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The Second International Conference on the Exploration of Phobos and Deimos
The Next Asteroid Sample Return
Mission of Japan: Hayabusa-2
14-16 March, 2011
NASA Ames Research Center, Mountain View, CA, USA
Presented by Seiji SUGITA (Univ. of Tokyo)
Prepared by Makoto Yoshikawa, Hajime Yano (JAXA)
and Hayabusa-2 Pre-project Team
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I am sorry for not attending this
very interesting meeting.
We, Hayabusa-2 pre-project team,
just have finished SDR (System
Definition Review) and we will
have some more programmatic
reviews this week and later this
month.
After those reviews, we will move
Makoto Yoshikawa into the Phase-B, so now is quite
(Hayabusa-2 Pre-project leader)
important period for us.
&
Two Itokawa Models
Thank you!
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Successful Hayabusa
2005
2003
S-type NEO Itokawa
2010
Asteroid Samples Were Recovered!!
Initial sample analysis results were reported at LPSC last week4
Summary of Current Status
• Hayabusa mission finished in 2010 (except for the curation and
the sample analysis).
• We have a lot of experiences from Hayabusa mission, and now
we are ready to start another sample return mission with more
robust and reliable systems.
• From the point of science, the sample return from a C-type
asteroid is very important for understanding the origin and
evolution of the solar system and life.
• Therefore, we have been planning Hayabusa-2 mission as a
sample return mission from a C-type asteroid.
• At the end of 2010, the budgetary request for Hayabusa-2 project
to start from the next fiscal year (April 2011~) was approved. At
present, Hayabusa-2 is a pre-project (Phase-A), and it will turn to
a formal project (Phase-B) by the end of March 2011 (this
month).
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Mission Objectives: Hayabusa-2
1. Science
"Where did we come from? "
• The origin and evolution of the Solar System
• The original material of terrestrial life
• The origin of water of the Earth ocean
2. Engineering
Develop original and unique technologies for solar system
exploration
• technologies verified by Hayabusa  more reliable, robust
• New challenges  physical interaction (impactor)
3. Exploration
Push the limit where human-beings can reach
• Deep space round trip
• Spaceguard, Resource utilization, Precursor for human missions….
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There Are Several Spectral Types of
Asteroids by Heliocentric Distance
D-type
・Richer in organic materials
・Tagish Lake?
S-type like
objects
S-type
・Rock and metals
・Ordinary chondrite
C-type like
objects
Distance from the Sun
・Organic, hydrated minerals
・Carbonaceous chondrite
C-type
Asteroid classification by spectral types
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Primitive Body Exploration Program
Considered in Japan
Post Hayabusa
Hayabusa
Hayabusa-2
2003 - 2010
Hayabusa-Mk-II
2014-
1999 JU3
Itokawa
Wilson-Harrington?
D-type Asteroid?
C-type
S-type
Main Asteroid Belt
D-type
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Target Asteroid : 1999 JU3
Rotation period: 0.3178day (~7.6 h)
Orbit
Itokawa
（λ，β)＝(331, 20)
Axis ratio = 1.3 : 1.1 : 1.0
Size : 0.922 ± 0.048 km
Albedo : 0.063 ± 0.006
Mars
Earth
H=18.82 ± 0.021, G=0.110 ± 0.007
Type : Cg
Shape model by Kaasalainen
(by Mueller
et. al)
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Spectrum of 1999 JU3
by Faith Vilas (AJ, 135, 1101, 2008)
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Mission Outline of Hayabusa-2
Launch
June 2018 : Arrival at 1999 JU3
Global observation of the asteroid,
deployment of small rover/lander,
multiple samplings
July 2014
Mothership carries
an impactor.
New Experiment
Sample analysis
Earth Return
Dec. 2020
Dec. 2019 : Departure
2019
The impactor collides to the
surface of the asteroid.
Further exploration
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Hayabusa-2 Spacecraft: New Evolutions from Lessons Learned
of Hayabusa and Adaptation to a Carbonaceous Asteroid
HGA: Planar Antenna
Target asteroid
1999 JU3 (C-type)
Near IR spectrometer
IR camera (thermal)
Impact Sampling
etc.
Launch Windows:
2014 – 2015
C-type
Changes from Hayabusa
Reaction Wheels
Chemical Thrusters
Ion engines
Software
etc.
Impactor
Rover: MINERVA-2
Lander : MASCOT
Stay Period:
Up to 18 months
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Nominal Payloads That Produce Science
Payloads
Specifications
Multiband Imager
(AMICA)
Wavelength: 0.4 – 1.0 µm, FOV: 5.7 deg x 5.7 deg,
Pixel Number: 1024 x 1024 px
filter (ul, b, v, w, x, p) (Heritage of Hayabusa)
Near IR Spectrometer
(NIRS3)
Wavelength: 1.8 – 3.2 µm, FOV: 0.1 deg x 0.1 deg
(Heritage of Hayabusa, but 3µm range is new)
Thermal IR Imager
(TIR)
Wavelength: 8 – 12 µm, FOV: 12 deg x 16 deg, Pixel
Number: 320 x 240 px (Heritage of Akatsuki)
Laser Altimeter
(LIDAR)
Measurement Range: 50 m – 50 km
(Heritage of Hayabusa)
Sampler
Minor modifications from Hayabusa-1
(Heritage of Hayabusa)
Small Carry-on
Impactor
Small, deployed system to form an artificial crater on
the surface (New)
Small Rover
(MINERVA-2)
Almost same as MINERVA of Hayabusa-1
(possible payload: Cameras, thermometers)
(Heritage of Hayabusa)
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International Collaborations under Discussion
Followings are potential collaborations under discussion:
* DLR/CNES : MASCOT = Mobile Asteroid Surface Scout
(Small lander of ~10kg Mass)
* NASA : Mini-M3 = mini Multi Mineral Mapper
(Imaging spectrometer)
RAD (Radiometer)
USO (Ultra stable oscillator)
* Europe : MAPIS = Marco-Pole Imaging Spectrometer
(Imaging spectrometer)
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Hayabusa-2 Mission Scenario
year
2014
2015
month 07 12
06 2016
2017
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Spacecraft
2018
06
2019
08 12
2020
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IES operation
(Back-up windows)
Launch
Earth Swing-by
Arrival at Science
1999JU3 observation
,
Sampling
Departure
from 1999
JU3
Earth
return
IES operation
Impactor
Option of shorter stay & earlier return
is also under consideration.
Departure
from 1999
JU3
Earth
return
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Summary
• The 2nd asteroid sample return mission
• Hayabusa-2 has been approved and will soon start
the Phase-B.
• The launch window is in 2014 (with back-ups in
2015).
• It will investigate 1999 JU3, a small C-type NEO,
in-situ in 2018-19, and bring its samples back to the
Earth in 2020.
• We would like to establish good international
collaborations.
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You Are Cordially Invited to….
ACM (Asteroids, Comets, Meteors) 2011 !!
• Date: 17-22 July, 2011
• Venue: Niigata, Japan
• Abstract Deadline:
19 April, 2011
• Topics include
"Sample return
from small bodies"
• For details, please search "
ACM 2011" on the web.
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