PSBL during
substorms and major storms from frequency band analysis of Polar data, Ann. Geophys.,
manuscript in preparation.
Ebihara, Y., Yamauchi, M., Nilsson, H., Lundin, R., and Ejiri, M. (2001), Wedge-like dispersion
of subkeV ions: Particle simulation and Viking observation, J. Geophys. Res., 106, 29,571.
Ebihara, Y. et al. (2003), Multiple Discrete-Energy Ion Features in the Inner Magnetosphere:
Event of February 9,1998, Annales Geophys.
Engebretson M. J., T. G. Onsager, D. E. Rowland, R. E. Denton, J. L. Posch, C. T. Russell, P. J.
Chi, R. L. Arnoldy, B. J. Anderson, H. Fukunishi (2005), On the source of Pc1-2 waves in the
plasma mantle, J. Geophys. Res., 110, A06201, doi:10.1029/2004JA010515.
Fennell, J. F., Chen, M. W., Roeder, J. L., Peterson, W. K., Trattner, K. J., Friedel, R., Livi, S.,
Grande, M., Perry, C., Fritz, T. A., and Sheldon, R. (1998), Multiple discrete-energy ion features
18
in the inner magnetosphere: Polar observations, in Physics of Space Plasmas, 15, 395, MIT
Center for Theoretical Geo/Cosmo Plasma Physics, Cambridge, MA.
Frahm, R. A., Reiff, P. H., Winningham, J. D. and Burch, J. L.(1986), Banded ion morphology:
Main and recovery storm phases, in Ion Acceleration in the Magnetosphere and Ionosphere,
Geophys. Monogr. Ser., vol. 38, edited by T. Chang et al., pp. 98-107, AGU, Washington, D. C.
Hirahara, M., Mukai, T., Nagai, T., Kaya, N., Hayakawa, H.,and Fukunishi, H. (1996), Two
types of ion energy dispersions observed in the nightside auroral regions during geomagnetically
disturbed periods, J. Geophys. Res., 101, 7749.
Hirahara, M., T. Mukai, E. Sagawa, N. Kaya, and H. Hayakawa (1997), Multiple energydispersed ion precipitations in the low-latitude auroral oval: Evidence of ExB drift effect and
upward flowing ion contribution, J. Geophys. Res., 102, 2513.
Hudson, M.K ,W. Lotko, C.A. Cattell, R. Lysak, I. Roth and M. Temerin (1995), Modeling
mesoscale processes in the global geospace system, in The Global Geospace Mission, Space Sci.
Reviews, 71, 623.
Kazama, Yoichi. and Mukai, Toshifumi (2003), Multiple energy-dispersed ion signatures in the
near-Earth magnetotail: Geotail observation. Geophys. Res. Lett., 30, 1384,
doi:10.1029/2002GL016637.
Karimabadi, H., T. B. Sipes, H. White, A. Dmitriev, J. K. Chao, and N. Balac (2006), Reverse
engineering algorithms and a survey of machine learning techniques: Derivation of analytical
solutions from time series data, pre-print.
Kistler, L. M., Klecker, B., Jordanova, V. K., M®obius, E., Popecki, M. A., Patel, D., Sauvaud,
J.-A., R¥eme, H., Di Lellis, A. M., Korth, A., McCarthy, M., Cerulli, R., Bavassano Cattaneo,
M.B., Eliasson, L., Carlson, C.W., Parks, G. K., Paschmann, G., Baumjohann, W., and
Haerendel,G. (1999), Testing electric field models using ring current ion energy spectra from the
Equator-S ion composition (ESIC) instrument, Ann. Geophys., 17, 1611.
Kovrazhkin, R. A., Sauvaud, J. -A., and Delcourt, D. C. (1999), Interball-Auroral observations of
0.1-12keV ion gaps in the diffuse auroral zone, Ann. Geophys., 17, 734.
Kozyra, J. U., A. F. Nagy, and D. W. Slater (1997), High-latitude energy source(s) for stable
auroral red arcs, Rev. Geophys, 35, 155.
Kozyra, J. U., M. O. Chandler, D. C. Hamilton, W. K. Peterson, D. M. Klumpar, D. W. Slater,
M. J. Buonsanto, and H. C. Carlson (1993), The role of ring current nose events in producing
stable auroral red arc intensifications during the main phase: Observations during September 1924, 1984, equinox transition study, J. Geophys. Res., 98, 9267.
Kozyra, J et al. (2004a), Coupling Processes in the Inner Magnetosphere Associated with
Midlatitude Red Auroras during Superstorms, SM12B-03, Fall AGU.
19
Kozyra, J. et al. (2004b), Superstorms Observations and Insights: Observer Perspective,
Huntsville Workshop, Oct.
Li, X., Baker, D. N., Temerin, M., Peterson, W. K., and Fennell, J. F. (2000), Multiple discreteenergy ion features in the inner magnetosphere: Observations and Simulations, Geophys. Res.
Lett, 27, 1447.
Liemohn, M. W., Khazanov, G. V., and Kozyra, J. U. (1998), Banded electron structure
formation in the inner magnetosphere, Geophys. Res. Lett., 25, 877.
Lopez, Ramon E., Michael Wiltberger and John G. Lyon (2004), Coupling between the solar
wind and the magnetosphere during strong driving: MHD simulations, IEEE Trans. Plasma Sci.,
32, 1439.
Mauk, B. H. (1986), Quantitative modeling of the ‘convection surge’ mechanism of ion
acceleration, J. Geophys. Res., 91, 13,423.
J. P. McFadden, Y.K. Tung, C. W. Carlson, R. J. Strangeway, E. Möbius, and L. M. Kistler
(2001), FAST observations of ion outflow associated with magnetic storms, Space Weather,
Geophysical Monograph 125, 413.
McFadden, J. P., C. W. Carlson, R. Strangeway, and E. Moebius (2003), Observations of
downgoing velocity dispersed O+ and He+ in the cusp during magnetic storms, Geophys. Res.
Lett., 30, 1947, doi:10.1029/2003GL017783.
Moore, T. E., W. K. Peterson, C. T. Russell, M. O. Chandler, M. R. Collier, H. L. Collin, P. D.
Craven, R. Fitzenreiter, B. L. Giles, and C. J. Pollock (1999), Ionospheric mass ejection in
response to a coronal mass ejection, Geophys. Res. Lett., 26, 2339.
Nakajima, A., K. Shiokawa, K. Seki, J. P. McFadden, and C. W. Carlson (2005), Particle and
field characteristics of broadband electrons observed by the FAST satellite during geomagnetic
storms, SA21A-0283, Fall AGU.
Peterson, W. K., Trattner, K. J., Lennartsson, O. W., Collin, H. L., Baker, D. N., Pulkkinen, T.
I.,Toivanen, P. K., Fritz, T. A., Fennell, J. F., and Roeder, J. L.(1998), Imaging the plasma sheet
with energetic ions from the Polar satellite, Proc. of ICS-4, Terra Sci. Publishing, Tokyo, 813.
Quinn, J. M., and McIlwain, C. E. (1979), Bouncing ion clusters in the Earth's magnetosphere, J.
Geophys.Res., 84, 7365.
Shiokawa, K., K. Yumoto, C.-I. Meng, and G. Reeves (1996), Broadband electrons observed by
the DMSP satellites during storm-time substorms, Geophys. Res. Lett., 23, 2529.
20
Shiokawa, K., C.-I. Meng, G. D. Reeves, F. J. Rich and K. Yumoto (1997), A multievent study
of broadband electrons observed by the DMSP satellites and their relation to red aurora observed
at midlatitude stations, J. Geophys. Res., 102, 14,253.
Shiokawa, K., T. Ogawa, H. Oya, F. J. Rich, and K. Yumoto (2001), A stable auroral red arc
observed over Japan after an interval of very weak solar wind, J. Geophys. Res., 106, 26,901.
Siscoe, G. L., G. M. Erickson, B. U. Ö. Sonnerup, N. C. Maynard, J. A. Schoendorf, K. D.
Siebert, D. R. Weimer, W. W. White, and G. R. Wilson (2002), Hill model of transpolar
potential saturation: Comparisions with MHD simulations, J. Geophys. Res., 107, 1075,
doi:10.1029/2001JA000109.
Strangeway, R. J., R. E. Ergun, Y.-J. Su, C. W. Carlson, and R. C. Elphic (2005), Factors
controlling ionospheric outflows as observed at intermediate altitudes, J. Geophys. Res., 110,
A03221, doi:10.1029/2004JA010829.
Strangeway, R. J., C. T. Russell, C. W. Carlson, J. P. McFadden, R. E. Ergun, M. Temerin, D.
M. Klumpar, W. K. Peterson, and T. E. Moore (2000), Cusp field-aligned currents and ion
outflows, J. Geophys. Res., 105, 21,129.
Streed, T., C. Cattell and I. Roth (2000a), Particle tracing in the magnetotail: Dependence on
global magnetic field model, UMSI Research Report.
Streed, T., C. Cattell and I. Roth (2000b), Modifications of ion trajectories in the magnetotail due
to low frequency waves, UMSI Research Report.
Su Y.-J., S. T. Jones, R. E. Ergun, S. E. Parker (2004), Modeling of field-aligned electron bursts
by dispersive Alfvén waves in the dayside auroral region, J. Geophys. Res., 109, A11201,
doi:10.1029/2003JA010344.
Thompsen, M. et al. (2004), Energized Ions in the Dayside Magnetosphere During the SEC
Events of Late October 2003, SH42A-05, AGU, Spring.
Winningham, J. D., Burch, J. L., and Frahm, R. A. (1984), Bands of ions and angular V's: A
conjugate manifestation of ionospheric ion acceleration, J. Geophys. Res., 89, 1749.
Wygant, J. R., et al. (2000), Polar spacecraft based comparisons of intense electric fields and
Poynting flux near and within the plasma sheet-tail lobe boundary to UVI images: An energy
source for the aurora, J. Geophys. Res., 105, 18,675.
Wygant, J. R., et al. (2001), Observations of intense electric and magnetic fields and associated
Poynting flux though-out the plasma sheet during major geomagnetic storms, Eos Trans. AGU,
82, Fall Meet. Suppl.
Wygant, J. R., et al. (2002a), Evidence for kinetic Alfvén waves and parallel electron
energization at 4-6 RE altitudes in the plasma sheet boundary layer, J. Geophys. Res., 107, 1201,
21
doi:10.1029/2001JA900113.
Wygant, J. R., et al. (2002b), Observations from the Polar and Cluster spacecraft of the structure
and dynamics of strong Poynting flux in the plasma sheet during periods of strong magnetic
activity, Eos Trans. AGU, 83, Fall Meet. Suppl.
Yamauchi, M., Lundin, R., Eliasson, L., and Norberg, O. (1996), Meso-scale structures of
radiation belt/ring current detected by low-energy ions, Adv. Space Res., 17(2), 171.
22
3. Summary of Personnel and Work Effort
NAME
C. Cattell
J. Dombeck
ROLE
PI
Co-I
INSTITUTION
U. Minnesota
U. Minnesota
23
Year 1
4%
42%
Year 2
4%
42%
Year 3
4%
42%
4. Facilities and Equipment
The Space Plasma Physics group at the University of Minnesota has a network of Unix
desktop machines, including primarily Sun Sparc’s. In addition, there are PCs running Linux,
and many Macintosh machines. These are all networked to both color and PostScript printers,
and to a VAX server with disk/tape chains, which serves all the ISTP KP files and Geotail, Wind
and Polar fields and waves data sets. We have the complete high time resolution FAST data set
on CD and the complete Polar and Cluster fields data on CD with appropriate software to access
the data. The available computer equipment are appropriate for this project.
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5. Budget Justification
UNIVERSITY OF MINNESOTA
Salaries: Based on current salary of named personnel and University rate for ABD (all but
dissertation) graduate student.
Fringe rates are 32.8% for IT Professional (J. Dombeck), 20.1% for Professor (Cattell) and
22.5% for ABD graduate student.
Salary increases: Based on 3% per year
Computer costs: Includes computer service contracts, computer supplies and software necessary
to the performance of the proposed research.
Travel, domestic: Travel to AGU based on $500. airfare, 5 days at $200/day (SF hotel/food
reimbursement rate) and $380 registration fee. Increase of 3%/year
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6. Biographical Sketches
C. Cattell, PI
J. Dombeck, Co-I
26
CYNTHIA A. CATTELL
Address:
School of Physics and Astronomy, University of Minnesota
116 Church Street, S. E. Minneapolis, MN 55455
Appointments:
2000-present
Professor of Physics, University of Minnesota
1994-2000
Associate Professor of Physics, University of Minnesota
1989-1994
Senior Fellow, Space Sciences Laboratory, Univ. of California, Berkeley
Selected Relevant Publications (from more than 100 refereed articles):
“The Association of Electrostatic Ion Cyclotron Waves, Ion and Electron Beams and Field-Aligned
Currents: FAST Observations of An Auroral Zone Crossing Near Midnight”, C. Cattell et al.,
Geophys. Res. Let., 25, 2053, 1998.
“FAST-Geotail Correlative Studies of Magnetosphere-Ionosphere Coupling in the Nightside
Magnetosphere, K. Sigsbee et al., Geophys. Res. Lett.,25, 2077, 1998.
“Pi2 pulsations observed with the Polar satellite and ground stations: Coupling of trapped and
propagating fast mode waves to a midlatitude field line,” Keiling, A., Wygant, J. R.,Cattell,
C.,Kim, K.-H., Russell, C. T., Milling, D. K.,Temerin, M., Mozer, F. S.,A Kletzing, C. A., J.
Geophys. Res.,106, p.25, 891, 2001.
“Evidence for kinetic Alfven waves and parallel electron energization at 4-6 Re altitudes in the
plasma sheet boundary,” Wygant, J., A. Keiling,, C. Cattell, R. Lysak, M. Temerin, F. Mozer, C.
Kletzing, J. Scudder, A. Streltsov, W. Lotko, and C. Russell,” J. Geophys. Res., 107, NO. A8,
10.1029/2001JA900113, 2002
"Observations of the seasonal dependence of the thermal plasma density in the southern hemisphere
auroral zone and polar cap at 1 Re", M. T. Johnson, J. R. Wygant, C. Cattell, F. S. Mozer, M.
Temerin, and J. Scudder, J. Geophys. Res., 106, p.19023, 2001.
“FAST observations of discrete electrostatic waves in association with downgoing ion beams in the
auroral zone,” C Cattell, L. Johnson, R. Bergmann, D. Klumpar, C. Carlson, J. McFadden , R.
Strangeway, R. Ergun, K. Sigsbee, R. Pfaff , J. Geophys. Res., 107, 1238,
doi:10.1029/2001JA000254, 2002.
“A comparison of Pi2 pulsations in the inner magnetosphere and magnetic pulsations at
geosynchronous orbit,” Kim, K.-H.,Takahashi, K.,Lee, D.-H.,Lin, N., Cattell, C. A., J. Geophys.
Res., 106, 18,865, 2001.
“FAST observations of the dependence of dayside field-aligned currents on solar wind
parameters,” C. Cattell, J. Dombeck, W. Peria, R. Strangeway, R. Elphic, C. Carlson, J.
Geophys. Res., J. Geophys. Res. , 108,10.1029/2001JA000321, 2003.
“Polar observations of solitary waves at high and low altitudes and comparison to theory,” C.
Cattell, J. Crumley, J. Dombeck, C. Kletzing, W. K. Peterson and H. Collin, Adv. Space Res., 28,
p. 1631, 2001.
“Large Amplitude Solitary Waves in and near the Earth’s Magnetosphere, Magnetopause and Bow
Shock: Polar and Cluster Observations,” C. Cattel1, C. Neiman, J. Dombeck, J. Crumley, J.
Wygant, C. A. Kletzing, W. K. Peterson, F.S. Mozer, Mats André, Nonlinear Processes in
Geophysics, 10: 13–26, 2003.
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‘Correlation of Alfven wave Poynting flux in the plasma sheet at 4-7 Re with ionospheric electron
energy flux, A. Keiling, Wygant, J. R.,Cattell, C., W. Peria, G. Parks, M. Temerin, Mozer, F. S.,
C. Russell and C. Kletzing, J. Geophys. Res., 107, 10.1029/2001JA900140, 2002.
‘Magnetospheric responses to sudden and quasiperiodic solar wind variations ,’
K.-H. Kim, C. A. Cattell, D.-H. Lee, K. Takahashi, K. Yumoto, K. Shiokawa, F. S. Mozer, M.
Andre, J. Geophys. Res.,107, NO. A11, 1406, doi:10.1029/2002JA009342, 2002.
‘FAST observations of of the solar illumination dependence of upflowing electron beams in the
auroral zone,’ C. Cattell, J. Dombeck, W. Yusoff, C. Carlson and J. McFadden, J. Geophys. Res.,
VOL. 109, A02209, doi:10.1029/2003JA010075, 2004
Electrodynamic of substorm-related field line resonance measured with the Polar satellite, A.
Keiling, K.-H. Kim, J. R. Wygant, C. Cattell, C. A. Kletzing, and C. T. Russell, J. Geophys.
Res.,, 108, A7, 1275, doi:10.1029/2002JA009340, 2003
‘The Global Morphology of Wave Poynting Flux: Powering the Aurora,’ A. Keiling, J. R. Wygant,
C. A. Cattell, F. S. Mozer, and C. T. Russell, Science, January 17; 299: 383-386, 2003.
. ‘Seasonal variations along auroral field lines: Measurements from the Polar spacecraft,’
M. T. Johnson, J. R. Wygant, C. A. Cattell, F. S. Mozer, Geophysical Research Letters, VOL. 30,
NO. 6, 1344, doi:10.1029/2002GL015866, 2003.
Enhanced tail electric feld triggered by solar wind pressure impulse, Kim, K.-H., C. A. Cattell, D.H. Lee, A. Balogh, M. Andre, Y. Khotyaintsev, S. B. Mende, and E. Lee, submitted to
Geophysical Research Letters, 2004.
Alfvén waves and Poynting flux observed simultaneously by Polar and FAST in the plasma sheet
boundary layer, Dombeck, J., C. Cattell, J. R. Wygant, A. Keiling, and J. Scudder (2005) J.
Geophys. Res., 110, A12S90, doi:10.1029/2005JA011269.
Simultaneous ground-based and satellite observations of Pc5 geomagnetic pulsations, S.-K. Sung,
K.-H. Kim, D.-H. Lee, C. A. Cattell, M. Andre, and Y. V. Khotyaintsev, s J. Geophys. Res, in
press, 2006..
Cattell, C., J. Dombeck, C. Carlson, and J. McFadden (2006), FAST observations of the solar
illumination dependence of downgoing auroral electron beams: Relationship to electron energy
flux, J. Geophys. Res., 111, A02201, doi:10.1029/2005JA011337.
Professional Activities:
C. Cattell has been a co-investigator on ISEE, Polar, Cluster and FAST and a PI on the AMPS
Mission study and many data analysis grants. She has been a member of various advisory
committees for Space Physics, including the National Academy of Sciences/Committee on Solar
Terrestrial Research(1993-1995) and the NASA Sun-Earth -Connection Advisory Subcommittee
(1998-2001), NAS Plasma Sciences Committee (2001-2005) and the SSSC Roadmap Committee
(2004-2005). She is a member of the ‘Physics Force’ team-an outreach group doing large scale,
exciting Physics demonstration shows for K12 schools and the general public throughout
Minnesota.
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John P. Dombeck
School of Physics and Astronomy, University of Minnesota
Tate Lab of Physics, 116 Church St. SE, Minneapolis, MN 55455
Current Responsibilities:
John Dombeck has been in the University of Minnesota Space Physics group for the past 9 years,
and in his current position as IT Professional for the past 5 years. In addition to his research, his
responsibilities include data analysis and development of analysis software for space physics
applications, including the Polar, FAST and Cluster missions. He is also responsible for
coordination and continuity of the space physics data analysis programming effort at the
University of Minnesota and system administration of the group’s data analysis network.
Other Experience:
John has broad science, technical, and management experience, having received a BSEE in 1992
and a BS in Physics in 1995. He has worked in an engineering capacity for Eaton Corporation,
developing hardware for the US Navy, as a Failure Analysis Engineer for IBM Corporation, and
as a programmer of flood prediction software at the National Weather Service. He also served
as the Product Development/Operations Manager for Callnetics Inc., in the real-estate industry,
where he was responsible, from concept to live operational maintenance, for the seven member
programming and system administration team for a national scale, real-time web and telephone
(IVR) based scheduling system.
Science Interest:
His science interests include major storm processes related to the powering of aurora, solitary
waves and the connection between solar wind and ionospheric conditions and auroral
acceleration processes. He received his PhD in 2005, and has 13 peer-reviewed publications.
Selected Papers:
Dombeck, J., C. Cattell, J. R. Wygant, A. Keiling, and J. Scudder (2005), Alfvén waves and
Poynting flux observed simultaneously by Polar and FAST in the plasma sheet boundary layer, J.
Geophys. Res., 110, doi:10.1029/2005JA011269.
Keiling, A., G. K. Parks, J. R. Wygant, J. Dombeck, F. S. Mozer, C. T. Russell, A. V. Streltsov,
and W. Lotko (2005), Some properties of Alfvén waves: Observations in the tail lobes and the
plasma sheet boundary layer, J. Geophys. Res., 110, doi:10.1029/2004JA010907.
Cattell, C., J. Dombeck, W. Yusof, C. Carlson, J. McFadden (2004), FAST observations of the
solar illumination dependence of upflowing electron beams in the auroral zone, J. Geophys. Res.,
109, doi:10.1029/2003JA010075.
Cattell, C., J. Dombeck, W. Peria, R. Strangeway, R. Elphic, C. Carlson (2003), Fast Auroral
Snapshot observations of the dependence of dayside auroral field-aligned currents on solar wind
parameters and solar illumination, J. Geophys. Res., 108, doi:10.1029/2001JA000321.
Dombeck, J., C. Cattell, J. Crumley, W. K. Peterson, H. L. Collin, and C. Kletzing (2001),
Observed trends in auroral zone ion mode solitary wave structure characteristics using data from
Polar, J. Geophys. Res., 106, 19,013.
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5. Co-I and/or Collaborator Commitments
Michelle Thompsen, Collaborator
Janet Kozyra, Collaborator
John Dombeck, Co-I
30
31
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8. Current and Pending Support
Cynthia A. Cattell
Current and Pending Support
Current (PI):
NASA FAST (subcontract from UCB) Data analysis
02/1/2005-1/31/2006
$69,000
Commitment: 4%
NASA SEC/GI: “Cross-scale coupling at the Earth's magnetosphere: Cluster and Polar studies”
4/1//04-3/31/07 Proposed: $288, 680.
Commitment: 12.5%
Pending:
NASA Solar/Heliosphere: “Microphysical processes at interplanetary shocks”
8/1/06-7/31/09 Proposed: $332,997
Commitment: 8.3%
NASA HGI: “Microphysical processes at interplanetary shocks”
2/1/07-1/31/10 Proposed: $332,997
Commitment: 8.3%
NASA HGI: “Particle acceleration processes on auroral field lines during major geomagnetic
storms” (this proposal)
2/1/07-1/31/10 Proposed: $378,009.
Commitment: 4%
Pending (Co-I):
NASA LWS/RBSP: J. Wygant, P.I. - “Electric Field And Search Coil (EFASC) Instrument Suite
for the Radiation Belt Storm Probe Mission”
4/1/06-9/2014 Proposed: $22.8M
Commitment: 6%
NASA MMS/IDS: H. Karamabadi, PI-“An integrated approach to mission planning, operation
and science of MMS: Theory, data analysis and Instrumentation”
5/1/06-9/30/2016 Proposed: $908,004.
Commitment: 8.3%
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Current and Pending Research Support for Dr. J. Dombeck
No Current Awards
Pending Support:
NASA Co-I
NASA HGI: C. Cattell, PI- “Particle acceleration processes on auroral field lines during major
geomagnetic storms”(this proposal)
2/1/07-1/31/10 Proposed: $378,009.
Commitment: 42%
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