A STUDY OF DUST GRAIN FORMATION A ROLE OF MINOR ELEMENTS
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1 A STUDY OF DUST GRAIN FORMATION A ROLE OF MINOR ELEMENTS November 9, 2011 Grain Formation Workshop Akemi Tamanai (KIP, Universität Heidelberg) Harald Mutschke (AIU Jena) Jürgen Blum (IGEP, TU Braunschweig) Annemarie Pucci (KIP, Universität Heidelberg)
2 Outline Introduction Dust Grain Observed spectra Spectra by meteorite Questions Condensation models Objective Experiment Samples Experimental setup Results Summary & Outlook
3 Dust Grain Dust grains play important role in many astronomical environments Molecular clouds maintain thermal balance Planet formation the building blocks of planetesimals The study of interplanetary dust particles (IDPs) and meteorites reveals a large variety of dust grains (e.g.) Carbonaceous Chondrite Allende (CV3) Fe-rich olivine ((Mg 0.55 Fe 0.45 ) 2 SiO 4 ) Hypersthene (MgFeSiO 3 ) Diopside (MgCaSiO 3 ) Pervoskite (CaTiO 3 ) Anorthite (CaAl 2 Si 2 O 8 ) Chromite (FeCr 2 O 4 ) Melilite (Ca 2 Al 2 SiO 7 ) Ilmenite (FeTiO 3 ) Wollastonite (CaSiO 3 ) Corundum (Al 2 O 3 ) Rutile (TiO 2 ) Tistarite (Ti 2 O 3 ) Spinel (MgAl 2 O 4 ) Phyllosilicates (talc, anthophyllite, ) Fullerene-like carbon. more (Jarosewich et al. 1987; Nagahara et al. 1987; Brearley 1996; Rubin 1997; Harris et al. 2000; Nozawa et al. 2009; Ma et al. 2010)
4 Observation Spitzer HD Disk Spectral Model HD (A5 star) 40 % silica and tektite 35% olivines and pyroxenes Lisse et al Lisse et al HD (F3/5 binary) 29 % olivines, 14 % pyroxenes, 12 % amorphous silicate 21 % FeS, 12 % ice Warm asteroidal dust (T=450K) at 1.8 AU Icy dust at 4-9 and AU HD69830 (K0V) Beichman et al. (2005): Spitzer IRS T(dust) ~ 400K M(dust) ~ 1000 zodi Tamanai & Mutschke 2010
5 Normalized Extinction Normalized Extinction Spectra obtained by meteorites Fe-rich Olivine Allende Log wavelength [ m] Carbonaceous Chondrite Allende CV3 Fe-rich olivine from Sri Lanka (Fo 80 ) Ferrous olivine in Allende is Fo (Johnson et al. 1990) Fe-rich Olivine NWA4759 Carbonaceous Chondrite NWA 4759 CV Log wavelength [ m] Tamanai et al. in prep.
6 Questions Questions with respect to dust formation and evolution processes How dust grains have undergone chemical and physical metamorphosis and evolved during the chemical transformation in different environments??? Q1 What is the highest temperature condensation material? Q2 How does silicate dust formation take place? Q3 How much silicates are formed? Q4 Does silicate formation start by surface growth on the high temperature condensates such as spinel and corundum or directly from a gas phase?
7 Cont. Model Calculation Corundum (Al 2 O 3 ) Spinel (MgAl 2 O 4 ) Gehlenite (Ca 2 Al 2 SiO 7 ) Diopside (CaMgSi 2 O 6 ) Forsterite (Mg 2 SiO 4 ) Enstatite (MgSiO 3 ) Troilite (FeS) Pressure vs. temperature variation in the mid-plane of the solar nebula at yr, yr and 1, 2, yr (dashed green lines, from left to right). Full red lines are stability limits of abundant minerals and (water) ice. (The model calculation of the evolution of an accretion disk around a star with 1M by H.-P. Gail.)
8 Model Calculation for Dust Grains Dust condensation models Theoretical approaches The abundances of condensates as a function of T for a single gas pressure (P gas =10 4 dyne/cm 2 ) Mg 2 SiO 4 k-al 2 O 3 Equation of state calculations (more details in Allard et al & Ferguson et al. 2005) (Ferguson, J.W., private communication: PHOENIX)
9 Objective Investigating the optical properties of chemical compounds which contain minor elements (Ca, Na, Ti, Li, Al) in order to clarify dust grain evolution (chemical pathway) Yardstick experiments Back up the condensation experiments e.g. Pyroxene (XYSi 2 O 6 ) Possible cations Mn, Cr, Al, Na, Li, Y A rare pyroxene the mineralogy of meteorites with isotopic anomalies in discussions (Cowley 1995)
10 Target Species Al-compounds Al 2 SiO 5 (Kyanite) Al 2 O 3 (corundum) + SiO 2 (quartz) Al 2 SiO 5 (kyanite) Al 2 TiO 5 (Titanate) (Tamanai et al. 2009) Al, Li, Na-compounds LiAlSi 2 O 6 (Spodumene) NaAlSi 2 O 6 (Jadeite) NaAlSi 2 O 6 (jedeite) + SiO 2 (quartz) NaAlSi 3 O 8 (albite) Kyanite Spodumene Jadeite
11 Aerosol Spectroscopy Experimental Setup Particle size: <1 m N 2 -gas Path length: ~18m Wavelength range: 2-50 m Sampling: Polyester capillary pore membrane filters Tamanai et al. 2006, 2009, 2010
12 Normalized Extinction Al-compounds Al 2 SiO 5 (Kyanite) CsI Aerosol Red-shift (CsI spectrum) Disparity in these spectra Possible reasons: - Suspended particles - Segregated well in the CsI pellet - Containing larger aggregates in the aerosol experiment Log wavelength [ m] Si-O vibrations: 9.88, 10.49, 11.10, 13.66, m Al-O vibrations: m
13 Normalized Extinction Al 2 SiO 5 (Kyanite) vs. Al 2 TiO 5 (Tialite) Al2TiO5 Al2SiO5 Comparison with a Al 2 TiO 5 spectrum Ti-O stretching m Al-O vibrations: m 22.2 m Log wavelength [ m] Pseudobrookite structure X 2 YO 5 (X, Y: Fe 2+, Fe 3+, Mg, Al, Ti, Si) (
14 Normalized Extinction Al, Li, Na-compounds LiAlSi 2 O 6 (spodumene) CsI Aerosol Log wavelength [ m]
15 Normalized Extinction NaAlSi 2 O 6 (Jadeite) CsI Aerosol Log wavelength [ m]
16 Normalized Extinction LiAlSi 2 O 6 (Spodumene) vs. NaAlSi 2 O 6 (Jadeite) LiAlSi2O6 NaAlSi2O Log wavelength [ m]
17 Summary Performed the mid-ir extinction measurements of chemical compounds containing minor elements for benchmark use --- Al 2 SiO 5 (kyanite) --- LiAlSi 2 O 6 (spodumene) --- NaAlSi 2 O 6 (jadeite) Outlook Taking into account of minor elements in condensation experiments Investigation of particle morphology --- Separating each morphological effect (size, shape, agglomeration) and measuring the absorption spectra
18 Acknowledgement MPIA Prof. Th. Henning Dr. C. Jäger Universität Heidelberg (ITA) Prof. H.-P. Gail IAU Jena Ms. G. Born Mr. W. Teuschel Hokkaido University Prof. T. Yamamoto Deutsche Forschungsgemeinschaft (DFG)
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