MONDAY 24 October, 2005

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AMS Technical Interchange Meeting CERN -
Geneva, Council Chamber 24 - 28 October,
2005 Preliminary AGENDA vs 4
MONDAY 24 October, 2005 0800-0900 Report to
the Collaboration Samuel C.C. Ting 0900-0915
Phase-II flight Safety Review Data Package Trent
Martin 0915-0930 AMS Quality Management
Plan John Stanford 0930-0945 coffee,
tea 0945-1145 Report on the AMS-02
Tracker Roberto Battiston et al., 1145-1215
On-orbit Operations Proposed Changes Paul
Nemeth 1215-1400 Lunch 1400-1800 Individual
group meetings
TUESDAY 25 October, 2005 0800-0830 NASA
Status Stephen Porter 0830-1030 Transition
Radiation Detector Stefan Schael, Klaus
Lübelsmeyer, Ulrich Becker et al., 1030-1045
Coffee, tea 1045-1200 Tracker Thermal Control
System J. van Es, He Zhenhui et al, 1200-1300
Status of Thermal Control System Joe Burger,
Marco Molina 1300-1400 Lunch 1400-1800
Individual group meetings
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WEDNESDAY 26 October, 2005 0800-0900 Report on
RICH Giuliano Laurenti et al., 0900-1000
Report on Scintillation Counters TOF and
ACC Federico Palmonari, Wolfgang Wallraff et
al., 1000-1015 Coffee, tea 1015-1145
Report on ECAL Franco Cervelli et
al, 1145-1215 Integration at CERN Robert
Becker, Trent Martin 1215-1400
Lunch 1400-1800 Individual group meetings
THURSDAY 27 October, 2005 0800-1000 AMS
Magnet New contracts Status Stephen Porter,
H. Hofer, S. Ting, S. Harrison 1000-1015 Coffee,
tea 1015-1200 Report on AMS Electronics Mike
Capell, Alexei Lebedev et al., P. Dennett
(including ACOP) 1200-1215 Weight
Summary Andrei Kounine 121501230
Remarks Samuel C.C. Ting 1230-1400
Lunch 1400-1430 Report on GPS
integration Claude Zurbach 1430-1500 Report on
Flight Software Andrei Kounine 1500-1530
Report on Ground Computing Vitali Choutko,
Alexander Eline et al., 1530-1545 Coffee,
tea 1545-1615 Report on AMS Analysis
Software Juan Alcaraz 1615-1715 Report on AMS
MOU Manuel Aguilar-Benitez
FRIDAY 28 October, 2005 0800-1800 Individual
Group Meetings Trent Martin
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Report to the Collaboration
The AMS Experiment
AMS
S.C.C. Ting
October 24-28, 2005
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Welcome Dr. Simona Di PippoDirector,
Observation of the Universe, Italian Space
Agency (ASI)
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Welcome CASTChina Academy of Space Technology
Professor Yin Liming, Vice President
Professor Yan Zhongwen, Deputy Director, System
Engineering Dept.
Professor Hou Zengqi
Professor Han Bo
Professor Zhong Qi
Professor Ding Xiaobo, Deputy Director, Intl
Marketing Coop. Div.
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Please switch off your mobile phone !If you
must use a computer,please sit in the last
rowso that you do not affect others.
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TIM issues of July 2005

• ECAL Test of Brick
• TCS Overweight of 40 kg
• CAB 12 kg
• Total Magnet weight?

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TIM issues of July 2005
TOTAL Magnet Weight?
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Report to Dr. Michael Griffin NASA Administrator
The Alpha Magnetic Spectrometer Experiment (AMS)
and Space Exploration
AMS
S.C.C. Ting
5 October 2005
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Dr. Raymond L. Orbach, Director, Office of
Science, Dept. of Energy
Distinguished research in theoretical and
experimental physics - more than 240
publications. Former Chancellor, UC
Riverside.Oversees research in high energy and
nuclear physics, basic energy sciences, magnetic
fusion energy, biological and environmental
research and computational science.
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Dr. Robin Staffin, Director, Office of High
Energy Physics, Assoc. Director, Office of
Science, DOE
Oversees most of the US High Energy Physics
programs including accelerator laboratories (BNL,
FNAL, ANL, SLAC, LBNL, and others).Also
oversees most of the US participation in
international collaborations at CERN, Desy Is
also responsible for NASA-DOE collaborations
GLAST, AMS
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Member of the Royal Spanish Academy of Sciences,
Director of Basic Research, CIEMAT (Spanish
National Laboratory for Energy, Technology and
Basic Research), responsible for the AMS Ring
Imaging Cerenkov Counter (RICH) detector.
Dr. Manuel Aguilar
Dr. Roberto Battiston
Director, INFN, Perugia, Italy, leader of the AMS
silicon tracker system.
President, Space Cryomagnetics Ltd, Oxfordshire,
England, a worlds leading expert in
superconducting magnets.
Mr. Stephen Harrison
Dr. Shih-Chang Lee
Member of Academia Sinica, Taiwan, responsible
for AMS electronics.
Director of the First Institute of Physics, RWTH
Aachen, Germany, responsible for the AMS
Transition Radiation Detector (TRD).
Dr. Stephan Schael
Member of the National Academy of Sciences,
Donner Professor of Physics, Yale University,
Editor, Physical Review Letters.
Dr. Jack Sandweiss
Mr. Stephen Porter
AMS Project Manager, NASA-JSC/EA
Dr. Samim Anghaie
University of Florida, a leading expert on space
nuclear power.
Dr. Robert Silbey
Dean of Science of M.I.T., Member of the National
Academy of Sciences.
Dr. Mike Capell
AMS Avionics Coordinator.
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Outline (of presentation to M. Griffin)

• Introduction to AMS Physics
• International Participation
• AMS-01 Physics Results
• AMS-02 Development of Superconducting
• Magnet Technology and Precision Detectors
• Physics Potential of AMS-02
• Reviews of AMS
• Application of AMS Technology to Exploration
• A selected sample of the slides presented follows

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Physics of AMS
Cosmic rays
Light rays and neutrinos

• Nobel Prizes,
• Pulsar,
• Microwave,
• Binary Pulsars,
• (4) X Ray sources

AMS will perform accurate measurements of
energetic charged cosmic rays (0.2 GeV/n to 2
TeV/n) and high energy gamma rays (0.5 GeV to
300 GeV)
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AMS A TeV (1012 eV) Magnetic Spectrometer in
Space 3m x 3m x 3m, 7t, 0.5m2 sr
The AMS detector has been under construction for
10 years.
y03K193_2ea
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International Participation in AMS
FINLAND
RUSSIA
HELSINKI UNIV. UNIV. OF TURKU
I.K.I. ITEP KURCHATOV INST. MOSCOW STATE UNIV.
DENMARK
UNIV. OF AARHUS
NETHERLANDS
GERMANY
ESA-ESTEC NIKHEF NLR
RWTH-I RWTH-III MAX-PLANK INST. UNIV. OF KARLSRUHE
KOREA
USA
EWHA KYUNGPOOK NAT.UNIV.
AM FLORIDA UNIV. JOHNS HOPKINS UNIV. MIT -
CAMBRIDGE NASA GODDARD SPACE FLIGHT CENTER NASA
JOHNSON SPACE CENTER UNIV. OF MARYLAND-DEPRT OF
PHYSICS UNIV. OF MARYLAND-E.W.S. S.CENTER YALE
UNIV. - NEW HAVEN
FRANCE
ROMANIA
CHINA
BISEE (Beijing) IEE (Beijing) IHEP (Beijing) SJTU
(Shanghai) SEU (Nanjing) SYSU (Guangzhou) SDU
(Jinan)
GAM MONTPELLIER LAPP ANNECY LPSC GRENOBLE
ISS UNIV. OF BUCHAREST
SWITZERLAND
ETH-ZURICH UNIV. OF GENEVA
TAIWAN
SPAIN
CIEMAT - MADRID I.A.C. CANARIAS.
ITALY
ACAD. SINICA (Taiwan) CSIST (Taiwan) NCU (Chung
Li) NCKU (Tainan) NCTU (Hsinchu) NSPO (Hsinchu)
ASI CARSO TRIESTE IROE FLORENCE INFN UNIV. OF
BOLOGNA INFN UNIV. OF MILANO INFN UNIV. OF
PERUGIA INFN UNIV. OF PISA INFN UNIV. OF
ROMA INFN UNIV. OF SIENA
MEXICO
UNAM
PORTUGAL
LAB. OF INSTRUM. LISBON
16 Countries, 56 Institutes, 500 Physicists
95 of AMS is constructed in Europe and
Asia Supported by ministries of
science/education/energy, space agencies, local
goverments and universities
Y96673-05_1Commitment
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First flight AMS-01
Approval April 1995, Assembly December 1997,
Flight June 1998
AMS
y96207_05b
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Tracing the origin of cosmic rays from precision
measurements of incident momentum vector and
location
Run/Event 897171331/310063 06-Jun-98 223348
Lat/Long 50N/27W
Side Views
Top View
RE
AMS-01/STS-91
Earths radii RE
RE
RE
Earths radii RE
RE
Primary proton, EK 516 MeV, Measured at RE
1.06 , traced back to RE gt 8
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Helium in Near Earth Orbit
(Mass of He4 3.7 GeV He3 2.8 GeV)
Helium spectrum
80
102
He4
3.650.09
70
He4
10
Rigidity (GV)
60
He3
50
1
Events
0
-0.4
0.4
0.8
-0.8
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Magnetic Latitude (rad)
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2.860.04
He3
40
20
30
Events
10
20
10
0
10 (GeV)
5
1
2
3
4
5
6
0
Physics Letters B vol.494 (3-4) (2000) p.193-202.
Mass (GeV)
Referee report This paper is an exciting and
important paper again from the AMS Collaboration.
It should be published.
AMS-01 results were not predicted by any cosmic
ray model
y99089_05.ppt
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Flight Vacuum Case at JSC
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Flight superconducting magnet coils are fully
assembled

• Volume 35 cu. ft.,
• Field 8,600 Gauss,
• Weight 1 ton

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Russian Participation in the AMS Magnet
The Russians are supporting the magnet
cryo-system by providing 5.1M and 332 man-years
for work in Switzerland, Germany and the UK.
Helium Tank
Vacuum Tank
Reporting twice yearly to Minister A.
RumyantsevMinister of Atomic Energy (Federal
Agency of Atomic Energy)
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Transition Radiation Detector (TRD)
Distinguishes electrons and positrons from all
other particles
Coordinators S.Schael, RWTH U.Becker, MIT
V0.99999C
20 mm
One of 20 layers
Radiator
6 mm
Xe/CO2
5248 tubes L(max) 1.8m
All Flight Hardware Modules produced. Assembly
complete in 2005.
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Silicon Tracker
Production completed. Test results from
accelerator.
Coord R.Battiston, ASIINFN-Perugia
8 planes 6.6 m2 Largest Silicon Detector with
10 ?m accuracy
y04K513_05
y03K193_03_ca.ppt
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Ring Imaging Cerenkov Counter (RICH)
Coordinator G.Laurenti, INFN-Bologna
Test results at 158 GeV/n
Particle (Z,v)
Radiator
?
? ? velocity v
?
Li
C
He
Ca
O
Reflector
Light (?) intensity ? Z2
10,880 Photon detectors
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RICH Test Beam Results E 158 GeV/n
Z
v/c
Charge measured up to Z 26 (Fe)
Velocity resolution 0.1
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2005 - 2006 Assembly of all Flight Hardware onto
the Superconducting Magnet
TRD
TRD
TOF
Magnet and Tracker
TOF
RICH
ECAL
RICH
Tracker
ECAL
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Antimatter
Matter
2x109 nuclei
Number of events
Nuclear charge
If no antimatter is found gt there is no
antimatter to the edge (1000 Mpc) of universe.
The physics of antimatter in the universe is
based on the existence of a strong Time
Reversal Violation the existence of Baryon Number
Violation (proton decay) Grand Unified
Theory Electroweak Theory This is the main
research topic for the current and next
generation of accelerators world wide
the Foundations of Modern Physics
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2. Dark matter There are many theoretical
suggestions that SUSY particles ??? are at
least part of the Dark matter.
y97089_2a.ppt
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IMPLEMENTING ARRANGEMENT BETWEEN THE DEPARTMENT
OF ENERGY AND THE NATIONAL AERONAUTICS AND SPACE
ADMINISTRATION REGARDING THE ALPHA MAGNETIC
SPECTROMETER IN SPACE PROGRAM

III. RESPONSIBILITIES
1- NASA
NASA provides 3 years on ISS Project Management
(Stephen Porter)
2- DOE
DOE provides Science Management Detector
construction Reviews International collaboration

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Department of Energy - Division of High Energy
Physics Two reviews of AMS, April 2-3, 1995 and
March 15, 1999, by
Professor Robert K. Adair Yale University
Professor Barry C. Barish California
Institute of Technology
Professor Stephen L. Olsen University of Hawaii
Professor Malvin A. Ruderman Columbia University
Professor David N. Schramm University of Chicago
Dr. George F. Smoot Lawrence Berkeley Laboratory
Professor Paul J. Steinhardt University of
Pennsylvania
Members of the National Academy of Sciences
and annual peer reviews by DOE
34
see Appendix 3

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ESA is providing complete TVT, complete EMI test
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The application of superconducting magnet
technology to space exploration can provide

• Accurate data on radiation flux
• Radiation shielding
• Propulsion
• Energy generation
• Energy storage (SMES)

The AMS group is interested in exploration and as
the construction of AMS is nearing completion,
we have invested considerable effort in support
of exploration.
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AMS will provide a permanent galactic cosmic
radiation monitor for all nuclei, for all energy
ranges with 1 accuracy.
Accelerator measurements of AMS-02 detector
Oxygen flux
Energy
Time
Energy (GeV/n)
y04K419_04a.ppt
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Superconducting magnets for radiation protection

• No field outside space ship - For EVA and to
  eliminate torque
• No field inside crew compartment - Safety for
  astronauts

Fe
B0 Outside
Magnet Design and Radiation Dose Computation(5
physicists, 60 weeks)
y04K409
For properties of Superconducting magnet
shielding, see Appendix 6
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Magnetic radiation protection system for Mars
missionby B. Blau, V.Choutko, S. Harrison, A.
Herve, S. Horvarth, H. Hofer, H.P. Marti, I.
Vetlitskiy, et al, (CERN, ETH, MIT, SCL)with
AMS technology
Internal coil support (7.4 ton)
Barrel toroid (8.8 ton)
Coil-to-coil support (1.5 ton)
6.2 tesla
Propulsion, energy and life support
Crew compartment
Ø 5.6 m
Ø 15 m
4.5 m
2 m
0.5 m
1.0 m
Endcap toroid (0.6 ton)
8 m
Superfluid He vessel (0.4 ton vessel 0.7 ton
He)
Thermal shield (7.1 ton)
plus Straps (1.4 ton) Services (2.8 ton)
Weight of complete system 30.7 ton
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Simulation of particles magnetic radiation
protection system
based on 2x109 particles
Endcap toroid
Crew compartment
Crew compartment
Barrel toroid
Solar Flare(side view, 50 MeV proton)
Multiple GCR(end view, including 25 GeV proton)
Using NASA Model BFO Dose Calculation
Magnetic shielding reduces dose from 90 rem/y to
19 6 rem/y (uncertainty due to lack of
knowledge of GCR from existing data). We
will continue RD to reduce the total weight and
dose.
y05K007V3
For Quench protection and new conductor RD, see
Appendix 7
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Lunar Surface Habitats Radiation Safety
Analysis NASA Langley Research Center, Hampton,
VA National Research Council, Washington, DC
College of William and Mary, Williamsburg, VA
On the lunar surface radiation exposure is given
by Galactic Cosmic Rays and by particles created
by interaction between GCRs and surface material

• Moon Base Outpost Phase
• Crew 8, Stay 90d, total 107d
• Spacecraft and Surface Habitats built in large
  volumes
• ? Surface Habitats shielded with a Regolith cover
  
• ? Shelter for Solar Particle Events (SPEs)
• Optimization Results
• ? Shielding Mass 10,000 T
• ? Total Dose Equivalent 2.72 rem
• ? Maximum Missions 20/34 for women/men

DOE Low Dose Radiation Research Program
Contractor Workshop June 27-30, 2001, Washington,
DC
For lunar radiation shielding details, see
Appendix 9
y05K143
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Radiation protection system on the moonbased on
existing AMS technology
Coil-to-coil support
1. No field outside magnet 2. No field inside
crew compartment 3. Minimum secondary radiation
inside crew compartment 4. Complete shielding of
solar flares 5. Total weight 30 T 6. Dose 2.5
rem/mission
Superfluid He vessel
Roof cap toroid
Ø 15 m
Coil support
6.2T
Side toroid
6.2T
Ø 5.6 m
2.25 m
8 m
Crew compartments
Thermal shield
2.25 m
Superfluid He vessel
Lunar surface
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Superconducting magnets for energy and propulsion
UF4-KF fuel mixture
Channels for Wall Cooling
Reactor
BeO
Super- conducting magnet
exhaust sent to high-T radiators and condensors
Swirl MHD Flow
Power conditioning for propulsion engine
(a) MHD/GCR cross section view
Vapor Core Reactor with MHD power conversion
(b) Plan view of sample trajectories in disk
Prof. Samim Anghaie, Director, Innovative Nuclear
Space Power and Propulsion Institute, INSPI
University of Florida, Gainesville.
y04K118b
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Superconducting Magnets for Electric Propulsion
(JSC)
Superconducting Coils
High power electric propulsion such as VASIMR and
other applied field plasma rockets relies on the
technology of superconducting magnets operating
in space.
Magnetic Field Lines
VASIMR Isp 10-30 Ksec
Superconducting Coils
y04K117a
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• The importance of being on the manifest
• Keep the excellent JSC Project Management team
  intact.
• Enable AMS to continue to receive high priority
  support from the
• 16 participating countries to complete the
  last phase of detector assembly.
• Enable the International team of 56 institutions
  to continue to participate in exploration efforts.

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• Summary
• Explore the foundation of modern physics (Grand
  Unified and Electroweak Theories, Time Reversal,
  SUSY and proton lifetime).
• Worldwide support for ISS science

AMS

• Accurate data on the radiation flux.
• Advance superconducting magnet technology for
  exploration
• ? Cosmic radiation shielding ? Propulsion
• ? Energy generation ? Energy storage (SMES)

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• Conclusions from the meeting with
• NASA Admistrator Dr. Michael Griffin, 5th Oct
  05.
• NASA will try to keep AMS on the shuttle manifest
  so that we are able to continue to receive NASA
  support for S. Porters group at JSC.
• NASA offered to put us on an ELV (Expendable
  Launch Vehicle) to ISS.

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Most Important
Finish the detector with Superconducting Magnet
Put it in test beam in 2007
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NASA support for the AMS superconducting magnet
The AMS superconducting magnet has been
developed under the leadership of Prof H. Hofer
of ETH-MIT with major financial support from
Switzerland, US (DOEMIT), Russia, China, Taiwan
and Spain. Over the last decade, many new
technologies were developed in Europe, financed
exclusively by the above countries. In
particular, the development of smallest cross
section Al stabilized conductor by ETH is the
key. NASA has been extremely supportive,
providing vacuum cases, systems engineering and
safety. We expect that NASA will continue to
support the magnet by providing an additional
3M for the He tank. The magnet, like the TRD,
Tracker and so forth, is an integral part of the
AMS experiment and is the property of the AMS
collaboration. We continue to look to NASA to
help us to put this magnet into space.
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