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Info about Shuttle Flight STS- 41
NASA
SPACE SHUTTLE MISSION STS-41
PRESS KIT
OCTOBER 1990
PUBLIC AFFAIRS CONTACTS
Mark Hess/Ed Campion
Office of Space Flight
NASA Headquarters, Washington, D.C.
(Phone: 202/453-8536)
Paula Cleggett-Haleim/Michael Braukus
Office of Space Science and Applications
NASA Headquarters, Washington, D.C.
(Phone: 202/453-1547)
Debra Rahn
International Affairs
NASA Headquarters, Washington, D.C.
(Phone: 202/453-8455)
Robert J. MacMillin
Jet Propulsion Laboratory
Pasadena, Calif.
(Phone: 818/354-5011)
Randee Exler
Goddard Space Flight Center,
Greenbelt, Md.
(Phone: 301/286-7277)
Nancy Lovato
Ames-Dryden Flight Research Facility,
Edwards, Calif.
(Phone: 805/258-3448
James Hartsfield
Johnson Space Center,
Houston, Texas
(Phone: 713/483-5111)
Lisa Malone/Pat Phillips
Kennedy Space Center, Fla.
(Phone: 407/867-2468)
Jerry Berg
Marshall Space Flight Center,
Huntsville, Ala.
(Phone: 205/544-0034)
CONTENTS
GENERAL RELEASE 3
GENERAL INFORMATION 5
STS-41 QUICK LOOK 6
PAYLOAD AND VEHICLE WEIGHTS 7
TRAJECTORY SEQUENCE OF EVENTS 8
SPACE SHUTTLE ABORT MODES 9
SUMMARY OF MAJOR ACTIVITIES 10
THE ULYSSES MISSION 11
Mission Summary 11
Ulysses Spacecraft 12
Scientific Experiments 14
Tracking and Data Acquisition 17
Ulysses Management 18
CHROMEX-2 18
Results from CHROMEX-1 19
SOLID SURFACE COMBUSTION EXPERIMENT 20
SHUTTLE SOLAR BACKSCATTER ULTRAVIOLET INSTRUMENT 20
INTELSAT SOLAR ARRAY COUPON 21
PHYSIOLOGICAL SYSTEMS EXPERIMENT 22
INVESTIGATIONS INTO POLYMER MEMBRANE PROCESSING 23
VOICE COMMAND SYSTEM 25
RADIATION MONITORING EQUIPMENT-III 26
CREW BIOGRAPHIES 26
MISSION MANAGEMENT TEAM 28
RELEASE: 90-122
ULYSSES DEPLOYMENT HIGHLIGHTS STS-41 MISSION
Space Shuttle mission STS-41 will be highlighted by deployment of the
Ulysses spacecraft on a 5-year journey to become the first probe to explore
the polar regions of the sun.
Current scheduling indicates a likelihood of launching on Oct. 8 or 9,
but a few days either side are possible, depending on actual test and
preparation time needed. The actual launch date will be set at the flight
readiness review, scheduled for Sept. 24-25. Landing is planned at
Edwards Air Force Base, Calif. The 4-day mission will be Discovery's 11th
flight.
After being deployed from Discovery under the oversight of Mission
Specialist Thomas D. Akers, a two-stage Inertial Upper Stage and a single-
stage Payload Assist Module will boost Ulysses on a trajectory that will take
it to Jupiter in 16 months. Upon arrival, in addition to making some
scientific studies of the giant planet, the spacecraft will receive a gravity
assist from Jupiter into a solar orbit almost perpendicular to the plane in
which the planets orbit. Ulysses is scheduled to make its first observations
of the sun's southern pole between June and October 1994 and continue on
to observe the northern solar pole between June and September 1995.
Also in Discovery's payload bay will be the Airborne Electrical Support
Equipment, an electrical generating system mounted on the side of the bay
to supply power to Ulysses. The Intelsat Solar Array Coupon, samples of
solar array materials mounted on Discovery's Remote Manipulator System,
is designed to study the effects of atomic oxygen wear on solar panels in
preparation for a future Shuttle mission to rescue the stranded Intelsat
satellite. The Shuttle Solar Backscatter Ultraviolet (SSBUV) experiment
also will be in Discovery's payload bay, mounted in two Get Away Special
containers. SSBUV will help fine tune the atmospheric ozone
measurements made by satellites already in orbit by providing a calibration
of their backscatter ultraviolet instruments.
Discovery also will carry the Chromosome and Plant Cell Division in
Space experiment, a study of plant root growth patterns in microgravity;
the Investigations into Polymer Membrane Processing experiment, a study
of materials processing in microgravity; the Physiological Systems
Experiment, an investigation of how microgravity affects bone calcium, body
mass and immune cell function; the Radiation Monitoring Experiment to
record radiation levels in orbit; the Solid Surface Combustion Experiment,
a study of flames in microgravity; and the Voice Command System, a
development experiment in voice commanding the Shuttle's onboard
television cameras.
Commanding Discovery will be Richard N. Richards, Capt., USN.
Robert D. Cabana, Lt. Col., USMC, is pilot. Richards will be making his
second space flight, after serving as pilot of STS-28. Cabana will be making
his first flight.
Mission specialists are William M. Shepherd, Capt., USN; Bruce
Melnick, Cmdr., USCG; and Thomas D. Akers, Major, USAF. Shepherd is
making his second flight, after being aboard STS-27. STS-41 will be
Melnick's and AkerUs first space flight.
Built by Dornier GmbH of West Germany, Ulysses is a joint project of
the European Space Agency (ESA) and NASA.
(End of general release. Background information follows.)
GENERAL INFORMATION
NASA Select Television Transmission
NASA Select television is available on Satcom F-2R, Transponder 13,
located at 72 degrees west longitude; frequency 3960.0 MHz, audio 6.8
MHz.
The schedule for television transmission from the orbiter and for the
change-of-shift briefings from Johnson Space Center, Houston, will be
available during the mission at Kennedy Space Center, Fla.; Marshall
Space Flight Center, Huntsville, Ala.; Johnson Space Center; and NASA
Headquarters, Washington, D.C. The TV schedule will be updated daily
to reflect changes dictated by mission operations.
Television schedules also may be obtained by calling COMSTOR,
713/483-5817. COMSTOR is a computer data base service requiring
the use of a telephone modem. A voice update of the TV schedule may
obtained by dialing 202/755-1788. This service is updated daily at
noon EDT.
Status Reports
Status reports on countdown and mission progress, on-orbit
activities and landing operations will be produced by the appropriate
NASA news center.
Briefings
An STS-41 mission press briefing schedule will be issued prior to
launch. During the mission, flight control personnel will be on 8-hour
shifts. Change-of-shift briefings by the off-going flight director will
occur at approximately 8-hour intervals.
STS-41 QUICK LOOK
Launch Date and Site:
Oct. 5, 1990
Kennedy Space Center, Fla., Pad 39-B
Launch Window: 7:35 a.m. - 9:53 a.m. EDT
Orbiter: Discovery (OV-103)
Orbit: 160 x 160 nautical miles, 28.45 degree inclination
Landing Date/Time: 9:42 a.m. EDT, Oct. 9, 1990
Primary Landing Site: Edwards Air Force Base, Calif.
Abort Landing Sites:
Return to Launch Site - Kennedy Space Center, Fla.
Transoceanic Abort Landing - Ben Guerir, Morocco
Abort Once Around - Edwards Air Force Base, Calif.
Crew:
Richard N. Richards, Commander
Robert D. Cabana, Pilot
Bruce E. Melnick, Mission Specialist 1
William M. Shepherd, Mission Specialist 2
Thomas D. Akers, Mission Specialist 3
Cargo Bay Payloads:
Ulysses/IUS/PAM-S
SSBUV
Intelsat Solar Array Coupon
Middeck Payloads:
Solid Surface Combustion Experiment (SSCE)
Investigations into Polymer Membrane Processing (IPMP)
Chromosome and Plant Cell Division in Space (CHROMEX-2)
Physiological Systems Experiment (PSE)
Voice Command System (VCS)
Radiation Monitoring Experiment-III (RME-III)
VEHICLE AND PAYLOAD WEIGHTS
Pounds
Orbiter (Discovery) empty 151,265
Remote Manipulator System (payload bay) 1,180
Ulysses/IUS/PAM-S (payload bay) 44,024
Airborne Electrical Support Equipment, RTG cooling
system (payload bay) 203
IUS Support Equipment (payload bay) 260
Shuttle Solar Backscatter Ultraviolet Instrument (SSBUV)
(payload bay) 1,215
Chromosome and Plant Cell Division in Space (CHROMEX) 85
Investigations into Polymer Membrane Processing (IPMP) 33
Physiological Systems Experiment (PSE) 132
Radiation Monitoring Experiment-III (RME-III) 23
Solid Surface Combustion Experiment (SSCE) 140
Voice Command System (VCS) 45
Orbiter and Cargo at SRB Ignition 256,330
Total Vehicle at SRB Ignition 4,524,982
Orbiter Landing Weight 197,385
TRAJECTORY SEQUENCE OF EVENTS
EVENT MET RELATIVE MACH ALTITUDE
(d/h:m:s) VELOCITY (ft)
(fps)
Launch 00/00:00:00
Begin Roll Maneuver 00/00:00:07 136 .1 400
End Roll Maneuver 00/00:00:19 417 .37 3,483
SSME Throttle Down to 65% 00/00:00:28 665 .6 7,900
Max. Dyn. Pressure (Max Q) 00/00:00:51 1,146 1.11 26,448
SSME Throttle Up to 104% 00/00:00:58 1,325 1.29 33,950
SRB Staging 00/00:02:05 4,144 3.76 156,585
Main Engine Cutoff (MECO) 00/00:08:30 24,455 22.3 361,210
Zero Thrust 00/00:08:38 24,509 22.28 363,225
ET Separation 00/00:08:50
OMS 2 Burn 00/00:39:55 221 42 sec. 160 x 160 nm
Ulysses/IUS Deploy (orbit 5) 00/06:01:00
OMS 3 Burn 00/06:16:00 31 16 sec. 160 x 177 nm
OMS 4 Burn 00/22:56:00 35 160 x 156 nm
Deorbit Burn (orbit 65) 04/01:08:00 278
Landing (orbit 66) 04/02:07:00
Apogee, Perigee at MECO: 157 x 35
Apogee, Perigee post-OMS 2: 160 x 160
Apogee, Perigee post deploy: 160 x 177
SPACE SHUTTLE ABORT MODES
Space Shuttle launch abort philosophy is to achieve a safe and intact
recovery of the flight crew, orbiter and its payload. Abort modes include:
% Abort-To-Orbit (ATO)
Partial loss of main engine thrust late enough to permit
reaching a minimal 105-nautical mile orbit with orbital
maneuvering system engines.
% Abort-Once-Around (AOA)
Earlier main engine shutdown with the capability to allow one
orbit around before landing at Edwards Air Force Base, Calif.;
White Sands Space Harbor (Northrup Strip), N. Mex.; or the
Shuttle Landing Facility (SLF) at Kennedy Space Center, Fla..
% Trans-Atlantic Abort Landing (TAL)
Loss of two main engines midway through powered flight would
force a landing at Ben Guerir, Morocco; Moron, Spain; or
Banjul, The Gambia.
% Return-To-Launch-Site (RTLS)
Early shutdown of one or more engines and without enough
energy to reach Ben Guerir, would result in a pitch around and
thrust back toward KSC until within gliding distance of the
Shuttle Landing Facility.
STS-41 contingency landing sites are Edwards AFB, White Sands,
Kennedy Space Center, Ben Guerir, Moron and Banjul.
SUMMARY OF MAJOR ACTIVITIES
Day One
Ascent
Post-insertion checkout
Pre-deploy checkout
Ulysses/IUS deploy
CHROMEX-2
Detailed science objective (DSO)/detailed test objective (DTO)
Physiological systems experiment (PSE)
SSBUV outgassing
Day Two
Air Force Maui Optical Site (AMOS) calibration test
Ulysses/IUS backup deploy opportunity
CHROMEX-2
DSO/DTO
RMS powerup and checkout
SSBUV Earth views
Voice command system (VCS) test #1
Day Three
CHROMEX-2
DTO
SSBUV Earth views
VCS test #2
Day Four
CHROMEX-2
DSO/DTO
SSBUV Earth views
VCS test #3
Flight control system (FCS) checkout
Reaction control system (RCS) hotfire
Cabin stow
Day Five
CHROMEX-2 status
DSO/DTO
PSE status
SSBUV Earth views
SSBUV deactivation
Deorbit preparation
Deorbit burn
Landing at EAFB
ULYSSES MISSION
Ulysses is a joint mission conducted by the European Space Agency
(ESA) and NASA to study the polar regions of the sun and the interplanetary
space above the poles. The spacecraft will be the first to achieve a flight
path nearly perpendicular to the ecliptic, the plane in which Earth and the
other planets orbit the sun.
Throughout its 5-year mission, Ulysses will study three general areas of
solar physics: the sun itself, magnetic fields and streams of particles
generated by the sun and interplanetary space above the sun.
The Ulysses spacecraft, a ground control computer system and a
spacecraft operations team are provided by ESA, while Space Shuttle
launch, tracking and data collection during the mission are being
performed by NASA and the Jet Propulsion Laboratory (JPL). Scientific
instruments aboard the craft have been provided by scientific teams in both
Europe and the United States.
ULYSSES MISSION SUMMARY
After astronauts release Ulysses from Discovery's payload bay at an
altitude of 160 nautical miles, a two-stage engine, the Inertial Upper Stage
(IUS), attached to Ulysses will ignite, sending the craft on its initial
trajectory.
After the IUS separates, a smaller booster engine, the Payload Assist
Module (PAM-S), will fire. Before the PAM-S fires, it will spin Ulysses up to
a rate of 70 revolutions per minute (rpm). After the engine burn concludes,
the spin rate will slow to about 7 rpm. Boom deployment will further slow
the spin rate to about 5 rpm. Ulysses will continue to spin at this rate
throughout the remainder of the mission.
The booster engines will send Ulysses first to Jupiter, which the craft
will encounter in February 1992. As Ulysses flies past Jupiter at about 30
degrees north Jovian latitude, the gravity of the giant planet will alter the
craft's trajectory so Ulysses dives downward and away from the ecliptic
plane.
In its orbit around the sun, Ulysses flight path will take it from a
maximum distance from the sun of 5.4 astronomical units (AU), or about
500 million miles, to a closest approach of 1.3 AU, or about 120 million
miles.
The spacecraft will reach 70 degrees south solar latitude in June 1994,
beginning its transit of the sun's south polar regions. The craft will spend
about 4 months south of that latitude at a distance of about 200 million
miles from the sun.
In February 1995, Ulysses will cross the sun's equator, followed by its 4-
month pass of the sun's northern polar region beginning in June 1995.
End of mission is scheduled for Sept. 30, 1995.
THE ULYSSES SPACECRAFT
Ulysses' systems and scientific instruments are contained within a main
spacecraft bus measuring 10.5 by 10.8 by 6.9 feet. Communication with
Earth is maintained via a 5.4-foot-diameter, parabolic high-gain antenna.
After release from Discovery's cargo bay, the 807-pound spacecraft will
deploy an 18.2-foot radial boom carrying several experiment sensors, as
well as a 238-foot dipole wire boom and a 26.2-foot axial boom, which serve
as antennas for a radio wave-plasma wave experiment.
The Ulysses spacecraft's main computer is its onboard data handling
system, responsible for processing commands received from the ground as
well as managing and passing on all data from each of Ulysses' science
instruments. This system includes: a decoder unit, which processes
incoming signals from the spacecraft radio and passes on commands to
other systems; a central terminal unit, which distributes commands,
monitors and collects data on spacecraft systems, and stores and passes on
data from Ulysses' science instruments; remote units, which handle input-
output to and from spacecraft systems; and the data storage unit, two tape
recorders. Each of the tape recorders can store 45.8 million bits of data --
representing 16 to 64 hours of data-taking, depending on how often data
are sampled.
Another system, attitude and orbit control, is responsible for
determining the Ulysses craft's attitude in space, as well as firing thrusters
to control the attitude and spin rate. This system includes a redundant
computer, sun sensors and the reaction control system, including eight
thrusters and the hydrazine fuel system. Ulysses' load of 73 pounds of
monopropellant hydrazine fuel is stored in a single diaphragm tank
mounted on the spacecraft's spin axis.
The spacecraft's telecommunications system includes two S-band
receivers, two 5-watt S-band transmitters, two 20-watt X-band
transmitters, the high-gain antenna and two smaller low-gain antennas.
The high-gain antenna is used to transmit in either S band or X band as
well as to receive in S band. The low-gain antennas are used both to
transmit and receive in the S band. The spacecraft receives commands
from Earth on a frequency of 2111.607 MHz in the S band. The craft can
transmit to Earth on 2293.148 MHz in the S band or on 8408.209 MHz in
the X band.
(pages 13 and 13-A are drawings of the Ulysses spacecraft and mission profile.)
Ulysses' power source is a radioisotope thermo-electric generator
(RTG), similar to RTGs flown on previous solar system exploration missions.
RTGs are required for these deep-space missions because solar arrays large
enough to generate sufficient power so far from the sun would be too large
and too heavy to be launched by available means. In the RTG, heat
produced by the natural decay of plutonium-238 is converted into
electricity by thermocouples.
SCIENTIFIC EXPERIMENTS
Ulysses' scientific payload is composed of nine instruments. In addition,
the spacecraft radio will be used to conduct a pair of experiments over and
above its function of communicating with Earth, bringing the total number
of experiments to 11. Finally, two other investigation teams will conduct
interdisciplinary studies.
The experiments are:
-- Magnetic fields. This investigation will measure the strength and
direction of the sun's polar magnetic fields, which are poorly known
because they are difficult to observe from Earth. These measurements
will help identify specific regions of the corona, the outer portion of the
sun's atmosphere, from which the solar wind originates. They also will
be important in understanding the propagation of energetic particles of
both solar and galactic origin, which are guided by the magnetic field.
Principal investigator of the experiment is Dr. Andre Balogh of Imperial
College, London.
-- Solar-wind plasma. The solar wind is a fully ionized gas, or "plasma,"
consisting of electrons and the positively charged atoms (ions) from
which the electrons have been removed. This experiment will measure
the basic properties of these ions and electrons such as speed, density
and temperature. The outflowing solar wind is expected to be different,
and possibly simpler, in the sun's polar regions than near the equator.
If this is true, it should be easier to relate the observed solar-wind
particles to conditions in the region of the sun where they originated.
Dr. Samuel J. Bame of Los Alamos National Laboratory is principal
investigator.
-- Solar-wind ion-composition spectrometer (SWICS). This investigation
will detect heavy ions (elements up to and including iron) which exist
in the corona and which constitute a minor but important constituent of
the solar wind. By measuring the composition, temperature and degree
of ionization of this component, it should be possible to infer the
temperature of the corona in the source region. This investigation will
also detect solar-wind ions that have been accelerated or energized in
interplanetary space, possibly including the sun's polar regions. Dr.
George Gloeckler of the University of Maryland and Dr. Johannes Geiss
of Universitt Bern, Switzerland, are co-principal investigators.
-- Heliospheric instrument for spectra, composition and anisotropy at low
energies. This energetic particle detector will measure the
composition and properties of low-energy solar-wind ions that have
been accelerated to higher energies than those observed by the SWICS.
Such particles can be energized at the sun as part of the process that
produces solar flares or in interplanetary space. The investigation will
determine whether such particles exist in the sun's polar regions. If so,
the measurements can be used to further study their origin, storage in
the corona and subsequent propagation into space. Dr. Louis J.
Lanzerotti of Bell Laboratories, New Jersey, is principal investigator.
-- Energetic-particle composition and neutral gas. An array of charged-
particle telescopes on Ulysses will detect medium-energy charged
particles and determine their composition, relative abundances,
energies and direction of travel. Charged particles in this energy range
mark a transition between solar particles and cosmic-ray particles
which are accelerated elsewhere in the galaxy and travel vast distances
to reach the solar system. A separate instrument will detect neutral
helium atoms entering the solar system from interstellar space and will
determine their speed, direction of arrival, temperature and density.
Dr. Erhardt Keppler of the Max-Planck-Institut fuer Aeronomie in
Lindau, Germany, is principal investigator.
-- Cosmic and solar particle investigation. This experiment covers even
higher-energy cosmic rays as well as detecting energetic solar and
interplanetary particles. Cosmic rays, which have been studied for many
years near the solar equator, are likely to have preferred access to the
equatorial zone of the solar system by way of the sun's polar regions.
This experiment may measure the properties of the cosmic rays before
they are strongly modified by their interaction with the solar-
interplanetary magnetic field. At present, the properties of cosmic rays
at these energies are not known as they exist in interstellar space. Dr.
John A. Simpson of the University of Chicago is principal investigator.
-- Solar X-rays and cosmic gamma rays. This experiment will detect X-
rays which are emitted sporadically from the vicinity of solar active
regions. Although these X-rays have been observed for many years by
spacecraft above the Earth's atmosphere, the altitude in the solar
atmosphere at which the radiation is emitted and its directivity, which
would help identify the source mechanism, are unknown. As Ulysses
travels pole-ward, the sun will cut off or "occult" radiation at low
altitudes and affect how the intensity varies with direction to the
source. Cosmic gamma-ray bursts were detected about 20 years ago but
their origin has remained obscure. By accurately timing their arrival at
Ulysses and at Earth, their source location can be pinpointed precisely
to see what astrophysical objects or bodies give rise to them. Dr. Kevin
Hurley of the University of California, Berkeley, and Dr. Michael
Sommer of the Max-Planck-Institut fuer Extraterrestrische Physik in
Garching, Germany, are co-principal investigators.
-- Unified radio and plasma-wave experiment. Two sets of long,
deployable antennas are used to measure high-frequency radio waves
emitted from solar active regions as well as lower-frequency "plasma"
waves generated in the solar wind near the spacecraft. The radio-wave
observations will be used to diagnose the space medium between the
sun's polar regions and Ulysses. Observations of the locally generated
waves will provide information about the internal workings of the polar
wind, particularly the instabilities that transfer energy between the
waves and their constituent particles. Dr. Robert G. Stone of the NASA
Goddard Space Flight Center, Greenbelt, Md., is principal investigator.
-- Cosmic dust. From the speed and direction of the small particles
detected by this experiment, their interplanetary trajectories can be
deduced. Mass and charge of the dust particles also will be measured so
that competing effects on their motion of solar radiation, gravitation and
solar-wind particles can be studied. The distribution of dust and its
changing properties from the solar equator to the sun's poles will help
distinguish the contributions of three major sources: comets, asteroids
and interstellar dust. Dr. Eberhard Gruen of the Max-Planck-Institut
fuer Kernphysik in Heidelberg, Germany, is principal investigator.
-- Coronal sounding. This experiment uses signals transmitted
simultaneously by Ulysses' radio at two frequencies to infer properties of
the sun's corona along the path from the spacecraft to the radio
receivers on Earth. From subtle shifts in phase of these two signals, the
density and directed velocity of coronal electrons can be inferred at the
location where the radio waves pass closest to the sun. Of particular
scientific interest are these properties of the corona in the sun's polar
regions as Ulysses ascends in latitude. Dr. Hans Volland of Universitaet
Bonn, Germany, is principal investigator.
-- Gravitational waves. This investigation also makes use of the spacecraft
radio transmitter for scientific purposes. According to Einstein's theory
of relativity, the motion of large masses in the universe -- such as those
associated with the formation of black holes -- should cause the
radiation of gravitational waves. Although such waves have yet to be
detected, they could be observed through their effect on the spacecraft,
which is expected to undergo a slight perturbation that might be
detectable as a shift in frequency of Ulysses' radio signal. Dr. Bruno
Bertotti of Universita di Pavia, Italy, is principal investigator.
In addition to the 11 experiment teams, two investigation teams will
study interdisciplinary topics:
-- Directional discontinuities. The solar-wind plasma is not homogenous
but consists of adjacent regions in which the plasma and magnetic field
are different. These regions are separated by thin surfaces, called
discontinuities, across which the properties change abruptly. Ulysses
measurements will be compared with theoretical models developed by a
team led by Dr. Joseph Lemaire of the Institut d'Aeronomie Spatiale de
Belgique, Belgium.
-- Mass loss and ion composition. This team will combine measurements
of the solar wind and magnetic field to study the mass and angular
momentum lost by the sun in the equatorial and polar regions. A
second problem which will be studied is the dependence of the solar
wind composition on solar latitude. This team is led by Dr. Giancarlo
Noci of the Istituto di Astronomia, Italy.
TRACKING AND DATA ACQUISITION
Throughout the Ulysses mission, tracking and data acquisition will be
performed through NASA's Deep Space Network (DSN).
The DSN includes antenna complexes at Goldstone, in California's
Mojave Desert; near Madrid, Spain; and at Tidbinbilla, near Canberra,
Australia. The complexes are spaced approximately 120 degrees apart in
longitude around the globe so that, as the Earth turns, a given spacecraft
will nearly always be in view of one of the DSN complexes.
Each complex is equipped with a 230-foot-diameter antenna; two 112-
foot antennas; and an 85-foot antenna. Each antenna transmits and
receives. The receiving systems include low-noise amplifiers.
Transmitters on the 230-foot antennas are rated at 100 kilowatts of power,
while the 112- and 85-foot antennas have 20-kilowatt transmitters. Each
antenna station also is equipped with data handling and interstation
communication equipment.
During most of the mission, the DSN will be in contact with Ulysses 8
hours per day. The spacecraft will record all its science and engineering
data during the 16 hours it is out of touch with Earth; during the 8 hours of
DSN contact, the spacecraft will transmit stored data from the craft's tape
recorder.
Mission plans call for a 112-foot antenna to be used both to transmit to
and receive from Ulysses. To conserve antenna coverage during periods of
high demand on the DSN, ground teams can switch to the 230-foot
antennas for communication with Ulysses; the larger antennas permit a
higher data rate, so 4 hours of antenna coverage each 48 hours is sufficient.
Data streams received from Ulysses at the DSN station are processed
and transmitted to the Mission Control and Computing Center at JPL in
Pasadena, Calif. Data are transmitted to Pasadena from the various DSN
stations by a combination of land lines, ground microwave links and Earth-
orbiting communication satellites.
ULYSSES MANAGEMENT
The Ulysses spacecraft was built for ESA by Dornier GmbH (Inc.) of
Germany. Subcontractors included firms in Austria, Belgium, Denmark,
France, Italy, The Netherlands, Spain, Sweden, Switzerland, the United
Kingdom and the United States. In addition to providing the spacecraft,
ESA is responsible for spacecraft operations.
Launch on Space Shuttle Discovery is provided by NASA. In addition,
NASA is responsible for the IUS and PAM-S upper-stage engines, built for
the U.S. Air Force by Boeing Aerospace & Electronics Co. (IUS) and
McDonnell Douglas Space Systems Co. (PAM-S). NASA also provides the
radioisotope thermo-electric generator (RTG), built for the U.S.
Department of Energy by the General Electric Co.
Tracking through the Deep Space Network and ground operations
facilities in Pasadena, Calif., are managed for NASA by JPL. The U.S. portion
of the Ulysses mission is managed by JPL for NASA's Office of Space
Science and Applications.
CHROMEX-2
The Chromosome and Plant Cell Division (CHROMEX-2) experiment is
designed to study some of the most important phenomena associated with
plant growth. The CHROMEX-2 experiment aims to determine how the
genetic material in the root cells responsible for root growth in flowering
plants responds to microgravity.
All plants, in the presence of light, have the unique ability to convert
carbon dioxide and water into food and oxygen. Any long expedition or
isolated settlement beyond Earth orbit will almost certainly necessitate the
use of plants to manufacture food for crew members. In addition,
information from space based life sciences research promotes fundamental
understanding of the mechanisms responsible for plant growth and
development. An improved understanding of plant responses to spaceflight
is required for the long-term goal of a controlled ecological life support
system for space use.
One of the practical benefits of studying and designing plant growth
systems (and eventually agricultural systems) for use in space is the
contribution this work may make to developing new intensive farming
practices for extreme environments on Earth. Over the last few decades,
basic research in the plant sciences has enabled the great increase in crop
productivity (the "green revolution") that has transformed modern
agriculture. Plant research in space may help provide the necessary
fundamental knowledge for the next generation of agricultural
biotechnology.
Dr. Abraham D. Krikorian of the State University of New York at Stony
Brook is the principal investigator. This experiment has been developed at
the Kennedy Space Center and uses the Plant Growth Unit developed by
the NASA Ames Research Center.
RESULTS FROM THE FIRST FLIGHT OF CHROMEX
The first flight of CHROMEX in March 1989 showed that spaceflight
seems to have a distinct, measurable and negative effect on the structural
integrity of chromosomes in root tip cells. The plantlets grew well, but at
the cellular level, in the chromosomes in rapidly dividing root tip cells,
damage was clearly visible through light microscopy. Damage or aberrations
were seen in 3-30% of dividing cell chromosomes. Ground controls were
damage-free. The exact cause for the chromosomal aberrations seen on
CHROMEX-1 is not known, but data from the radiation measuring devices
flown with the plantlets suggest that radiation alone was insufficient to
cause the observed damage. The principal investigator has suggested that
an interaction of microgravity and radiation may be responsible. This
hypothesis cannot be fully tested until an artificial gravity centrifuge is
developed to enable additional space biology experiments.
Roots grown in space also were seen to have a higher percentage of cells
undergoing division than ground controls. As expected, roots grew in all
directions in space, while roots grew normally and downward on the
ground controls. More root tissue grew on the space flown plants, but this
was probably due to the increased moisture held in the foam used as
artificial soil in the Plant Growth Unit. The plants were grown as planned
without microbial contamination throughout the flight and ground control
experiments.
SOLID SURFACE COMBUSTION EXPERIMENT
The Solid Surface Combustion Experiment (SSCE) will study the basic
behavior of fire by examining the spreading of flame over solid fuels without
the influence of gravity. This research may lead to improvements in fire
prevention or control both on Earth and in spacecraft.
On Earth, spreading flames are strongly affected by gravity. Hot gases,
which are less dense than cold gases, ascend from flames in the same way
that oil floats on water. This phenomena -- "buoyant convection" --
removes hot gases from the flame and draws in fresh air to take their
place. The resulting air motion tends to cool the flame. However, it also
provides fresh oxygen, which makes the flame hotter. The heating and
cooling effects compete, with the outcome depending upon the speed of
the airflow (A campfire, for example, is strengthened by blowing, while a
match can be blown out). Scientists quantify the airflow effects on Earth by
augmenting buoyant convection with controlled amounts of forced
convection. On Earth, gravity prevents observation of airflows slower than
buoyant convection speeds, limiting the ability to develop complete models
of solid surface combustion.
SSCE will provide observations of flames spreading without buoyant
convection. Air motion is eliminated except to the extent that the flame
spreads into fresh air and away from the hot gases. Convective cooling and
the heating effect of fresh oxygen are simultaneously minimized. The
competition between heating and cooling effects will be quantified by
performing tests in artificial atmospheres that have different fractional
amounts of oxygen (the air we breathe is 21% oxygen).
The SSCE hardware consists of a chamber to house the burning sample,
two cameras to record the experiment on film and a computer to control
experiment operations. Fuel and air temperatures are recorded during the
experiment for comparison with theory. The SSCE test plan calls for eight
Shuttle flights over the next 3 years. Five flights will use samples made of a
special ashless filter paper and three will use samples of
polymethylmethacrylate (PMMA), commonly known as plexiglass. Each test
will be conducted in an artificial atmosphere containing oxygen at levels
ranging from 35% to 50%.
The SSCE was conceived by the principle investigator, Dr. Robert A.
Altenkirch, Dean of Engineering at Mississippi State University; the flight
hardware was developed by the NASA Lewis Research Center, Cleveland.
SHUTTLE SOLAR BACKSCATTER ULTRAVIOLET (SSBUV) INSTRUMENT
The Shuttle Solar Backscatter Ultraviolet (SSBUV) instrument was
developed by NASA to compare the observations of several ozone measuring
instruments aboard the National Oceanic and Atmospheric Administration's
TIROS satellites (NOAA-9 and NOAA-11) and NASA's NIMBUS-7 satellite.
The SSBUV data is used to calibrate these instruments to insure the most
accurate readings possible for the detection of ozone trends.
The SSBUV will help scientists solve the problem of data reliability
caused by the calibration drift of the Solar Backscatter Ultraviolet (SBUV)
instruments on these satellites. The SSBUV uses the Space Shuttle's
orbital flight path to assess instrument performance by directly comparing
data from identical instruments aboard the TIROS spacecraft and NIMBUS-
7 as the Shuttle and satellite pass over the same Earth location within an
hour. These orbital coincidences can occur 17 times a day.
The satellite-based SBUV instruments estimate the amount and height
distribution of ozone in the upper atmosphere by measuring the incident
solar ultraviolet radiation and ultraviolet radiation backscattered from the
Earth's atmosphere. The SBUV measures these parameters in 12 discrete
wavelength channels in the ultraviolet. Because ozone absorbs in the
ultraviolet, an ozone measurement can be derived from the ratio of
backscattered radiation at different wavelengths, providing an index of the
vertical distribution of ozone in the atmosphere.
The SSBUV has been flown once, on STS-34 in October 1989. Its
mission successfully completed, the SSBUV was refurbished, recalibrated
and reprocessed for flight. NASA plans to fly the SSBUV approximately
once a year for the duration of the ozone monitoring program, which is
expected to last until the year 2000. As the project continues, the older
satellites with which SSBUV works are expected to be replaced to insure
continuity of calibration and results.
The SSBUV instrument and its dedicated electronics, power, data and
command systems are mounted in the Shuttle's payload bay in two Get
Away Special canisters that together weigh 1,200 pounds. The instrument
canister holds the SSBUV, its aspect sensors and in-flight calibration
system. A motorized door assembly opens the canister to allow the SSBUV
to view the sun and Earth and closes during in-flight calibration. The
support canister contains the power system, data storage and command
decoders. The dedicated power system can operate the SSBUV for
approximately 40 hours.
The SSBUV is managed by NASA's Goddard Space Flight Center,
Greenbelt, Md., for the Office of Space Science and Applications. Ernest
Hilsenrath is the principal investigator. Donald Williams is the experiment
manager.
INTELSAT SOLAR ARRAY COUPON
The Intelsat Solar Array Coupon (ISAC) experiment on STS-41 is being
flown by NASA for the International Telecommunications Satellite
Organization (INTELSAT). The experiment will measure the effects of
atomic oxygen in low Earth orbit on the Intelsat satellite's solar arrays, to
judge if the stranded satellite's arrays will be seriously damaged by those
effects.
Intelsat, launched aboard a commercial expendable launch vehicle
earlier this year, is stranded in a low orbit and is, at the request of the
company, being evaluated for a possible Space Shuttle rescue mission in
1992.
ISAC consists of two solar array material samples mounted on Discovery's
remote manipulator system (RMS) arm. The arm will be extended to hold
the samples perpendicular to the Shuttle payload bay, facing the direction
of travel, for at least 23 consecutive hours.
PHYSIOLOGICAL SYSTEMS EXPERIMENT
The Physiological Systems Experiment (PSE) is a middeck payload
sponsored by the Pennsylvania State University's Center for Cell Research, a
NASA Office of Commercial Programs Center for the Commercial
Development of Space. The corporate affiliate leading the PSE investigation
is Genentech, Inc., South San Francisco, Calif., with NASA's Ames Research
Center, Mountain View, Calif., providing payload and mission integration
support.
The goal of the PSE is to investigate whether biological changes caused
by near weightlessness mimic Earth-based medical conditions closely
enough to facilitate pharmacological evaluation of potential new therapies.
Research previously conducted by investigators at NASA, Penn State and
other institutions has revealed that in the process of adapting to near
weightlessness, or microgravity, animals and humans experience a variety
of physiological changes including loss of bone and lean body tissue, some
decreased immune cell function, change in hormone secretion and cardiac
deconditioning, among others. These changes occur in space-bound
animals and people soon after leaving Earth's gravitational field. Therefore,
exposure to conditions of microgravity during the course of space flight
might serve as a useful and expedient means of testing potential therapies
for bone and muscle wasting, organ tissue regeneration and immune system
disorders.
Genentech is a biotechnology company engaged in the research,
development, manufacture and marketing of recombinant DNA-based
pharmaceuticals. The company replicates natural proteins and evaluates
their pharmacological potential to treat a range of medical disorders.
In this experiment, eight healthy rats will receive one of the natural
proteins Genentech has developed. An identical group will accompany
them during the flight, but will not receive the protein, thereby providing a
standard of comparison for the treated group. Both groups will be housed
in self-contained animal enclosure modules which provide sophisticated
environmental controls and plenty of food and water throughout the flights
duration. The experiment's design and intent has received the review and
approval of the Animal Care and Use Committees from both NASA and
Genentech. Laboratory animal veterinarians will oversee selection, care and
handling of the animals.
Following the flight, the rat tissues will be thoroughly evaluated by
teams of scientists from Genentech and the Center for Cell Research in a series
of studies which will require several months.
Dr. Wesley Hymer is Director of the Center for Cell Research at Penn
State and co-investigator for PSE. Dr. Michael Cronin, Genentech, is
principal investigator.
INVESTIGATIONS INTO POLYMER MEMBRANE PROCESSING
The Investigations into Polymer Membrane Processing (IPMP), a
middeck payload, will make its second Space Shuttle flight for the Office of
Commercial Programs-sponsored Battelle Advanced Materials Center for
the Commercial Development of Space (CCDS) in Columbus, Ohio.
The objective of the IPMP research program is to gain a fundamental
understanding of the role of convection driven currents in the transport
processes which occur during the evaporation casting of polymer
membranes and, in particular, to investigate how these transport processes
influence membrane morphology.
Polymer membranes have been used in the separations industry for many
years for such applications as desalination of water, atmospheric
purification, purification of medicines and dialysis of kidneys and blood.
The IPMP payload uses the evaporation casting method to produce
polymer membranes. In this process, a polymer membrane is prepared by
forming a mixed solution of polymer and solvent into a thin layer; the
solution is then evaporated to dryness. The polymer membrane is left with
a certain degree of porosity and then can be used for the applications listed
above.
The IPMP investigations on STS-41 will seek to determine the
importance of the evaporation step in the formation of thin-film
membranes by controlling the convective flows. Convective flows are a
natural result of the effects of gravity on liquids or gasses that are non-
uniform in specific density. The microgravity of space will permit research
to study polymer membrane casting in a convection-free environment.
The IPMP program will increase the existing knowledge base regarding
the effects of convection in the evaporation process. In turn, industry will
use this understanding to improve commercial processing techniques on
Earth with the ultimate goal of optimizing membrane properties.
The IPMP payload on STS-41 consists of two experimental units that
occupy a single small storage tray (one-half of a middeck locker) which
weighs less than 20 pounds.
Early in Flight Day 1, a crew member will turn the valve to the first stop
to activate the evaporation process. Turning the valve opens the pathway
between the large and sample cylinders causing the solvents in the sample
to evaporate into the evacuated larger cylinders. Both flight units are
activated at the same time.
The STS-41 experiment will investigate the effects of evaporation time
on the resulting membranes by deactivating the two units at different times.
The evaporation process will be terminated in the first unit after a period of
5 minutes, by turning the valve to its final position. This causes the process
to terminate by flushing the sample with water vapor, and thus setting the
membrane structure. After the process is terminated, the resulting
membrane then will not be affected by gravitational forces experienced
during reentry, landing and post-flight operations. The second unit will be
deactivated after a period of 7 hours.
In IPMP's initial flight on STS-31, mixed solvent systems were
evaporated in the absence of convection to control the porosity of the
polymer membrane. Ground-based control experiments also were
performed. Results from STS-31 strongly correlated with previous KC-135
aircraft testing and with a similar experiment flown on the Consort 3
sounding rocket flight in May 1990. The morphology of polymer
membranes processed in reduced gravity showed noticeable differences
from that of membranes processed on Earth.
However, following post-flight analysis of the STS-31 experiment, it was
decided to incorporate a minor modification to the hardware to
significantly improve confidence in the analysis by providing additional
insight into the problem. In addition, the modification would further
remove remaining variables in the experiment.
The two most significant variables remaining in the experiment as
originally configured are the time factor and the gravitational forces
affecting the samples prior to retrieval of the payload. With the addition of
a 75-cc cylinder containing a small quantity of distilled water pressurized
with compressed air to greater than 14 psig, Space Shuttle crew members
will be able to abruptly terminate (or "quench") the vacuum evaporation
process by flushing the sample with water vapor. After the process is
terminated, the resulting membrane will not be further affected by gravity
variations. The planned modifications will not alter the experimental
objectives and, in fact, will further contribute to a better understanding of
the transport mechanisms involved in the evaporation casting process.
Subsequent flights of the IPMP payload will use different polymers,
solvents and polymer-to-solvent ratios. However, because of the
modification to the hardware, the polymer/solvent combination used on
this flight will be the same as that used on the first slight. The polymer,
polysulfone, is swollen with a mixture of dimethylacetamide and acetone in
the IPMP units. Combinations of polymers and solvents for later
experiments will be selected and/or adjusted based on the results of these
first flights.
Principal investigators for the IPMP is Dr. Vince McGinness of Battelle.
Lisa A. McCauley, Associate Director of the Battelle CCDS, is Program
Manager.
VOICE COMMAND SYSTEM
The Voice Command System (VCS) is a flight experiment using
technology developed at the Johnson Space Center, Houston, to control the
onboard Space Shuttle television cameras using verbal commands.
On STS-41, the VCS will be used by mission specialists William
Shepherd and Bruce Melnick. The system allows the astronauts to control
the cameras hands-free using simple verbal commands, such as "stop, up,
down, zoom in, zoom out, left, right." The VCS unit is installed in
Discovery's aft flight deck, in an instrument panel directly below the
standard closed circuit television displays and controls.
Shepherd and Melnick will operate the VCS at least three times each
during the mission. The original television displays and controls on board
Discovery will be used for standard operations during the flight. When the
VCS is powered on, the manual controls will remain operational, and the
cameras can be controlled using either method.
The VCS displays and controls are a 2- by 10-inch fluorescent display
and three switches, a power switch, mode switch and reset switch. Voice
commands from Shepherd and Melnick have been recorded prior to the
flight and voice templates inside the VCS were made to allow the computer
to recognize them. When using the VCS, the mission specialist will wear a
special headset with a microphone that feeds the verbal commands into the
system.
If successful, the VCS could be incorporated as standard equipment aboard
the Shuttle, allowing much simpler television operations. Such
simplification could greatly reduce the amount of hands-on work needed
for television operations during such times as maneuvers with the Shuttle's
remote manipulator system robotic arm. Normally, an astronaut controlling
the arm uses two hands for the task and must remove one hand to adjust
television coverage. Information from this flight can determine if
microgravity affects the user's voice patterns in a way that can inhibit the
VCS's ability to recognize them.
RADIATION MONITORING EQUIPMENT-III
The Radiation Monitoring Equipment-III measures ionizing radiation
exposure to the crew within the orbiter cabin. RME-III measures gamma
ray, electron, neutron and proton radiation and calculates -- in real time --
exposure in RADS-tissue equivalent. The information is stored in memory
modules for post-flight analysis.
The hand-held instrument will be stored in a middeck locker during
flight except for activation and memory module replacement periods.
RME-III will be activated as soon as possible after achieving orbit and will
operate throughout the mission. A crew member will enter the correct
mission elapsed time upon activation and change memory modules every
two days.
RME-III is the current configuration, replacing the earlier RME-I and
RME-II units. RME-III last flew on STS-31. The experiment has four zinc-
air batteries and five AA batteries in each replaceable memory module.
RME-III is sponsored by the Department of Defense in cooperation with
NASA.
STS-41 CREW BIOGRAPHIES
Richard N. Richards, 44, Capt., USN, will serve as commander. Selected
as an astronaut in 1980, he considers St. Louis, Mo., his hometown.
Richards will be making his second space flight. Richards served as pilot of
STS-28, a dedicated Department of Defense mission launched Aug. 8, 1989.
He graduated from Riverview Gardens High School, St. Louis, in 1964.
Richards received a bachelor of science degree in chemical engineering
from the University of Missouri in 1969 and received a master of science
degree in aeronautical systems from the University of West Florida in 1970.
Commissioned as a Navy Ensign upon graduation from the University of
Missouri, Richards was designated a Naval aviator in August 1970. His flight
experience has included more than 4,000 hours in 16 different types of
aircraft, including more than 400 aircraft carrier landings.
Robert D. Cabana, 41, Lt. Col., USMC, will serve as pilot. Selected as an
astronaut in 1985, Cabana considers Minneapolis, his hometown. He will
be making his first space flight.
Cabana graduated from Washburn High School, Minneapolis, in 1967 and
received a bachelor of science degree in mathematics from the Naval
Academy in 1971. He has logged more than 3,700 flying hours in 32
different types of aircraft, including the AD-1 oblique wing research
aircraft.
At NASA, Cabana has worked as the Astronaut Office Space Shuttle flight
software coordinator, deputy chief of aircraft operations and lead astronaut
in the Shuttle avionics integration laboratory, where the orbiter's flight
software is tested.
Bruce E. Melnick, 40, Comdr., USCG, will serve as Mission Specialist 1
(MS1). Selected as an astronaut in 1987, he was born in New York, but
considers Clearwater, Fla., his hometown. He will be making his first space
flight.
Melnick graduated from Clearwater High School in 1967 and attended
Georgia Tech in 1967-68. He received a bachelor of science degree in
engineering from the Coast Guard Academy in 1972 and received a master
of science in aeronautical systems from the University of West Florida in
1975.
At NASA, Melnick has served on the astronaut support personnel team
and currently represents the Astronaut Office in the assembly and checkout
of the new Space Shuttle orbiter Endeavour at the contractor facilities in
Downey and Palmdale, Ca.
William M. Shepherd, 41, Capt., USN, will serve as Mission Specialist 2
(MS2). Selected by NASA as an astronaut in 1984, he was born in Oak
Ridge, Tenn. Sheperd will be making his second space flight.
Shepherd served as Mission Specialist on STS-27, a dedicated
Department of Defense flight, launched Dec. 2, 1988.
Shepherd graduated from Arcadia High School, Scottsdale, Ariz., in
1967. He received a bachelor of science degree in aerospace engineering
from the Naval Academy in 1971 and received degrees of ocean engineer
and master of science in mechanical engineering from the Massachusetts
Institute of Technology in 1978.
Thomas D. Akers, 39, Major, USAF, will serve as Mission Specialist 3
(MS3). Selected as an astronaut in 1987, he considers Eminence, Mo., his
hometown. This will be Akers first space flight.
Akers currently serves as the Astronaut Office focal point for Space
Shuttle software development and the integration of new computer
hardware for future Shuttle missions.
Akers graduated from Eminence High School, valedictorian of his class.
After graduating from the University of Missouri-Rolla in 1975, he spent 4
years as the high school principal in his hometown of Eminence. He joined
the Air Force in 1979 and was serving as executive officer to the Armament
Division's deputy commander for research, development and acquisition at
Eglin AFB, Fl., when selected for the astronaut program.
MISSION MANAGEMENT TEAM
NASA HEADQUARTERS
Washington, D.C.
Richard H. Truly Administrator
J.R. Thompson Deputy Administrator
Dr. William B. Lenoir Associate Administrator, Office of Space Flight
Robert L. Crippen Director, Space Shuttle
Leonard S. Nicholson Deputy Director, Space Shuttle (Program)
Brewster Shaw Deputy Director, Space Shuttle (Operations)
Lennard A. Fisk Associate Administrator, Space Science and Applications
Alphonso V. Diaz Deputy Associate Administrator, Space Science
and Applications
Dr. Wesley Huntress Director, Solar System Exploration Division
Frank A. Carr Deputy Director, Solar System Exploration Division
Robert F. Murray Program Manager
Dr. J. David Bohlin Program Scientist
ESA HEADQUARTERS
Paris, France
Prof. Reimar Luest Director General
Dr. Roger Bonnet Director of Scientific Programmes
David Dale Head of Scientific Projects
Derek Eaton Project Manager
EUROPEAN SPACE RESEARCH AND TECHNOLOGY CENTRE
Noordwijk, The Netherlands
Marius Lefevre Director
Derek Eaton Manager, Ulysses Project
Dr. Klaus-Peter Wenzel Ulysses Project Scientist
Koos Leertouwer Ground/Launch Operations Manager Ulysses Project
Alan Hawkyard Integration Manager Ulysses Project
Peter Caseley Science Instruments Manager Ulysses Project
EUROPEAN SPACE OPERATIONS CENTRE
Darmstadt, Germany
Kurt Heftmann Director
Felix Garcia-Castaner Operations Department Head
Dave Wilkins Spacecraft Operations Division Head
Peter Beech Mission Operations Manager
Nigel Angold Spacecraft Operations Manager
JET PROPULSION LABORATORY
Pasadena, Calif.
Lew Allen Director
Peter T. Lyman Deputy Director
John R. Casani Assistant Laboratory Director for Flight Projects
Willis G. Meeks Project Manager
Dr. Edward J. Smith Project Scientist
Donald D. Meyer Mission Operations and Engineering Manager
John R. Kolden Integration and Support Manager
Gene Herrington Ground Systems Manager
Joe L. Luthey Mission Design Manager
Tommy A. Tomey Science Instruments Manager
JOHNSON SPACE CENTER
Houston, Texas
Aaron Cohen Director
Paul J. Weitz Deputy Director
Daniel Germany Manager, Orbiter and GFE Projects
Donald R. Puddy Director, Flight Crew Operations
Eugene F. Kranz Director, Mission Operations
Henry O. Pohl Director, Engineering
Charles S. Harlan Director, Safety, Reliability and Quality Assurance
MARSHALL SPACE FLIGHT CENTER
Huntsville, Ala.
Thomas J. Lee Director
Jay Honeycutt Deputy Director (Acting)
G. Porter Bridwell Manager, Shuttle Projects Office
Dr. George F. McDonough Director, Science and Engineering
Alexander A. McCool Director, Safety, Reliability and Quality Assurance
G. Porter Bridwell Acting Manager, Solid Rocket Motor Project
Cary H. Rutland Manager, Solid Rocket Booster Project
Jerry W. Smelser Manager, Space Shuttle Main Engine Project
Gerald C. Ladner Manager, External Tank Project
Sidney P. Saucier Manager, Space Systems Project Office
Acting Manager, Upper Stage Projects Office
KENNEDY SPACE CENTER
Merritt Island, Fla.
Forrest S. McCartney Director
James A Thomas Deputy Director
Robert B. Sieck Launch Director
George T. Sasseen Shuttle Engineering Director
John T. Conway Director, Payload Management and Operations
Joanne H. Morgan Director, Payload Project Management
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