Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://www.cosmos.ru/oct4/2007/ppt/03_04_Antonella_Barucci.pdf Äàòà èçìåíåíèÿ: Tue Dec 4 17:11:47 2007 Äàòà èíäåêñèðîâàíèÿ: Sat Dec 22 10:23:56 2007 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: jupiter

M.A. Barucci

NEO Sample R eturn Mission « Marco Polo »
Proposal to ESA COS MIC VIS ION This proposal, prepared by a joint E uropean Japa nese tea m, is supported b y 440 co nfir med scientists.

Moscow, October 3rd, 2007


Tea m l eaders: M.A. B arucci (LES IA, Paris Observatory, F) M. Yoshikawa (JSPEC/JAXA, J )
Core members : P. Michel (OCA, Nice F), J. Brucato (INAF, Nap les I), I. Franchi (Open University, UK), E. Dotto (INAF, Rome I), M. Fulch ignoni ( Univ. Paris Diderot, F), S. Ula mec (DLR, Koln D, Europe) ; J. Kawagu shi ( JSPEC/JAXA), H. Yano (JSPEC/JAXA, Japan) & R.P. Binzel (MI T, Cambr id ge, USA)


In the early solar nebula, the dust accreted to for m planetesimals a nd the planetesi mals accreted to form planetary embryos. In the asteroid belt this process was stopped when Jupiter formed.


Good selected target:
the mo st pri mitive C or D asteroid s

#
CAIs
Cho ndr ules
Euc rites Differentiat ion HED differentiation Angr ites Pallas it e

Planetes imal Differentiation
M esosiderit es

Planetary Accretion

Ma rs Ea rth


Origin of the Life:
· Th e planets of the inner Solar System experien ced an intense influx of co metary and asteroidal material for s everal hundred million years after they formed. · Th e earliest evid ence for life on Earth coin cides with the decline of this enhanced bo mbard ment. Th e fact that the influx contained vast amounts of co mplex o rganic material offers a t antalising possibility that it may be related to the o rigin o f life.


Main questions:
1) 2) 3) 4) What were the initial conditions and evolution history of the solar nebula? Which were the properties of the building blocks o f t he terrestrial planets? How did major e vents (e.g. agglomeration, heating, .....) influenced the history o f planetesimals? Do primitive class objects contain presolar material yet unknown in meteoritic samples?

5) What are the organics in primitive materials? 6) How NEO organics can shed light on the origin of molecules necessary for life? 7) What is t he role of NEO impacts in t he origin and evolution o f life on Earth?


Scientific objectives of a NEO S R
W hat are th e in iti al co nd itio ns an d evolu tio n hi sto ry of the so lar n ebu la ?
H ow NEOs and met eorit es are related to get her ? Which are t he p rop erties of th e b uild in g b locks o f terrest rial p lanet s?

Composi tion of primi ti ve mat erial

What is t he ro le of NEO im pacts in t he o rigin of life?

Ho w d oes comp osit ion vary with geo log ical co nt ext ? H ow do sp ace w eat hering and co llisions af fect NEO co mpo sitio n? Int erior

Elem ent al/Iso to pical com po sit io n

Nat ure of o rganics

Min er alo gy

Surf ace morp ho log y

Mass, gravity den sit y

In ternal st ructu re

Lan der

Orbiter

Sampl e coll ecti on & retu rn


M ARCO POLO

Baseline scenario (Option 1)
m apping

ESA JAXA
landing and sam pling

cruise phase
sam pling sy stem ERC space craft propulsion m odule Lander

NEO
rem ote se nsing package i n si tu anal yses TTC re lay

science phase

Launch re-entry phase Earth

return phase

Operations


The accessibility of NEOs
NEA ACCESSIBILITY H-PL OT

16 14 12
delta -V (k m/s ec )

Sa m ple U pd at e 02/ 2007: 3238 o b ject s wi t h H <22

PHAET HON

P/ ENCKE EPHAIST OS

10 8
Mer cur y
EROS 2002AT 4

OLJ ATO

Jupiter
WIL SON-HARRINGT ON

6 4 2 0 0
Ven us

2001S G28 6 1996FG3 1993JU3

As ter oid M ain Bel t
NEA po pula tio n (H<2 2) IT OKAWA sho rt-p er io d com e ts dor m a nt co m e ts NEA s visi te d SR m is s ion ta r ge ts

Ma rs

EART H 1

2

3

4

5

ap helio n distan ce (A U)


Baseline Marco Polo to 4015 Wilson-Harrington
Launcher : Soyuz Fregat (indirect injection) :


Selected targets/flexibility
WilsonHarrin gton 2002 AT4 2001 SG 286 1996 FG3 (double) q=1 UA Q=4.3 q=1.2 Q=2.7 q=0.9 Q=1.8 q=0.7 Q=1.4 D C - type 2-4 k m 0.3-0.4 D - typ e 0.3-0.5 D - typ e 1.4 0.43
(1) (2)

P= 6.1 hrs ? ? 3.6

C - type


Main Space craft
Science
Du st Enviro n me nt Or b ital & Rotation al Ev olu tion Mo rp ho logy, Topography Macro scale Dust & Reg o lith Size ,Sh ape ,Mass,Gr avity,De n sity In ter n al Stru cture, Stratigr aphy Macro scale co mp ositio n Macroscale Miner alogy

Hi-Re s Came ra Radio Scie nce V -NIR Spectrometer

Dust Monitor Lase r Altime te r MIR Spectrometer

Choice & characte rization of the sam pling site De scent Camera Ion Lase r Mass Anal. V olatile s De te ctor
Te xtu re Th er mal pr ope rtie s M icro scale Dust,&Reg o lith Ele me ntal composition M icro scale M iner alo g y M icro scale che mical co mp . Su b -su rface vo latiles

The rm al se nsors Ele ctron m icroscope XRD/XRF

Lander


(The Fi rst Descent: Lander Release)

(The Seco nd Descent: To uch & Go Sampling)

(2) ESA Lander (1) Arm Extended (2) T arget Marker #2 (1) T arget Marker #1

As teroid Surfac e Lander : Phila e heritage

(3) T ouc h Dow n & Sampling w ith Shoc k Abs orption w ith J oints

UHF a n t en na

As teroid Surfac e

C o d gas t h u st ers l r

Sa mp l ng sys t e i m


(Sun/Ea rth Face)
1. 4 m

(Astero id Face) Marco Po lo Spacecraft Baseline Design

20 m

2

Solar Array Panels High Ga in Antenn a 4m

2. 2 m

5m

(Capsule Face)
Star Trac ker MINER VA x2 Earth Return Caps ule ESA L ander T arget Markers Extended Arm Sampling Monitor Camera ESA Samp ler

(Io n Engine Face)

>1. 5 m

>5 m

Sc ienc e Ins trument Platform

Ion Engine Clus ter Platform

J AX A Sampler



Telescopic mast for sampling devices
The Storable Tubular Extendable Member (STEMTM) is a unique product with over 30 years of space flight heritage
-Locks in p lace whe n Deploy ed -Retractability feature
QuickTimeTM et un dÈcompresseur TIFF (non compressÈ) sont requis pour visionner cette image.

-Lig ht and volume efficie nt -Sized to fit various stengt hs and stiffness based on needs
Length: up to 14 m Diameter: 16 c m Mass: 12.8 kg

Exa mple fro m Northrop Gru mman ( model 7301)


Sequence o f Sample Co ntainer Insertio n to the Capsule

(1)
C apsule

ES A P ad B io-S ealing

Bi-Stem Arm Re traction
First Lid JAXA C ontainer

S econd Lid

(2)
Firs t Inse rtion

(3)

Bio-Se al

(4)

Se cond Inse rtion

(5)

Latch & Caps ule Se aling


Laboratory i nvesti gatio n:
High spatia l resolution and analytical precision are needed: · Examples of the type of sample processin g include preparation of polished flat surfaces (for optical, e-beam and ion beam studies), acid disso lution and so lvent extraction. · High precision analyses include determinin g trace element abundances to ppb levels and isotopic ratios approaching ppm levels of precision, nor mally with a spatial resolution of a micron or less. · Such information can only be achieved by large, complex in struments ­ e.g. h igh mass resolut ion instruments ( large ma gnets, high vo ltage), bright sources (e.g. Synchrotron) and usually requires mu lti-approach studies in order to understand the nature and history of specific components.


Conclusion:
A samp le return mission to a NEO, has the potential to revolutionize our understanding of pr imitive materials essential to understand the conditions for planet formation and emergency of life. It can provide us important information needed to develop strategies to protect the Earth from potential hazards. Moreover robotic sample return mission to NEOs will be pathfinders for sample returns from h igh gravity bodies and, later on, for human missions that might use asteroid resources to facilitate human exploration and the development of space.


MARCO POLO, the and explo rer, was m time in Euro pe the and its culture in the in China given in its

Venetian marchand entio ning fo r the first existence o f Japan acco unts o f its travels boo k "Il Milio ne".

He was refe rring to the Japan as "Cipangu"

T h e L ande r is named SI FNO S fro m the Aegean island of Sifnos. Duri ng the e arly Bro n ze Age (3000 BC), settle rs f ro m Asia Mino r came to the i sland o f Sifno s a nd meddled with the inhabitants, develo ping the Ea rl y W e s tern cu ltu re.

http://www.lesi a.ob sp m. fr/co smicvi sio n/ neo sr


Other po ssible scenario s, all i nvol vi ng So yuz Fregat


Sticky pad

ARS (Asteroid Regolith Si mulant)

10g /1 s

Increasing the applied force increases the contact with the simulant and thus increases the yield of each sample. A: 67N; B :111N; C:160 N; D:200 N
Johns Hopkins Univers ity App lied P hysics Laboratory



DEIMOS SAMPLE RETURN Sampli ng Mechani sms Co ncept
· Co ncept : To uch & Go with a co llectio n based o n gas injectio n ­ To uch & Go direct collect ion : T o avoid the anchorage reliab ility and feasib ility concerns · Quite unknown soil nature & Weak gravity · Reduction of unbalance r isk thanks to wide spread pad and penetrator retractability. ­ Sample co llected thanks to gas injectio n · A penetrator enters the ground and inject a gas flow · T he ejected material is gu ided towards receptacles · Sample down to few cm below the surface ­ Co mpatible with redundancy ­ Access to internal (few cm) materials


Such a Sample Return mission would p erfo rm fi rs t-cl ass scien ce in vestigat te s t/v a lid a t e th e f o ll o w in g k e y functions/technologies r

allo w us to ions an d to in n o v a tiv e el evan t :

· Guidan ce, n avi gation, control and autono my approach of the mother sp acecraft durin g the cruise and target app roach ph ases. · Navi gation sensors and cont rol strategies fo r the soft and precision landing and for the obstacl e avoid ance (to a li mited extend, du e to the different gravity and rel ati ve d yn ami cs conditions and for the lack of at mosphere).


· Robotic devices (e. g., driller, robotic arms), containers and mechanis ms in vol ved in the sample collection, handling, sealing, transfer, storage. · Hi gh-sp eed reentry capsule and related op erations. · To test new technolo gy develop ments: on board artificial intelligen ce, teleco mmunication, in situ energy, re-entry velocit y, planetary protection..... · To p repare new adequ ate laboratory facilities for extraterrestrial sample anal ysis.


MISSION SCENARIO (option 2)
JAXA ESA cruise phase
CCMM ESA m odule re le ase for landing ERC Lande r NEO SCEM TTC re lay

manoeuvre phase

rem ote se nsing package space craft propulsion m odule

rem ote se nsing activ ity

sam ple caniste r in situ analy se s and sam pling
canister migration canister ejectio n

science phase

Earth re-entry phase
canister capt ure

return phase

manoeuvre phase

SCE M: Sample Conditioning and Ejection Mechanism

CCMM: Canister Capture and Migration Mechanism


· The S torable Tub ular Exte ndable Me mber (STEMTM) is a unique product with over 30 years of space flight herita ge includi ng pro gra ms suc h as Vo ya ger, GPS IIR, Hubble Space Telescope and Mars Pathfi nder. These prod ucts are available as the most si mple STEM mec ha nis m or the s maller package o f the B I-STE MTM or the Interlocked B I-STE M whic h provides improved torsional rigidity and allows longer deployed lengths. · STEM has bee n produced fro m 12 millimeter to 50 millime ter diameters and is ma nufactured in beryllium copper for a nte nna eleme nts a nd stainless steel for structural applications.


(Mo dified Spacecraft Co nfiguratio n fo r Sub-surface Sampling by Lander)
Earth Return Caps ule Vo lume for Bio-Sealing ESA L ander Can is ter Catc her T arget Markers

Can is ter Catc her Lander Sample Can is ter Spac ecraft Samplers Can is ter Ejec tion Retrac ted Mec hanis m ESA L ander Sub-s urfac e Drill As teroid Surfac e

("Catch-Ball" Operatio n) (Option 2)