New Millennium Program (NMP)
Andrew Foster

Deep Space Missions
A Vision of the 21st Century Space
Exploration
In the next century, to travel
outside of the Solar sytem may still be too time consuming for the short
life period of human beings. However the well developing high technologies
and clever arrangement might bring in a new vision for the 21st Century
Space Exploration.
Beside the expensive human flights,
many scienttific studies inside the solar system, the Sun, the planets,
the asteroids and comets, and other objectives
can be organized into a "Network"
mission.
A single spacecraft might be able
to release multiple (10 - 15?) landers or penetrators or some new form
of sientific investigation units to a certain area in space.
And multiple simultaneous spacecrafts
will be able to form a powerful "network".
This "network" will provide comprehensive
studies of dynamic, complex phenomena.
To prepare such a new era of space
exploration, to further create the fast, flexible, low cost and high efficiency
access to space, new technologies will be critical.
New Millennium Program - Technology-validation
Mission
The goal of the NMP is to identify
and test advanced technologies that are needed in the 21st century space
exploration.
Through a series of deep space
and earth orbiting flights, NMP will demonstrate those promising but risky
new technologies in space to prove that they work.
Once validated, the new technologies
pose less of a risk to missions that would like to use them to achieve
their scientific objectives.
During NMP flights, scientific
data will also be returned as a dual goal for this program.
DS1, DS2 and EO1 missions are
on the way.
DS1 - First Deep Space Mission
DS1 Spacecraft
encounts Comet
With launch scheduled in July 1998
on a Delta-7326 rocket, the DS1 spacecraft will fly by and gather data
about an asteroid, then Mars, and finally a comet.
Fly by Asteroid McAuliffe
in Jan. 1999
DS1 will fly by near-Earth asteroid
McAuliffe at just 5 - 10 km above the surface. - the smallest flyby distance
of a celestial body accomplished by any spacecraft.
During the close flyby, DS1 will
capture images, measure baasic physicaal properties such as mineral composition,
dimensions, shape, surface features, and reflectivity; and search for changes
in the solar wind as it interacts with the asteroid.
Like comets, asteroids are very
difficult to observe from Earth as they ars so small and distant.
Pass by Mars in April 2000
In April 2000, a pass by Mars will
be used for a gravity assist, transferring energy to DS1 to help speed
it on the way to its comet encounter.
The flyby Mars provides another
chance to test DS1's unique sceince instruments. The spacecraft may also
encounter and image one of the two tiny moons of Mars, Phobos or Deimos.
Encounter Comet West-Kohoutek-Ikemura
in June 2000
Comets are nearly invisible except
when near the Sun, where a comet's solid nucleus changes from solid to
gas without becoming liquid. Glowing dust and ion tails can extend millions
of kilometers as the comet streaks by in its orbit.
Flying close to a speeding, luminous
comet is a risk, but much can be learned.
DS1 will take close-up pictures
of West-Kohoutek-Ikemura, determine the size and shape of the nucleus,
and study the coma.
If all is well, DS1 will continue
on in space, perhaps encounting other asteroid or comet.
Advanced Technology of DS1
Ion Thruster
Solar Concentrator
Arrays
Autonomous Miniature
Camera/
Navigational System
Spectrometer
First NMP technology validation
mission.
First close-up images of a
comet.
Shortest flyby distance of
any solar system body.
First use of high-performance,
solar electric ion propulsion.
This is the first time in the
history of solar system expolration that solar electric propulsion is used
as the primary means of propelling a spacecraft toward its destination.
With electrical propulsion,
we ionize to xenon and then electrically accerate it to a speed of ~30km/second.
When the xenon ions are emitted at such a high speed, they push the spacecraft
in the opposite direction.
The ion propulsion system will
be powered by solar array panels .
Solar electric propulsion thus
allows spacecraft to be lighter and less expensive, and to be launched
on smaller, cheaper launch vehiles
First use of autonomous navigation
in deep space.
DS1 will use an onboard, autonomous
system to navigate to celestial bodies.
The system will make navigation
decisions about spacecraft trajectory and targeting of celestial bodies
with little assistance from Earth.
That means the spacecraft will
guide itself to pinpoint and control when and where to encount a planet,
moon, asteroid or comet . . .
To imagine a car driving itself
across the United States from los Angeles tto Washington D.C., and parking
itself in a designed space upon arrival - after having completed the entire
trip on one tank of fuel.
That's the power of combining ion
propulsion and autonomous navigation.
Other advanced tecnologies
Miniature camera/Spectrometer.
Experiment with "intelligent"
power switch.
Microelectronics experiment
to consume less power.
Diagnostics for the Ion Thruster.
Experimental "cable free" incooperation
of microelectronics into spacecraft.
"Artificial Intelligence" software
experiment.
Ka-band Radio Frequency experiment.
Spacecraft "health" monitoring
experiment.
Instrument to measure Solar
Wind and Comet Environments.
Beacon Monitoring Operations
experiment.
DS2 - Second Deep Space Mission
(Mars Microprobe)
Mars Microprobes riding
with MSP 98 Lander
Riding with MSP 98 Lander
During its journey to Mars , the
two microrpobes will be attached to the Mars Surveyor 98 Lander (MSP 98
Lander), underneath the spacecraft's solar panels.
This ride to Mars for these
two basketball-sized planetary penetrators cost
$2.8 million. However since they
are too small to occupy a special spacecraft. they will be quite happy
to take the ride with MSP 98 Lander.
Targeting Martian South
Polar Ice cap
Microprobes targeting
Mars South Polar Ice Cap
After an 11 months cruise, the microprobes
and MSP 98 Lander will arrive at Mars in Dec. 1999. They will be near the
southern summer solstice.
The prime landing site of the Lander
is located at the north most boundary of the Martian Polar Layered Terrain
(PLT). ThePLT is of significant scientific interest due tto its role as
a reservoir for water and other volatiles on Mars..
The Microprobe landing site will
be just outside the permanent carbon deoxide south polar ice cap. It may
impact anywhere 50 - 100 km from the Lander.
Just prior to atmosphere entry,
the Lander will seperate from its cruise ring. The force of seperation
will initiate mechanical pyro devices, which in turn will seperate the
microprobes from the cruise ring about 18 seconds later.
Entry, Descent and Impact
Structure
of Mars Microprobe
The microprobe entry, descent and
impact system is single stage from atmosphere entry until impact.
The aeroshell uses an advanced
ablative material, which can withstand temperature associated with heating
rate up to 300 W/cm2. This aeroshall will maintain a constant aerodynamic
shape and be carried to the surface. Upon impact the aeroshall will shatter
leaving the aftbody clear for communications with the Mars Global Surveyor
(MGS) spacecraft.
The microprobe is expected to hit
the surface with an impact velocity of 160 to 200 m/s, an impact incidence
angle < 25 degree, and an angle of attack < 12 degree.
Upon impact , the penetrator well
seperate into a forebody and a aftbody. that are connected via a flexible
cable system.
The forebody (weight > 900 gram)
is expected to penetrate to a depth of 0.3 - 2 m for soil types that vary
from frozen-soil to very loose fine-grained soil. The forebody must also
withstand a peak rigid body shock of up to 30,000 G's. It will be buried
in the soil and operate in temperature range from 0 to -120 oC
.
The aftbody )weight >1050gram) will
stay on the surface and withstand a peak rigid body shock of < 80,000
G's. The aftbody is designed to operate in temperature range from 0 to
-80 oC.
Scientific Experiments
The forebody includes:
- Microcontroller.
- Power
microeletronics.
- Subsurface
sample/water detection experiment.
- Two
temperature sensors.
- Three
axis impact accelerometer.
The Aftbody includes:
- Two
lithium batteries.
- Microtelecommunication
system (telecom-on-a-chip) with antenna.
- Meteorological
pressure sensor.
- Descent
accelerometer.
- Sun
detecttor.
Upon impact, 3 accelerometers will
measure the deceleration of the forebody before it comes to rest in the
soil. This data may provide clues to climate history if geological stratification
or an ice layer is detected below the surface.
It will also show the depth of
probe penetration.
Within minutes of impact, a micromotor
will drive a small drill out of the side wall of the penetrator. Soil tailings
from the drill will be pulled intto the water experiment sample cup.Collection
of a subsurface soil sample is very important for future missions and the
search for life on Mars.
The water experiment will be performed
to detect the presence of subsurface ice. It will also characterize subsurface
soil composition.
The probe will collect temperature,
pressure, and Sun detection measurements every hour for at least the first
2 Martian days. It will continue until the probe battery is depleted (About
20 additional sols)
The data collected will be stored
in the probes' microcontrollers until transmitting to MGS spacecraft. MGS
will then relay the microprobe data to NASA's Deep Space Network on Earth.
EO1 - Earth Orbitor 1 Mission
Earth
Orbitor 1
EO1 is an advanced land imaging
mission that will demonstrate new instruments and spacecraft systems.
EO1 will be launched in the first
half of 1999.
(More missions will coming)
DS 3 - Third Deep Space Mission
If approved by NASA, revolutional
tecnologies will enable free-flying spacecraft to function as a space-based
interferometer.
DS 4 - Fourth Deep Space Mission
If approved by NASA, for the first
time, a spacecraft will land on a comet and retrieve a sample.








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