Experimental approach of dust processing in protoplanetary disks ...

Experimental approach of dust
processing in protoplanetary disks and
comparison with returned samples
Mathieu Roskosz
Workshop MarcoPolo-R, December 2012, CNES-Hqs
Mathieu.roskosz@univ-lille1.fr

Recuits sur des précurseurs de
diopsides (740°C, 10j)
(thermal annealing)

ISM Vs. Protoplanetary disk
Evaporation/condensation
Thermal annealing
Amorphous-Crystalline
F. Kemper, W. J. Vriend, and A. G. G. M. Tielens
Ap. J. 609, 826–837
R. van Boekel, et al.
Nature 432, 479-482

A controversial mineralogical zoning
VLT
Spitzer
An inner disk dominated
by pyroxenes
An outer disk dominated
by olivine
Detection of SiO 2 polymorphs
Watson et al., ApJS 180 (2009) 84-101
Sargent et al., ApJS 182 (2009) 477-508
Sargent et al., ApJ 690 (2009) 1193-1207
R. van Boekel, et al.
Nature 432, 479-482

Experimental details
• 970-1070 K
• A few hours to 2 months
• Glasses and homogeneous
nanoporous volatile-free
gels
• In situ HT X-ray Diffraction
• TEM
• Conventional XRD
• Spectroscopies (Raman and IR)

Quelques Subsolidus résultats: crystallization 740°C, 10j
Dynamical annealing of MgSiO 3
(Roskosz et al., ApJ (2009))

Local and bulk cation dynamics control low-T
dust crystallization
• Even starting from an enstatite precursor, below 700°C, only forsterite forms…
MgSiO 3 amorphous Mg 2 SiO 4 +SiO 2
(Roskosz et al., A&A, 2011)
Mobility decouplings in solids explains the metastable low-temperature
formation of the MgO-(CaO)-rich phases
(Roskosz et al., JNCS (2005) 351, 1266-1282; JNCS (2006) 352, 180-184)

Metastable low-T assemblages identified "
in Stardust samples

Metastable low-T assemblages identified "
in Stardust samples
Conclusion et applications
Al
Si
SiO 2
1 µm
Pt
Mg
S
Fe
500 nm
« Fo 58 »
« Fo 93 »
Close association of olivines and quartz polymorphs (micrography H. Leroux)

Recuits sur des précurseurs de
diopsides (740°C, 10j)
(irradiation)

Irradiation in astrophysical environments
• SN shock waves
• Cosmic rays
• X-winds
• Solar flairs, outflows…
Irradiation :
interactions particles-matter
(photons, electrons, ions) inducing
modifications of the material
• Grain size distribution
• Lifetime
• Structure
• Composition
• Porosity
• Optical properties
• Isotopic signatures
Lin et al., 1994, Adv. Space Res,
20, 465
Implantation
Sputtering

Electron irradiation
Transmission
Electron
Microscope(MET)
• Irradiation and in situ characterization
(microstructure, crystallinity, composition).

Electron irradiation:
Amorphization, radiolysis, chemistry
Chemical changes associated with amorphization
Phase
transition
Olivine
MgO
+SiO 2
1 µm
(Carrez et al. 2002)
Irradiation of MgSiO 3
composition at 300 keV
Oxygen bubbles formation
Carrez et al., 2001
San Carlos olivine irradiated :
Differential loss of the different elements.
Structure-dependent kinetics

Itokawa Dust particules collected from the
Hayabusa mission
Amorphization,
In situ reduction of iron from
minerals into metallic nuggets,
Noble gas implantation…
A closer look at experimental data
may help to quantitatively describe
the space weathering
Noguchi et al., Science, 2011

Electron irradiation of OM’s
Polyethylene terephthalate (PET) is a
semicrystalline symetrical arrangement
of aromatic groups and aliphatic chains
Comprehensive description of
irradiation-induced modifications of the
IOM in relation with their D/H
signatures
PhD thesis of Boris Laurent, UMET in coll. MNHN
http://umet.univ-lille1.fr/Projets/FrIHIDDA/
12 keV, e - , PET, 2500 nm

Electron irradiation of OM’s
IR spectra of electron-irradiated PET at 30 keV
EPR spectroscopy of irradiated PET
showing the appearance of mono- and
biradicals
IR image of the growing band at 1600 cm -1 in
electron-irradiated PET at 30 keV
Laurent et al. coming LPSC

Electron irradiation of OM’s:"
Waiting for MarcoPolo-R…
D/H ratios of irradiated PET as a function of Dose:
Several hundreds permil fractionation, attainment of a steady state (??)
For a detailed study of the correlations between irradiation, catalysis,
structural and D/H modification of OM, please attend the coming LPSC
Laurent et al. coming LPSC

Thanks to
• H. Leroux, B. Laurent, J. Gillot, UMET
• L. Rémusat, F. Robert, MNHN
• H. Vezin, LASIR

Experimental approach of dust
processing in protoplanetary disks and
comparison with returned samples
Mathieu Roskosz
Workshop MarcoPolo-R, December 2012, CNES-Hqs
Mathieu.roskosz@univ-lille1.fr

Exemple 1: composition enstatite
Cristallisation sous la température de transition vitreuse
a
b
c
200 nm

Durée de vie de l’assemblage Forsterite+SiO 2
Thickness ^2 (microns)
120
100
80
60
40
20
580MPa
450 MPa
210 MPa
1 Wt% H 2 O
1000°C
Thickness^2 (microns)
25
20
15
10
5
nominally anhydrous
0,1 Wt% H2O
1 Wt% H2O
210 MPa
1000°C
thickness^2 (microns)
700
600
500
400
300
200
100
0
0
0 10 20 30 40 50 60 70 80 90 100
time (h)
1450°C
1400°C
1350°C
0 Wt% H 2 O
1 bar
0 20 40 60 80 100 120
time (h)
0
0 10 20 30 40 50 60 70 80 90 100
time (h)
Fo+SiO 2 DOIT se transformer en
enstatite
La vitesse de cette transformation
dépend fortement de P, H 2 O, et T
Que se passe-t-il à basse P, T et
sans eau (sous 1000°C) ?
Data from Yund, 97, CMP; Fisler et al., 97, PCM

Durée de vie de l’assemblage Forsterite+SiO 2
Recuits sur un assemblage de fin grains de forsterite encapsulés dans une
matrice de silice pure formée par sol-gel.
Recuits à 1000°, 1100° et 1250°C jusqu’à 1 mois
Les extrapolations arrhéniennes des données HP ou HT avec et sans eau
prédisent une vitesse de croissance de la couche d’enstatite d’au moins
10 -11 m.s -1 à 1100°C

Durée de vie de l’assemblage Forsterite+SiO 2
500 nm 200 nm
Moins de 4 10 -16 m.s -1
Pourtant la diffusion cationique
opère (murissement des textures)
La nucléation d’enstatite est
inhibée à l’interface
Fo/SiO 2 par un
ΔV global de -6%
En l’absence de pression de
confinement et d’eau
L’assemblage Fo+SiO 2 peut être
préservé à T

Mineralogical zoning

Conclusion et applications

Mineralogical zoning

Irradiation in astrophysical environments
• Nature des particules (photon, électrons, ions)
• Flux des particules (particules cm -2 s -1 )
• Fluence (particules cm -2 )
• Spectre d’énergie (eV, keV or MeV ?)
Stone et al., 2008, Adv. Space Res, 454, 71
Lin et al., 1994, Adv. Space Res, 20, 465

Irradiation par des ions: exemple 2/3
amorphisation
Conditions
experimentales:
He sur olivine
Energie: 4 keV
5 10 16 ions/cm 2 10 17 ions/cm 2
Implantation
5 10 17 ions/cm 2 10 18 ions/cm 2
Porosité des
poussières
Implantations de gaz
rares
Réduction de la taille
des poussières dans
l’ISM ?
Surpression, fracturation
Demyk et al., 2001,
Carrez et al., 2002

Le grand recyclage stellaire
X