Summary Report

Workshop on Energetic Particle Measurements for the GOES R+ Satellites

Held at the

NOAA Space Environment Center

Boulder, CO

October 28-29, 2002

# 

Workshop reporter: Dr. J. E. Mazur

The Aerospace Corporation

Space Sciences Department

January 2003

#  

1\. Summary [3](#summary)

1\. Synthesis of workshop recommendations
[6](#synthesis-of-workshop-recommendations)

1.1 Electrons 100 eV-30 keV: surface charging
[6](#electrons-100-ev-30-kev-surface-charging)

1.2 Protons [7](#protons)

1.2.1 Protons \<30 keV: surface dose and damage
[7](#protons-30-kev-surface-dose-and-damage)

1.2.2 Protons \>300 MeV: total dose in SEP events
[8](#protons-300-mev-total-dose-in-sep-events)

1.3 Z≥2 [9](#z2)

1.3.1 Z≥2, 1-100 keV: surface damage [9](#z2-1-100-kev-surface-damage)

1.3.2 Z≥2 above 10 MeV/nucleon: single-event effects
[9](#z2-above-10-mevnucleon-single-event-effects)

2\. Measurement priorities [12](#measurement-priorities)

3\. Instrument options [14](#instrument-options)

3.1 Electrons and protons 100 eV - 30 keV
[14](#electrons-and-protons-100-ev---30-kev)

3.2 Z≥2 above 10 MeV/nucleon [15](#z2-above-10-mevnucleon)

4\. References [15](#references)

5\. Acronym list [16](#acronym-list)

Appendix 1. Questionnaire results
[17](#appendix-1.-questionnaire-results)

Appendix 2. Summary of workshop presentations
[20](#appendix-2.-summary-of-workshop-presentations)

Appendix 3. Attendance list distributed on October 28, 2002.
[23](#appendix-3.-attendance-list-distributed-on-october-28-2002.)

Appendix 4. Workshop schedule. [25](#appendix-4.-workshop-schedule.)

#  

# 1. Summary

# 

On October 28-29, 2002, the NOAA Space Environment Center hosted a
workshop to solicit views on energetic particle measurements for the
future GOES R+ spacecraft. Terry Onsager of NOAA/SEC and Joe Mazur of
The Aerospace Corporation invited workshop speakers, other attendees,
and distributed a workshop questionnaire. Attendees included
representatives from NOAA, the US military, academic institutions, and
other government agencies. This document is a synthesis of the
recommendations for particle measurements for the GOES R+ vehicles based
on the workshop presentations and the responses to a workshop
questionnaire.

Table 1 lists the main recommendations of the workshop. The fiducial for
the workshop was the capability of the GOES N-Q energetic particle
instrumentation \[Onsager\]. In the case of electrons and protons, these
recommendations extend the GOES N-Q capabilities to energies below 30
keV. The major justifications were the improved specification of the
electron spectrum in surface charging events and the extension of
radiation belt models to cover energies important for surface dose and
damage of spacecraft surfaces. Surface charging is a significant hazard
for spacecraft in GEO and the question of surface dose and damage is
important for applications of new spacecraft materials. There is also
the science interest in the acceleration and drift of substorm electrons
because, for example, of their possible role as seed particles for
further acceleration up to MeV energies.

The case of Z≥2 ions is a new capability for GOES N-Q which measure only
Z=2 above 4 MeV. The major justification for the heavy ion measurements
was the improved specification of heavy ion spectra in solar particle
events that cause single-event effects in electronics. The required
instrumentation is more complex than the GOES-9 \"Dome\" detectors.
There was also a recommendation to include Z=8 at plasma energies for
its role in surface damage to satellites.

Measurements of protons and electrons below 30 keV would be achievable
with a single electrostatic analyzer. The energetic heavy ions would
require a more complex solid-state detector telescope. See section 3 for
more details on the instrument options.

In all cases, the workshop attendees agreed that GOES data are valuable
for near-real time situational awareness. Several presenters also
stressed the value of the easily accessible and long-term archive of
GOES data for development of future models and for input to science
analysis.

+--------+----------+----------+----------+-----------+---------+----+
| **Spe  | **Energy | **Target | **       | **Pitch   | **Instr | ** |
| cies** | range**  | phen     | Spectral | angle     | ument** | Pa |
|        |          | omenon** | reso     | res       |         | ge |
|        |          |          | lution** | olution** | **Type  | \# |
|        |          |          |          |           | ^1^**   | ** |
+--------+----------+----------+----------+-----------+---------+----+
| Ele    | 100 eV-  | Surface  | 10 to 40 | 5 to 36   | ESA ^2^ | 6  |
| ctrons | 30 keV   | charging | channels | bins; if  |         |    |
|        |          |          |          | not       |         |    |
|        |          |          |          | possible, |         |    |
|        |          |          |          | restrict  |         |    |
|        |          |          |          | to        |         |    |
|        |          |          |          | e         |         |    |
|        |          |          |          | quatorial |         |    |
|        |          |          |          | pitch     |         |    |
|        |          |          |          | angles    |         |    |
+--------+----------+----------+----------+-----------+---------+----+
| P      | 100 eV-  | Surface  | 10 to 40 | 5 to 36   | ESA     | 7  |
| rotons | 30 keV   | damage   | channels | bins; if  |         |    |
|        |          |          |          | not       |         |    |
|        |          |          |          | possible, |         |    |
|        |          |          |          | restrict  |         |    |
|        |          |          |          | to        |         |    |
|        |          |          |          | e         |         |    |
|        |          |          |          | quatorial |         |    |
|        |          |          |          | pitch     |         |    |
|        |          |          |          | angles    |         |    |
+--------+----------+----------+----------+-----------+---------+----+
| P      | \>300    | Total    | 5        | 2 look    | Same as | 8  |
| rotons | MeV      | dose in  | channels | d         | GOES-9  |    |
| ^3^    |          | SEP      | ;        | irections |         |    |
|        |          | events   | channel  |           |         |    |
|        |          |          | widths   |           |         |    |
|        |          |          | chosen   |           |         |    |
|        |          |          | to       |           |         |    |
|        |          |          | optimize |           |         |    |
|        |          |          | st       |           |         |    |
|        |          |          | atistics |           |         |    |
|        |          |          | in       |           |         |    |
|        |          |          | typical  |           |         |    |
|        |          |          | MeV^-2^  |           |         |    |
|        |          |          | spectra  |           |         |    |
+--------+----------+----------+----------+-----------+---------+----+
| Z≥2    | 1- 100   | Surface  | 10 to 40 | One       | ESA or  | 9  |
|        | keV      | damage   | channels | e         | magneti |    |
| (Z=8)  |          |          |          | quatorial | c-specr |    |
|        |          |          |          | look      | om-eter |    |
|        |          |          |          | direction |         |    |
+--------+----------+----------+----------+-----------+---------+----+
| Z≥2    | 10-500   | Sing     | 10       | One look  | M       | 9  |
|        | MeV      | le-event | diff     | direction | ultiple |    |
| O      | /nucleon | effects  | erential | (west)    | soli    |    |
| ption: |          | in SEP   | for      |           | d-state |    |
| coarse |          | events   | coarse   |           | d       |    |
| Z      |          |          | mass     |           | etector |    |
| reso   |          |          | re       |           | te      |    |
| lution |          |          | solution |           | lescope |    |
| ^4^    |          |          | in       |           |         |    |
|        |          |          | strument |           |         |    |
+--------+----------+----------+----------+-----------+---------+----+
| Z≥2    | LET from | Sing     | \>36     | One look  | Soli    | 10 |
|        | 0.1- 100 | le-event | channels | direction | d-state |    |
| O      | MeV/     | effects  | in LET   | (west)    | d       |    |
| ption: | mg-cm^2^ | in SEP   |          |           | etector |    |
| LET    |          | events   |          |           | behind  |    |
| m      |          |          |          |           | sh      |    |
| onitor |          |          |          |           | ielding |    |
+--------+----------+----------+----------+-----------+---------+----+

*Table 1. Summary of GOES R+ energetic particles workshop
recommendations.*

*Notes: ^1^ See section 3.*

> ^2^ *Electrostatic analyzer.*
>
> *^3^ Modification of current capability of GOES N-Q: higher spectral
> resolution &*
>
> *optimized channel widths.*

^4^ *Coarse resolution in Z corresponding to the mass groups He, CNO,
Ne-S, and Fe.*

Section 1 of this document contains a summary and synthesis of the major
recommendations in the context of the GOES I-M and N-Q capabilities.
Section 2 discusses the priority of the recommendations, keeping in mind
that the priorities for space environment data change as spacecraft
technologies evolve. Section 3 discusses some instrument options for
making the recommended measurements.

# 1. Synthesis of workshop recommendations

The recommendations discussed in this section originate from the
presentations at the workshop as well as the discussions and the
workshop questionnaire. We present them in a format that NOAA/SEC might
use to develop requirements for the GOES R+ particles instrumentation.
They break down into three main areas: electrons (section 1.1), protons
(section 1.2), and Z≥2 ions (section 1.3).

## 1.1 Electrons 100 eV-30 keV: surface charging

The workshop recommended extending the energy range for electrons to
below the lower energy limit of the GOES N-Q satellites of 30 keV. The
main phenomenon driving this recommendation was differential charging of
satellite surfaces (Fennell; Mandell; Carey). Fennell presented an
overview of surface charging, pointing out the general conditions that
lead to surface charging, but also noting that the phenomenon cannot yet
be predicted in detail for a given vehicle in spite of significant
modeling efforts. Bodeau \[1\] pointed out an additional value of having
monitors of the surface charging environment at the GOES satellites:
GOES vehicles are closer to other satellites that orbit over the
continental United States (CONUS) than the well-instrumented Los Alamos
National Laboratory (LANL) vehicles \[Baker et al. 1985\].

Figure 1 shows an electron spectrum measured at geostationary orbit
(GEO) during a charging event on a LANL vehicle \[Mandell\] along with
fits to the spectrum. In this case the data down to \~100 eV constrained
the model of the environment.

![](media/image1.png){width="4.541666666666667in"
height="3.926388888888889in"}

*Figure 1. Measured electron spectrum (data points) and model fits
(curves) to the electron environment during a surface-charging event on
a LANL vehicle \[Mandell\].*

Figure 2 shows the energy coverage electrons for GOES I-M and N-Q. The
figure also shows the workshop recommendation of a lower-energy limit of
\~ 100 eV for GOES R+.

![](media/image2.png){width="6.49375in" height="2.9402777777777778in"}

*Figure 2. Electron energy coverage of GOES I-M, N-Q, and workshop
recommendation for R+. Energies above 4 MeV are integral.*

## 1.2 Protons 

### 1.2.1 Protons \<30 keV: surface dose and damage

The workshop recommended extending the energy range for protons to below
the lower energy limit of the GOES N-Q satellites of 30 keV. The
phenomena driving this recommendation were radiation dose to surfaces,
surface damage \[Bodeau; Fennell\] and source populations for the ring
current \[Carey; Sibeck\].

Fennell \[1\] presented one example of ground-based tests of solar array
cover glass samples after exposure to 10 years of the low-energy proton
environment (Figure 3). Discolorations in the figure indicated changes
to the light transmittance of cover glass samples made with different
compositions. The changes from a visibly clear glass would have
decreased the power output of the underlying arrays significantly. The
value of GOES measurements of protons down to \~100 eV would be the
construction of an environment specification for use in spacecraft
design \[Bodeau; Fennell\].

![](media/image3.png){width="6.057638888888889in"
height="4.595138888888889in"}

*Figure 3. Laboratory exposures of samples of solar array cover glass to
low-energy protons \[Fennell\].*

### 1.2.2 Protons \>300 MeV: total dose in SEP events

There were two recommendations for the high-energy (\>300 MeV) GOES
proton measurements. They both referred to the specification of the most
extreme solar energetic particle events where the spectral forms are
important inputs to total dose calculations for spacecraft design. The
first was to increase the spectral resolution above 300 MeV (GOES I-M,
N-Q HEPAD has 3 differential channels and one integral above 700 MeV) in
order to better measure the solar energetic spectrum of total ions at
extremely high energies \[Carey; Chenette\]. The second recommendation
was to adjust these high-energy range channel widths according to a
typical energy-2 spectral slope to insure adequate statistics in the
higher-energy channels \[Kahler\].

Figure 4 shows the energy coverage of protons for GOES I-M and N-Q and
the workshop recommendation of a lower-energy limit of \~ 100 eV. This
lower energy limit would be the same as the electron limit if the
measurements were made with a switching electrostatic analyzer (see
section 3).

![](media/image4.png){width="6.49375in" height="2.9291666666666667in"}

*Figure 4. Proton energy coverage of GOES I-M, N-Q, and workshop
recommendation for R+.*

## 1.3 Z≥2 

For ions more massive than protons, the workshop presentations,
questionnaire, and discussions focused on both surface-damage from
low-energy plasma and single-event effects from high-energy ions. The
GOES I-M and N-Q cover helium from \~1-850 MeV/nucleon but do not
identify heavier ions in any energy range. Most workshop attendees
suggested the addition of Z\>2 ion measurements to GOES R+ in order to
address the phenomena summarized in the following two sections.

### 1.3.1 Z≥2, 1-100 keV: surface damage

The workshop recommended measurements of \~1-100 keV O+, in addition to
the H+ discussed in section 1.2.1, to address the most abundant species
in the Earth\'s ring current for their effects on satellite surfaces
(*e.g.* Fennell; Carey; Sibeck). Specifically, these ions cause high
radiation doses in surfaces as well as sputtering of materials whose
by-products might contaminate systems using optical coatings, even solar
arrays. Since the surface effects are accumulated over long exposures to
the environment, the value of making these measurements on the GOES
satellites would be the ultimate specification of the environment for
the design of future GEO spacecraft.

### 1.3.2 Z≥2 above 10 MeV/nucleon: single-event effects

The workshop discussed single-event effects from high energy (\>10
MeV/nucleon) heavy ions and the uncertain specification of the energy
spectra of these ions in intense solar energetic particle events
\[Barth; Golightly; Miller; Chenette\]. The workshop recommended that
coarse mass resolution from \~10-500 MeV/nucleon would be sufficient
(He, CNO, Ne-S, & Fe), and offered an alternative approach based on
particle energy deposit.

Chenette presented examples of the worst-case solar energetic particle
(SEP) environment for ions, pointing out that the composition and
variability of the galactic cosmic rays above \~10 MeV/nucleon are well
defined and not necessary to measure with GOES. The uses of these data
include spacecraft anomaly investigations, decisions for launches of
vehicles with single-event effect (SEE) susceptibilities, and archival
data for the generation of environmental models. Figure 5 compares the
helium spectrum from the recent 14 July 2000 event with the worst-case
\"1-day in a thousand\" measured on the IMP-8 satellite, highlighting
their differences and the need to better specify these large-event
spectra \[Chenette\].

![](media/image5.png){width="6.4944444444444445in"
height="4.607638888888889in"}

*Figure 5. 10-100 MeV/nucleon helium spectra in intense SEP events
\[Chenette\].*

Barth, Fennell, and Miller discussed the high-Z solar particle
environment from the LET (linear energy transfer) perspective. They also
pointed out the need for improved specification of the high-energy and
high-Z SEP environment, but expressed in units of LET (MeV/mg-cm^2^)
most useful to the spacecraft design and testing communities (Figure 6).
Section 3 discusses this measurement approach in more detail. Note that
the LET measurement does not resolve mass, but includes all the species
that are relevant to the energy deposit behind a known amount of
spacecraft shielding.

![](media/image6.png){width="6.488888888888889in"
height="3.8743055555555554in"}

*Figure 6. LET fluence spectrum integrated over a sequence of intense
solar particle events \[Barth\].*

Figure 7 summarizes the coverage in particle energy and atomic number
for Z≥2 ions on GOES I-M, N-Q, and the workshop recommendations for R+.

![](media/image7.png){width="6.495833333333334in"
height="4.353472222222222in"}

*Figure 7. Energy coverage versus atomic number for GOES I-M, N-Q, and
workshop recommendations for R+.*

# 2. Measurement priorities

The workshop discussions did not significantly address measurement
priorities. For the purposes of this report, one way to infer the
priorities implied at the workshop is to survey the presentations and
questionnaires for the frequency with which the various phenomena and
measurements were mentioned. This approach has unknown uncertainty, as
does any ranking of priorities based on the design needs for future
spacecraft. It is especially uncertain given the relatively low number
of participants.

Table 2 lists the number of presentations that explicitly mentioned the
need to make the following measurements. Based on the 11 presentations,
there was no phenomenon discussed at the workshop that had more interest
than any other. This suggests an equal priority for the recommended GOES
R+ measurements.

  ----------------------------------- -----------------------------------
  **Phenomena/measurement**           **Number of presentations that
                                      mentioned the need for the
                                      measurement**

  Surface charging from 100 eV - 100  5
  keV electrons                       

  Surface damage from 1-100 keV ions  3

  Single-event effects from \>10      4
  MeV/nucleon Z≥2                     
  ----------------------------------- -----------------------------------

*Table 2. Number of references in 11 workshop presentations to various
recommended GOES R+ measurements.*

For another approach to determining priorities, Fennell presented the
results of a survey of the effects of the space environment on space
systems \[Koons *et al.* 1999\]. Figure 8 is a histogram of the number
of spacecraft anomaly reports versus environmental cause from the Koons
*et al.* survey. Figure 8 suggests that the specification of the
surface-charging environment is most important since most of the surface
charging anomalies occurred in GEO. However, as noted above, if surface
charging is highly localized and unpredictable, then the long-term
specification of other surface effects and the LET environment may be a
more important contribution for GOES.

![](media/image8.png){width="6.49375in" height="4.534027777777778in"}

*Figure 8. Histogram of the number of spacecraft anomalies versus
environmental cause from the survey of Koons et al. \[Fennell &
Mazur\].*

# 3. Instrument options

There were few discussions on instrument options at the workshop, so not
every recommendation had an accompanying discussion about the details of
how to make the measurement. The following sections list the details
that were mentioned in the presentations. Table 3 lists the instrument
options ordered by their complexity relative to the simplest instruments
discussed at the meeting (surface charge monitor and LET monitor).

+-----------------------+-----------------------+-----------------------+
| **Instrument**        | **Product**           | **Relative            |
|                       |                       | complexity**          |
+-----------------------+-----------------------+-----------------------+
| Surface charge        | Surface-charging      | Simple                |
| monitor               | environment           |                       |
+-----------------------+-----------------------+-----------------------+
| LET monitor           | LET behind known      | Simple                |
|                       | shielding             |                       |
+-----------------------+-----------------------+-----------------------+
| ESA                   | -   Spectrum of       | Moderate, but         |
|                       |     electrons         | technologically       |
|                       |     responsible for   | mature                |
|                       |     surface-charging; |                       |
|                       |     low-energy        |                       |
|                       |     protons           |                       |
|                       |     responsible for   |                       |
|                       |     surface           |                       |
|                       |     dose/damage       |                       |
|                       |                       |                       |
|                       | -   In principle, Z≥2 |                       |
|                       |     using foil        |                       |
|                       |     technique         |                       |
+-----------------------+-----------------------+-----------------------+
| Z≥2 telescope         | SEP spectra above 10  | Moderate/high given   |
|                       | MeV/n                 | coarse resolution     |
|                       |                       | requirement           |
+-----------------------+-----------------------+-----------------------+
| Magnetic spectrometer | Plasma composition    | High                  |
+-----------------------+-----------------------+-----------------------+

*Table 3. Approximate relative complexity of several instrument options
for the recommended GOES R+ measurements.*

## 3.1 Electrons and protons 100 eV - 30 keV

The same instrument that would provide the spectral measurements of
electrons below \~30 keV for surface charging effects could also provide
the low-energy proton measurements important for surface dose and other
surface effects. An electrostatic analyzer with a cycling power supply
fulfills these requirements with resources on the order of a few kg and
a few watts \[Carey\]. In principle this same instrument could also
provide the plasma O+ measurement in Table 1 by using a thin foil to
stop the heavy ions, where the heavy ion intensity would be inferred by
subtraction.

Fennell noted another example of a dual electron and ion capability in a
single instrument. An ion detector in back of a small magnetic
spectrometer designed for electrons could provide clean proton
measurements in the range of \~10-100 keV. In this case, the clean
proton measurement results from the deflection of the lower-rigidity
electrons, and a threshold on a solid-state detector determines the
low-energy limit. The limit is not as low as achievable with an
electrostatic analyzer \[Carey\].

Fennell also noted the usefulness of a simple charging-plate design as
implemented on *Intelsat* satellites for monitoring the surface-charging
environment. In this case, the instrument returns the potential of the
monitor relative to the spacecraft with a simple and robust technique
but does not return the detailed spectra of the plasma environment that
were responsible for charging events. A charging plate is thus a simpler
and lower-cost alternative to an electrostatic analyzer.

## 3.2 Z≥2 above 10 MeV/nucleon

Measurements of 10-500 MeV/nucleon Z≥2 ions with resolution of the major
groups of He, CNO, Ne-S, and Fe, fulfills the need to specify the poorly
characterized variability of the heavy-ion components in intense SEP
events. The coarse resolution lightens the requirements for knowledge of
particle trajectories through an instrument with a stack of multiple
solid state detectors. It would still be necessary to have sufficient
detector material to stop high energy Fe (*e.g.* the range of 170 MeV/n
Fe is \~8.2 mm in silicon).

Barth noted that the energy spectra of individual ion species could be
transformed into units of LET behind various thicknesses of spacecraft
shielding for spacecraft engineering. However, Barth, as well as Miller
and Fennell, also pointed out the advantages of a direct measurement of
LET behind shielding. These advantages included the direct measurement
of the parameter used in the engineering community (LET), the ability to
measure LET behind several choices of shielding on the same vehicle, the
inclusion of all relevant particle masses, and the relative simplicity
of the instrument compared to a mass spectrometer.

In either case (mass spectrometer with coarse mass resolution or LET
monitor), the workshop discussions noted that these measurements are not
required on every GOES vehicle since the phenomenon is not as localized
in local time as, for example, surface charging. Mazur pointed out the
SEP anisotropy of \> 10 MeV protons at GEO due to particle access from
the East versus the West, but noted the Western-looking direction would
be sufficient for specifying the heavy-ion environment. It was also
noted that these Z≥2 ions could also be measured at an L1 monitor and
still have significant application to satellites in GEO, although the
time delay for propagating shocks from L1 to Earth can introduce
uncertainty in specifying the SEP environment for the space station
\[Golightly\].

# 

# 4. References

D. N. Baker, W. Aiello, J. R. Asbridge, R. D. Belian, P. R. Higbie, R.
W. Klebesadel, J. G. Laros and E. R. Tech, \"Los Alamos Energetic
Particle Sensor Systems at Geostationary Orbit,\" AIAA 85-0243. 1985.

J. Barth & M. Xapsos, \"SEP measurements required for environment models
and system design and testing\", GOES R+ EP Workshop, Boulder, CO, 28-29
October 2002.

M. Bodeau, \"What do satellite manufacturers want from GOES?\", GOES R+
EP Workshop, Boulder, CO, 28-29 October 2002.

T. Carey, \"LANL perspectives on space environment monitoring\", GOES R+
EP Workshop, Boulder, CO, 28-29 October 2002.

D. Chenette, \"On-orbit space systems users requirements for GOES
energetic particle data: a perspective from Lockheed Martin\", GOES R+
EP Workshop, Boulder, CO, 28-29 October 2002.

J. Fennell & J. Mazur, \"Overview of the impact of the space environment
on space systems\", GOES R+ EP Workshop, Boulder, CO, 28-29 October
2002.

J. Fennell, \"Let\'s not forget surface charging\", GOES R+ EP Workshop,
Boulder, CO, 28-29 October 2002.

M. Golightly, \"3^rd^ generation GOES spacecraft program: billions of
dollars...GOES energetic particle measurements for support of manned
spaceflight: priceless\", GOES R+ EP Workshop, Boulder, CO, 28-29
October 2002.

S. Kahler, \"Air Force Research Laboratory perspective on energetic
particle measurements\", GOES R+ EP Workshop, Boulder, CO, 28-29 October
2002.

H. Koons, J. E. Mazur, R. S. Selesnick, J. B. Blake, J. F. Fennell, J.
L. Roeder, & P. C. Anderson, The impact of the space environment on
space systems, Aerospace Technical Report TR-99(1670)-1, 1999.

M. Mandell, \"The case for low-energy electrons\", GOES R+ EP Workshop,
Boulder, CO, 28-29 October 2002.

K. Miller, \"The charged particle environment from a spacecraft
designer\'s perspective\", GOES R+ EP Workshop, Boulder, CO, 28-29
October 2002.

T. Onsager, \"GOES I-M and N-Q EPS Overview\", GOES R+ EP Workshop,
Boulder, CO, 28-29 October 2002.

D. Sibeck, \"Geospace and NASA\'s Living With a Star program\", GOES R+
EP Workshop, Boulder, CO, 28-29 October 2002.

# 5. Acronym list

CONUS continental United States

HEPAD high-energy proton and alpha detector

GEO geostationary orbit

LANL Los Alamos National Laboratory

LET linear energy transfer

SEE single-event effect

SEP solar energetic particle

# Appendix 1. Questionnaire results

On the GOES R+ workshop web site, NOAA/SEC provided the following
questionnaire to survey the uses, limitations, and needs of users of
GOES energetic particle data. The total number of responses to the
survey was 12; 8 of the people who responded also attended the workshop.

**GOES R+ Energetic Particle Workshop Questionnaire**

**1. Select the category that best describes you as a current user of
GOES energetic particle (EP) data.**

**\_Government**

**\_Military**

**\_University/educational institution**

**\_Commercial/business**

**\_Other**

**2. For what purpose do you use the GOES EP data?**

**\_Science research**

**\_Situational awareness of the space environment**

**\_As input to space weather models**

**\_Other**

**3. Do you know of a need to measure the following on the GOES R+
platforms?**

**Energetic heavy nuclei - indicate mass resolution and desired energy
range of measurements**

  --------------------- ------------------------- -----------------------
  **No**                                          

  **If Yes, specify:**  **Mass resolution**       **Energy coverage
                                                  (MeV/n)**

                        **Coarse element groups   **Minimum**
                        (CNO, Ne-S, Fe)**         

                        **Resolve all even-Z      **Maximum**
                        elements**                
  --------------------- ------------------------- -----------------------

**Pitch angle resolution - indicate species, energy range, and angular
resolution**

  --------------------- ------------------------ ------------------------
  **No**                                         

  **If Yes, specify:**  **species**              **Energy coverage
                                                 (MeV/n)**

                        **ions**                 **Minimum**

                        **electrons**            **Maximum**
  --------------------- ------------------------ ------------------------

**Particles at energies below \~30 keV:**

  -------------------------------- --------------------------------------
  **No**                           

  **If Yes, specify:**             **species**

                                   **ions**

                                   **electrons**
  -------------------------------- --------------------------------------

**4. Which best describes the bulk of your access to the current suite
of GOES EP measurements?**

**\_Near-real time**

**\_Archival**

**5. What do you think are the significant limitations of GOES EP data?
Indicate all that apply.**

**\_Energy range**

**\_Time resolution**

**\_Energy resolution**

**\_Ion composition**

**\_Pitch angle coverage**

**6. Rate your satisfaction with current GOES EP measurements.**

**\_Highly satisfied**

**\_Satisfied**

**\_Indifferent**

**\_Dissatisfied**

**\_Highly dissatisfied**

**7. Other comments or suggestions.**

The responses to the questionnaires mostly reflected the opinions in the
workshop presentations and discussions because of the significant number
of respondents who also attended the workshop. The following tables
compile the answers to the questionnaire, each followed by a summary
finding. Note the percentages refer to the fraction out of 12. Not all
questions were answered fully.

+---------------------+---------------+----------+----------+----------+
| Question            | Number of     | Coarse   | Resolve  | Typical  |
|                     | respondents   | mass     | all      | energy   |
|                     | who saw a     | re       | even-Z   | ranges   |
|                     | need for this | solution | ions     | (MeV/n)  |
|                     | measurement   | (CNO,    |          |          |
|                     |               | Ne-S,    |          |          |
|                     |               | Fe)      |          |          |
+---------------------+---------------+----------+----------+----------+
| Need for            | 9 (75%)       | 7 (58%)  | 2 (17%)  | 30-400   |
| measurements of     |               |          |          |          |
| energetic heavy     |               |          |          | 0.02-0.6 |
| nuclei              |               |          |          |          |
|                     |               |          |          | 20-1000  |
|                     |               |          |          |          |
|                     |               |          |          | 10-200+  |
+---------------------+---------------+----------+----------+----------+

**Summary finding: Most respondents (75%) saw a need for Z≥2**
**measurements. Most were also satisfied with coarse mass resolution of
the heavy ions in the energy range from \~ 10 to a few hundred
MeV/nucleon.**

+----------+---------------+----------+----------+----------+----------+
| Question | Number of     | Ions     | E        | Typical  | Typical  |
|          | respondents   |          | lectrons | energy   | pitch    |
|          | who saw a     |          |          | ranges   | angle    |
|          | need for this |          |          |          | re       |
|          | measurement   |          |          | (MeV)    | solution |
|          |               |          |          |          | (        |
|          |               |          |          |          | degrees) |
+----------+---------------+----------+----------+----------+----------+
| Pitch    | 10 (83%)      | 7 (58%)  | 8 (67%)  | 0.01-1   | 5-36     |
| angle    |               |          |          | *ions*   |          |
| re       |               |          |          |          |          |
| solution |               |          |          | 0.01-10  |          |
|          |               |          |          | *e-*     |          |
+----------+---------------+----------+----------+----------+----------+

**Summary finding: Most respondents (83%) wanted pitch angle resolution
for both ions and electrons. The requested resolution varied from
5-degree bins to 36-degree bins. One respondent suggested an
energy-dependent resolution, with only 2 bins for electrons above a few
hundred keV where there are fewer particles.**

+---------------------+---------------+----------+----------+----------+
| Question            | Number of     | Ions     | E        | Typical  |
|                     | respondents   |          | lectrons | energy   |
|                     | who saw a     |          |          | range    |
|                     | need for this |          |          | (from    |
|                     | measurement   |          |          | one      |
|                     |               |          |          | res      |
|                     |               |          |          | pondent) |
|                     |               |          |          |          |
|                     |               |          |          | (keV)    |
+---------------------+---------------+----------+----------+----------+
| Particles below 30  | 7 (58%)       | 5 (42%)  | 6 (50%)  | 0.03-30  |
| keV                 |               |          |          |          |
+---------------------+---------------+----------+----------+----------+

**Summary finding: Most respondents (58%) wanted to extend the GOES
capability below 30 keV for both electrons and ions.**

  --------------------- --------- ------------ ------------ -------------- ----------
  Question              Energy    Time         Energy       Ion            Pitch
                        range     resolution   resolution   comp-osition   angle
                                                                           coverage

  Significant           6 (50%)   3 (25%)      9 (75%)      6 (50%)        7 (58%)
  limitations of                                                           
  current GOES EP                                                          
  measurements                                                             
  --------------------- --------- ------------ ------------ -------------- ----------

**Summary finding: Over 50% of the respondents thought there are
limitations in GOES energy range & resolution, ion composition, and
pitch angle coverage. The time resolution of the GOES data was not a
significant limitation.**

  --------------------- ----------- ----------- ------------- -------------- -------------- ---------
  Question              Highly      Satisfied   Indifferent   Dissatisfied   Highly         No
                        satisfied                                            dissatisfied   comment

  Rate your             0 (0%)      4 (33%)     4 (33%)       3 (25%)        0 (0%)         1 (8%)
  satisfaction with                                                                         
  current GOES EP                                                                           
  measurements                                                                              
  --------------------- ----------- ----------- ------------- -------------- -------------- ---------

**Summary finding: There was roughly an equal mix of respondents who
were satisfied, indifferent, or dissatisfied with the current GOES
particle measurements.**

# Appendix 2. Summary of workshop presentations

Sources: presentations as forwarded to the workshop reporter,
reporter\'s notes during the presentations and during the workshop
discussions

Criterion for listing in the table: specific recommendations for GOES R+
above and beyond the requirements for GOES I-M and N-Q

+-------------+-------------+-------------+-------------+-------------+
| *           | **          | **Protons** | **Z≥2**     | **Comments  |
| *Presenter( | Electrons** |             |             | on          |
| s)/source** |             |             |             | a           |
|             |             |             |             | vailability |
|             |             |             |             | of GOES     |
|             |             |             |             | data and    |
|             |             |             |             | environment |
|             |             |             |             | models**    |
+-------------+-------------+-------------+-------------+-------------+
| Joe Fennell | -   Extend  | 1-100 keV H | -   1-100   | -   GOES    |
|             |     m       | for surface |     keV O+  |             |
|             | easurements | damage      |     for     |  spacecraft |
|             |     down to | environment |     surface |     are     |
|             |     1 keV   |             |     damage  |             |
|             |     for     |             |             | \"gateway\" |
|             |     surface |             | environment |     to the  |
|             |             |             |             |     ma      |
|             |    charging |             | -   Simple  | gnetosphere |
|             |             |             |     LET     |             |
|             | environment |             |     sensor  | -   Near    |
|             |             |             |     to      |             |
|             | -   Option: |             |     monitor |   real-time |
|             |             |             |     energy  |     data    |
|             |    separate |             |     deposit |     from    |
|             |     surface |             |     from    |     GOES    |
|             |             |             |     high    |     are     |
|             |    charging |             |     energy  |             |
|             |     monitor |             |     solar   |    critical |
|             |             |             |     and     |     for     |
|             |             |             |             |     space   |
|             |             |             |    galactic |             |
|             |             |             |             | situational |
|             |             |             |   particles |             |
|             |             |             |             |   awareness |
+-------------+-------------+-------------+-------------+-------------+
| Mike        |             | Protons     | Heavy-ions  | Nea         |
| Golightly   |             | from10 to   | relevant    | r-real-time |
|             |             | 500 MeV     | for         | data        |
|             |             | most        | s           | a           |
|             |             | significant | ingle-event | vailability |
|             |             | for human   | effects on  | critical to |
|             |             | bio damage  | some ISS    | ISS support |
|             |             |             | subsystems  |             |
+-------------+-------------+-------------+-------------+-------------+
| Kyle Miller |             |             | -           | Need        |
|             |             |             | Measurement | validated   |
|             |             |             |     of LET  | models of   |
|             |             |             |     in      | worst-case, |
|             |             |             |     range   | typical,    |
|             |             |             |     of      | and total   |
|             |             |             |             | solar       |
|             |             |             |    \~10-100 | particle    |
|             |             |             |     M       | fluence     |
|             |             |             | eV/mg-cm^2^ | focused on  |
|             |             |             |     rather  | effects on  |
|             |             |             |     than    | space       |
|             |             |             |             | systems     |
|             |             |             |  individual | (e.g.       |
|             |             |             |     species | energy      |
|             |             |             |             | deposit, or |
|             |             |             | -   Z≥2 not | LET)        |
|             |             |             |     used in |             |
|             |             |             |     total   |             |
|             |             |             |     dose    |             |
|             |             |             |     c       |             |
|             |             |             | alculations |             |
|             |             |             |     at      |             |
|             |             |             |     present |             |
+-------------+-------------+-------------+-------------+-------------+

+-------------+-------------+-------------+-------------+-------------+
| Mike Bodeau | Spectra     | 1- 100 keV  |             | -   Need    |
|             | over \~10   | for         |             |             |
|             | -100 keV    | spacecraft  |             |   long-term |
|             | for         | design      |             |     data    |
|             | analysis of | (e.g. solar |             |     archive |
|             | surface     | arrays)     |             |     &       |
|             | charging    |             |             |     models  |
|             | environment |             |             |     of      |
|             | in GEO      |             |             |     plasma  |
|             | longitudes  |             |             |             |
|             | over CONUS  |             |             | environment |
|             |             |             |             |     at GEO  |
|             |             |             |             |             |
|             |             |             |             | -   Not     |
|             |             |             |             |     many    |
|             |             |             |             |     data on |
|             |             |             |             |     GEO     |
|             |             |             |             |     surface |
|             |             |             |             |             |
|             |             |             |             |    charging |
|             |             |             |             |             |
|             |             |             |             | environment |
|             |             |             |             |     for     |
|             |             |             |             |             |
|             |             |             |             |  satellites |
|             |             |             |             |     over    |
|             |             |             |             |     CONUS   |
+-------------+-------------+-------------+-------------+-------------+
| Dave        |             |             | -   High-Z  | GOES data   |
| Chenette    |             |             |     solar   | valuable    |
|             |             |             |             | because of  |
|             |             |             |    particle | easy access |
|             |             |             |             | to near     |
|             |             |             | composition | real-time   |
|             |             |             |     poorly  | data and    |
|             |             |             |             | long-term,  |
|             |             |             |   specified | consistent  |
|             |             |             |     in      | archive     |
|             |             |             |     models  |             |
|             |             |             |     (e.g.   |             |
|             |             |             |             |             |
|             |             |             |  worst-case |             |
|             |             |             |     flux of |             |
|             |             |             |             |             |
|             |             |             |  heavy-ions |             |
|             |             |             |             |             |
|             |             |             |    probably |             |
|             |             |             |             |             |
|             |             |             |   uncertain |             |
|             |             |             |     by      |             |
|             |             |             |     factor  |             |
|             |             |             |     of 10)  |             |
|             |             |             |             |             |
|             |             |             | -   Desire  |             |
|             |             |             |     Z≥2     |             |
|             |             |             |             |             |
|             |             |             | composition |             |
|             |             |             |     and     |             |
|             |             |             |             |             |
|             |             |             |    spectra, |             |
|             |             |             |             |             |
|             |             |             |   10-100\'s |             |
|             |             |             |             |             |
|             |             |             | MeV/nucleon |             |
+-------------+-------------+-------------+-------------+-------------+
| Janet Barth |             |             | -           |             |
| & Mike      |             |             | Recommended |             |
| Xapsos      |             |             |     new     |             |
|             |             |             |             |             |
|             |             |             |  instrument |             |
|             |             |             |     to      |             |
|             |             |             |     monitor |             |
|             |             |             |     LET up  |             |
|             |             |             |     to      |             |
|             |             |             |     \~100   |             |
|             |             |             |             |             |
|             |             |             |  MeV/mg-cm2 |             |
|             |             |             |             |             |
|             |             |             |   (includes |             |
|             |             |             |     Z≥2     |             |
|             |             |             |     ions)   |             |
|             |             |             |             |             |
|             |             |             | -           |             |
|             |             |             |   Advantage |             |
|             |             |             |     of      |             |
|             |             |             |     direct  |             |
|             |             |             |             |             |
|             |             |             | measurement |             |
|             |             |             |     of      |             |
|             |             |             |     energy  |             |
|             |             |             |     deposit |             |
|             |             |             |     behind  |             |
|             |             |             |             |             |
|             |             |             |  spacecraft |             |
|             |             |             |             |             |
|             |             |             |   shielding |             |
+-------------+-------------+-------------+-------------+-------------+
| Tom Carey   | -   Few eV  | -   0.3 to  | 1-100 keV   |             |
|             |     to \~50 |     -\>500  | O+          |             |
|             |     keV     |     MeV     | r           |             |
|             |     with 10 |             | ing-current |             |
|             |     to 40   | -   biggest | composition |             |
|             |     energy  |     need is | for surface |             |
|             |             |             | effects     |             |
|             |    channels |    improved |             |             |
|             |             |             |             |             |
|             | -   0.3-10  |    spectral |             |             |
|             |     MeV:    |             |             |             |
|             |     biggest |  resolution |             |             |
|             |     need is |     (5 or   |             |             |
|             |             |     more    |             |             |
|             |    improved |     d       |             |             |
|             |             | ifferential |             |             |
|             |    spectral |             |             |             |
|             |             |   channels) |             |             |
|             |  resolution |             |             |             |
|             |     (4 or   |             |             |             |
|             |     more    |             |             |             |
|             |     d       |             |             |             |
|             | ifferential |             |             |             |
|             |             |             |             |             |
|             |   channels) |             |             |             |
+-------------+-------------+-------------+-------------+-------------+
| Steve       |             | Optimize    |             | GOES solar  |
| Kahler      |             | energy      |             | particle    |
|             |             | channels    |             | m           |
|             |             | for a       |             | easurements |
|             |             | typical E-2 |             | essential   |
|             |             | solar       |             | for         |
|             |             | particle    |             | research    |
|             |             | spectrum (  |             |             |
|             |             | to ensure   |             |             |
|             |             | sufficient  |             |             |
|             |             | statistics  |             |             |
|             |             | in each     |             |             |
|             |             | channel at  |             |             |
|             |             | high        |             |             |
|             |             | energy)     |             |             |
+-------------+-------------+-------------+-------------+-------------+
| Stephan     | 30 eV to    |             |             |             |
| Quigley     | 100 keV for |             |             |             |
|             | surface     |             |             |             |
|             | charging    |             |             |             |
|             | sp          |             |             |             |
|             | ecification |             |             |             |
+-------------+-------------+-------------+-------------+-------------+
| Myron       | 1 eV to 100 |             |             | GOES        |
| Mandell     | keV with    |             |             | low-energy  |
|             | 10\'s of    |             |             | electron    |
|             | channels    |             |             | data would  |
|             | (capability |             |             | be used to  |
|             | similar to  |             |             | develop     |
|             | LANL        |             |             | ass         |
|             | mag         |             |             | et-specific |
|             | netospheric |             |             | models of   |
|             | particle    |             |             | spacecraft  |
|             | analyzer    |             |             | charging    |
|             | instrument) |             |             | for design  |
|             |             |             |             | and         |
|             |             |             |             | in-fight    |
|             |             |             |             | analysis    |
+-------------+-------------+-------------+-------------+-------------+
| Dave Sibeck | -   20 keV  | -   20 -    | -   20 -    | Improve     |
|             |     to 10   |     600 keV |     600 keV | a           |
|             |     MeV     |     H+ with |     O+ with | vailability |
|             |     with    |     full    |     full    | of          |
|             |     full    |     pitch   |     pitch   | high-time   |
|             |     pitch   |     angle   |     angle   | resolution  |
|             |     angle   |             |             | m           |
|             |             |  resolution |  resolution | agnetometer |
|             |  resolution |             |             | data        |
|             |             | -   if      | -   if      |             |
|             | -   if      |             |             |             |
|             |             |    complete |    complete |             |
|             |    complete |     pitch   |     pitch   |             |
|             |     pitch   |     angle   |     angle   |             |
|             |     angle   |             |             |             |
|             |             |  resolution |  resolution |             |
|             |  resolution |     not     |     not     |             |
|             |     not     |             |             |             |
|             |             |   possible, |   possible, |             |
|             |   possible, |             |             |             |
|             |             |    restrict |    restrict |             |
|             |    restrict |     FOV to  |     FOV to  |             |
|             |     FOV to  |             |             |             |
|             |             |  equatorial |  equatorial |             |
|             |  equatorial |     pitch   |     pitch   |             |
|             |     pitch   |     angles  |     angles  |             |
|             |     angles  |             |             |             |
+-------------+-------------+-------------+-------------+-------------+

# 

# Appendix 3. Attendance list distributed on October 28, 2002. 

Total attendance = 27.

  ---------- ------------ ----------------- -------------- -----------------------------------
  **Name**                **Institution**   **Phone**      **Email address**

  Michael    Bodeau       Boeing Satellite  310-416-6928   <Michael.bodeau@boeing.com>
                          Systems                          

  Pat        Bornmann     Ball Aerospace    303-939-5833   <Pbornmann@ball.com>

  Tom        Carey        Los Alamos        505-667-1239   <Tcarey@lanl.gov>
                          National Lab                     

  Thomas     Cayton       Los Alamos        505-665-2582   <Tcayton@lanl.gov>
                          National Lab                     

  David      Chenette     Lockheed Martin   650-424-3449   <Dave.chenette@lmco.com>
                          ATC                              

  Stephen W. Dandt        Ball Aerospace    303-939-5023   <Sdandt@ball.com>

  Gerald     Dittberner   NOAA/NESDIS       301-457-5125   <Gerald.dittberner@noaa.gov>
                                            x113           

  Jim        Eraker       Ball Aerospace    303-939-5655   <Jeraker@ball.com>
                          BATC                             

  Joe        Fennell      The Aerospace     310-336-7075   <Joseph.fennell@aero.org>
                          Corporation                      

  Howard     Garcia       NOAA/SEC          303-497-3916   <Howard.a.garcia@noaa.gov>

  Michael    Golightly    NASA/JSC          281-483-6190   <Mgolight@ema.jsc.nasa.gov>

  George     Ho           JHU/APL           240-228-7083   <George.ho@jhuapl.edu>

  Stephen W. Kahler       AFRL/VSBXS        781-377-9665   <Stephen.kahler@hanscom.af.mil>

  Xinlin     Li           University of     303-492-3514   <Lix@lasp.colorado.edu>
                          Colorado/LASP                    

  Myron      Mandell      SAIC              858-826-1622   <Myron.mandell@saic.com>

  Joe        Mazur        The Aerospace     310-336-2389   <Joseph.mazur@aero.org>
                          Corporation                      

  Kyle       Miller       Mission Research  719-237-4703   <Kimller@mrcll.com>
                          Corporation                      

  Joe        Mobilia      Lockheed Martin   650-424-3292   <Joseph.mobilia@lmco.com>
                          ATC                              

  Bill       Murtagh      OL-P/AFWA USAF    303-497-7492   <William.murtagh@noaa.gov>

  Neal       Nickles      Ball Aerospace    303-939-4783   <Nnickles@ball.com>

  Terry      Onsager      NOAA/SEC          303-497-5713   <Terry.onsager@noaa.sec>

  Ahmet      Ozkul        INTELSAT          202-944-7334   <Ahmet.ozkul@intelsat.com>

  Bob        Prochaska    Raytheon          719-637-7089   <Robert_d_prochaska@raytheon.com>

  Stephen    Quigley      AFRL/VSBX         719-556-2889   <Stephen.quigley@cisf.af.mil>

  David      Sibeck       NASA/GSFC         301-286-5998   <David.sibeck@gsfc.nasa.gov>

  Howard     Singer       NOAA/SEC          303-497-6959   <Howard.singer@noaa.gov>

  Zdenka     Smith        NOAA/SEC          303-497-3473   <Zdenka.smith@noaa.gov>

  Ron        Zwickl       NOAA/SEC          303-497-3029   <Ron.d.zwickl@noaa.gov>
  ---------- ------------ ----------------- -------------- -----------------------------------

![](media/image9.png){width="6.5in" height="4.51875in"}

Figure A1. Representation of different institutions at the workshop: gov
= US government, mil = US military, edu = educational, com = commercial.

# Appendix 4. Workshop schedule.

**GOES R+ Energetic Particles Workshop**

Monday-Tuesday, October 28 - 29 2002

NOAA

David Skaggs Research Center

325 Broadway

Boulder, CO

Room 2A305

Phone: 303-497-3113

Schedule summary:

Monday, October 28, 2002

  ------------------------------ ----------------------------------------
  09:00 - 10:30                  Session 1

  10:30 - 11:00                  Coffee break

  11:00 - 12:00                  Session 2

  12:00 - 13:00                  Lunch break

  13:00 - 15:00                  Session 3

  15:00 - 15:30                  Coffee break

  15:30 - 17:00                  Session 4
  ------------------------------ ----------------------------------------

Tuesday, October 29, 2002

  ------------------------------ ----------------------------------------
  09:00 - 12:00                  Session 1

  ------------------------------ ----------------------------------------

Breakfast:

A light breakfast will be served every morning from 08:00-09:00 outside
room GC402, one floor down from the entrance area to the David Skaggs
Research Center.

Presentations:

The times and order of the presentations are flexible. We have allocated
20-30 minutes per talk, including at least 5 minutes of discussion.

NOAA will provide overhead projectors and computer projectors. There
will also be a laptop for running Powerpoint charts (bring presentations
on a CD-ROM if you choose to use this method).

Joe Mazur and Terry Onsager will ask for copies of the presentations.
Either hardcopy at the meeting or electronic files sent via email after
the meeting are acceptable.

+------+-----------------------------------+---------------------------+
| *    |                                   |                           |
| *Mon |                                   |                           |
| day, |                                   |                           |
| Oct  |                                   |                           |
| ober |                                   |                           |
| 28,  |                                   |                           |
| 20   |                                   |                           |
| 02** |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
| *    |                                   |                           |
| *Wel |                                   |                           |
| come |                                   |                           |
| &    |                                   |                           |
| work |                                   |                           |
| shop |                                   |                           |
| ov   |                                   |                           |
| ervi |                                   |                           |
| ew** |                                   |                           |
+------+-----------------------------------+---------------------------+
| 0    | Welcome & local arrangements      | Terry Onsager/NOAA        |
| 9:00 |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
| 0    | Workshop goals                    | Terry Onsager/NOAA        |
| 9:10 |                                   |                           |
|      |                                   | Joe Mazur/The Aerospace   |
|      |                                   | Corporation               |
+------+-----------------------------------+---------------------------+
| 0    | Energetic particle sensors on the | Terry Onsager/NOAA        |
| 9:20 | current GOES spacecraft           |                           |
+------+-----------------------------------+---------------------------+
| 0    | Overview of the impact of the     | Joe Mazur/The Aerospace   |
| 9:30 | space environment on space        | Corporation               |
|      | systems                           |                           |
+------+-----------------------------------+---------------------------+
| **E  |                                   |                           |
| nerg |                                   |                           |
| etic |                                   |                           |
| part |                                   |                           |
| icle |                                   |                           |
| mea  |                                   |                           |
| sure |                                   |                           |
| ment |                                   |                           |
| re   |                                   |                           |
| quir |                                   |                           |
| emen |                                   |                           |
| ts** |                                   |                           |
+------+-----------------------------------+---------------------------+
| 1    | 3^rd^ generation GOES spacecraft  | Mike Golightly/NASA       |
| 0:00 | program: billions of              | Johnson Space Center      |
|      | dollars...GOES energetic particle |                           |
|      | measurements for support of       |                           |
|      | manned spaceflight: priceless     |                           |
+------+-----------------------------------+---------------------------+
| 1    | Break                             |                           |
| 0:30 |                                   |                           |
+------+-----------------------------------+---------------------------+
| 1    | The charged particle environment  | Kyle Miller/Mission       |
| 1:00 | from a spacecraft designer\'s     | Research Corporation      |
|      | perspective                       |                           |
+------+-----------------------------------+---------------------------+
| 1    | What do satellite manufacturers   | Mike Bodeau/Boeing        |
| 1:20 | want from GOES?                   |                           |
+------+-----------------------------------+---------------------------+
| 1    | On-orbit space systems users      | Dave Chenette/Lockheed    |
| 1:40 | requirements for GOES energetic   | Martin Advanced           |
|      | particle data: a perspective from | Technology Center         |
|      | Lockheed Martin                   |                           |
+------+-----------------------------------+---------------------------+
| 1    | Lunch                             |                           |
| 2:00 |                                   |                           |
+------+-----------------------------------+---------------------------+
| 1    | SEP measurements required for     | Mike Xapsos/Mike          |
| 3:00 | environment models and system     | Jones/NASA Goddard Space  |
|      | design and testing                | Flight Center             |
+------+-----------------------------------+---------------------------+
| 1    | European Space Agency interests   | Eammon Daly/European      |
| 3:20 | in GOES energetic particle        | Space Agency              |
|      | measurements                      |                           |
+------+-----------------------------------+---------------------------+
| 1    | LANL perspectives on space        | Tom Carey/Los Alamos      |
| 3:40 | environment monitoring            | National Laboratory       |
+------+-----------------------------------+---------------------------+
| 1    | Air Force requirements for        | Maj. Pete Engelman/USAF   |
| 4:00 | energetic particle measurements   |                           |
+------+-----------------------------------+---------------------------+
| 1    | Air Force Research Laboratory     | Steve Kahler/Air Force    |
| 4:20 | perspective on energetic particle | Research Laboratory       |
|      | measurements                      |                           |
+------+-----------------------------------+---------------------------+
| 1    | Proposed space environmental      | Stephan Quigley/Air Force |
| 4:40 | effects on satellite operations   | Research Laboratory       |
|      | (SEESO) product                   |                           |
+------+-----------------------------------+---------------------------+
| 1    | Break                             |                           |
| 5:00 |                                   |                           |
+------+-----------------------------------+---------------------------+
| 1    | Let\'s not forget surface         | Joe Fennell/ The          |
| 5:30 | charging                          | Aerospace Corporation     |
+------+-----------------------------------+---------------------------+
| 1    | The case for low-energy electrons | Myron Mandell/ Science    |
| 5:50 |                                   | Applications              |
|      |                                   | International Corporation |
+------+-----------------------------------+---------------------------+
| 1    | General discussion                | All                       |
| 6:10 |                                   |                           |
+------+-----------------------------------+---------------------------+
| 1    | Adjourn                           |                           |
| 7:00 |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
| **   |                                   |                           |
| Tues |                                   |                           |
| day, |                                   |                           |
| Oct  |                                   |                           |
| ober |                                   |                           |
| 29,  |                                   |                           |
| 20   |                                   |                           |
| 02** |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
| *    |                                   |                           |
| *Int |                                   |                           |
| erag |                                   |                           |
| ency |                                   |                           |
| coor |                                   |                           |
| dina |                                   |                           |
| tion |                                   |                           |
| and  |                                   |                           |
| rese |                                   |                           |
| arch |                                   |                           |
| p    |                                   |                           |
| ersp |                                   |                           |
| ecti |                                   |                           |
| ve** |                                   |                           |
+------+-----------------------------------+---------------------------+
| 0    | Geospace and NASA\'s Living With  | Dave Sibeck/ NASA Goddard |
| 9:00 | a Star program                    | Space Flight Center       |
+------+-----------------------------------+---------------------------+
| 0    | Space Environment Sensor Suite    | Pat Bornmann/ Ball        |
| 9:20 | for NPOESS                        | Aerospace and             |
|      |                                   | Technologies Corporation  |
+------+-----------------------------------+---------------------------+
| 0    | Measurements needed to improve    | Xinlin Li/ University of  |
| 9:40 | forecast and specification of     | Colorado Laboratory for   |
|      | energetic electrons               | Atmospheric and Space     |
|      |                                   | Physics                   |
+------+-----------------------------------+---------------------------+
| 1    | General discussion of priorities  | All                       |
| 0:00 | for energetic particle            |                           |
|      | measurements including:           |                           |
|      |                                   |                           |
|      | 1\. Needs and requirements for    |                           |
|      | heavy ion measurements (species,  |                           |
|      | energy ranges, mass resolution,   |                           |
|      | etc.)                             |                           |
|      |                                   |                           |
|      | 2\. Needs and requirements for    |                           |
|      | low-energy electron measurements. |                           |
|      |                                   |                           |
|      | 3\. Additional modifications that |                           |
|      | could enhance the value of the    |                           |
|      | energetic particle data.          |                           |
|      |                                   |                           |
|      | 4\. Existing technologies that    |                           |
|      | can make these measurements at    |                           |
|      | reasonable cost.                  |                           |
+------+-----------------------------------+---------------------------+
| 1    | Adjourn                           |                           |
| 2:00 |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+
|      |                                   |                           |
+------+-----------------------------------+---------------------------+