GRAVITATIONAL INSTABILITY ON PROPAGATION OF MHD WAVES INASTROPHYSICAL PLASMA
Alemayehu Mengesha Cherkos1,2 AND S. B. Tessema 1,2
1. Entoto Astronomical Observatory and Space Science Research Center, P.O. Box 8412, Addis

Ababa, Ethiopia
2. Department of Physics, Kotebe College, P.O. Box 31248, Addis Ababa, Ethiopia(alexye9@yahoo.com)
Abstract
We determine the general dispersion relation for the propagation of magnetohydrodynamic (MHD)
waves in astrophysical plasma by considering the effect of gravitational instability and viscositywith anisotropic pressure tensor and heat-conducting plasma. Basic MHD equations have been
derived and linearized by the method of perturbation to develop the general form of dispersion
relation equation. Our result indicates that the transverse propagation of waves in such a plasma isaffected by the inclusion of heat conduction. For wave propagation, parallel to the magnetic field
direction, we find that the fairhose mode is unaffected, whereas the mode corresponding to thegravitational instability is modified in astrophysical plasma with anisotropic pressure tensor being
stable in the presence of viscosity and strong magnetic field at considerable wavelength.

Study of solar cycle variation and its impact on critical frequency of F2 layer
P. K. Purohit1and Roshni Atulkar1
National Institute of Technical Teachers' Training and Research, Bhopal – 462002, MP, India.

1

The period of approximately 11 year cycle of solar activity is characterized by the rise and fall in the numbers
and surface area of sunspots. We observed a number of other solar activity indices, including the 10.7 cm radio
flux, solar Mg II core to wing ratio, relative sunspot number Rz and solar flare index geomagnetic activity thatvary in association with the sunspots for solar cycles 23 (1996–2008). This paper presents an analysis of the Fregion variability of the ionospheric F2 layer critical frequency (foF2) at Australian mid latitude ionosonde
station, Hobart (42.88° S and 147.32° E) during the period 1996 – 2008 of solar cycle 23. The diurnal, monthly,and yearly. characteristics of ionospheric F-region parameter foF2 have been studied in detail. We also
compared the dependence of foF2 on solar activity indices by using a correlation analysis, and showed asignificant linear relationship between the foF2 values and Solar indices. The foF2 variation is strongly
influenced by solar activity with about an 11-year solar cycle from the solar maximum to solar minimum.

Table 1. Correlation of foF2 with solar indices during different phases of solar cycle 23.
Geomagnetic Indices Vs Fof2.

Correlation

Flare Index-foF2

0.85

Rz-foF2

0.92

F10.7-foF2

0.93

Mg II c/w-foF2

0.88

Figure – 1: Monthly variation of solar indices with criticalfrequency foF2 during Solar Cycle 23.

Figure-3: Behavior of critical frequency foF2 and solar
indices during the solar cycle 23.

Figure–2: Annual variation of solar indices with criticalfrequency foF2 during Solar Cycle 23.

Figure – 4: Scatter and Correlation of foF2 with Flare index,
sunspot number (Rz), Radio flux (F10.7) and Mg II core to
wing ratio during the solar cycle 23.

References[1] Adler N O et al 1997., Solar cycle length variation: its relation with ionospheric parameters, Journal of
Atmospheric and Solar-Terrestrral Physics, Vol. 59, No. 2, pp. 159 162.[2] Bruevich E.A.et al 2011., Changed
Relation Between Radio Flux F10;7 And Some Solar Activity Indices During Cycles 21 – 23, Solar and Stellar
Astrophysics (astro-ph.SR.[3] Bilitza D. 2000The importance of EUV indices for the international reference
ionosphere. Phys Chem Earth (C), 25: 515–521[4] Sethi N. K., Goel et al 2002Solar cycle variations of foF2
from IGY to 1990, Ann. Geophys., 20, 1677 – 1685.

Study of magnetic storm effects on the variation of TEC over low, mid and high latitude station
1

Roshni Atulkar1 and P. K. Purohit1
National Institute of Technical Teachers' Training and Research, Bhopal – 462002, MP, India.

The ionosphere is very important because of its influence on the passage of radio waves. Total electron content (TEC) is a key
ionospheric parameter that describes the major impact of the ionosphere on the propagate on of radio waves which are crucial
for terrestrial and space communication. The present investigation is dedicated to study the latitudinal variation of ionosphere.
The study is carried out by taking three stations one each in low, mid and high latitude regions namely IISC, Bangalore, India(13.020 N, 77.570E), GUAO, Urumqi, China (43.820N, 87.600E) and NYAL, NY-Alesund, Norway (78.920N, 11.860E)
respectively. To study the changes in the ionosphere at three selected station we have considered the GPS observations. The
GPS derived TEC values have been collected from the SOPAC (Scripps Orbits and Permanent Array Center) data archive of
the IGS (International GPS service). We studied the behaviour of ionospheric Total Electron Content (TEC) during thegeomagnetic storms. We have selected 5 intense geomagnetic storms (Dst ≤ -100nT) that were observed during the year 2012.
From our analysis we observed that the effect of geomagnetic storms on VTEC is highest at low latitude, moderate at midlatitude and low at high latitude.
Table 1. Catalogue of all the five selected intense geomagnetic storm events along with Peak Dst.

Event Date

Peak Dst(Min.)

9 March 2012

-143nT

24 April 2012

-104nT

15 July 2012

-133nT

1October 2012

-133nT

14 November 2012

-109nTFigure 1:

Figure 2

Figure 3

Figure 4

Figure 5
Figure 1. 2,3,4 and 5. Plot of temporal evolution of ionospheric VTEC along with Dst, IMF Bz and AE during the geomagnetic storm of
9 March, 24 April,15 July,1 October, and 14 November 2012.

References[1] Akasofu S -I.(1981) Relationships between the AE and Dst indices during geomagnetic storms. J. Geophys. Res.86:4820–
4822.[2] Mendillo M, et al. 1970, Ionospheric storms at midlatitudes. Radio Sci.;5:895–898. and,doi: 10.1029/RS005i006p00895.[3] Titheridge J E et al.1988. A comparison of Northern and Southern Hemisphere TEC storm
behaviour. J. Atmos. Terr. Phys.;50:763–780.

Moon-Earth: global basaltic effusions, their different ages, common chemical trends(alkalinity, iron content)
Gennady G. Kochemasov
IGEM of the Russian Academy of Sciences, 35 Staromonetny, 119017 Moscow,kochem.36@mail.ru

Global basaltic covers are very characteristic phenomena in the inner solar system. Basaltic
effusions of different ages and compositions originated in asthenospheric layers of theplanetary mantles. To heat and melt some parts of the mantle, a part of enormous mechanicalenergy of orbiting cosmic bodies was transferred to the heat energy.
“Orbits make structures” – a main point of the new wave planetology based on one
important property of the Keplerian elliptical planetary orbits [2, 3] . The ellipticity implies
periodical changes of accelerations and, thus, orbital forces structuring cosmic bodies. The
Earth and the Moon sharing the same circumsolar orbit have similar main structural features.
Among them there are terrestrial Oceans and lunar Basins. The most obvious are two tectonic
triads: Pacific Ocean – Malay Archipelago – Indian Ocean on Earth and Procellarum Basin –Mare Orientale – SPA Basin on the Moon. The planetary depressions of both bodies arecovered with basalts, but basaltic effusions are drastically different in age: the AR on Moon
and Mz-Cz on Earth. These ages well correlate with the bodies masses. The more massive andinert Earth has heated and melted mantle much later (The Newton’s law of inertia). Energy of
movement transfers to the heat energy.
The both cosmic bodies, as well as the rest of them, are tectonically dichotomous. Theirsubsided hemispheres, for keeping angular momentum of hemispheres equal, are filled with
dense basaltic material. But times of the fillings are significantly different.
The Earth-Moon system expands with time, that is increases its angular momentum. A
natural response to it is in slowing down rotation of both bodies diminishing their angularmomentum (action - opposite action). Diminishing momenta are compensated by melting anduplifting to surfaces dense basaltic material. But on the Moon it happened much earlier(4.5-3 billion years ago) because of diminished inertia of the small mass satellite. At muchlarger and massive with large inertia Earth this process was significantly “delayed” intime.(Mz-Cz). Earth is 81 times more massive than Moon. (3-4.5 billions) : 81 = 37-55
million years. According to this calculation, a “peak” of the basaltic reaction of Earth, fillingin by basalts the oceanic depressions is in the boundary of Mesozoic and Cenozoic [3]].
Despite of enormous age differences between lunar and terrestrial basaltic covers (billionsof years!) some common chemical shift of their compositions is notable and significant. Let
us compare Procellarum Basin and Pacific Ocean basalts. The oldest parts of their covers
occur mainly in the West of Procellarum (KREEP) and SW of the Pacific (Ontong Java
Plateau – the largest LIP of Earth). Potassium, phosphorus, rare earths, thorium enrich theolder lunar KREEP basalts. The older terrestrial oceanic Ontong Java basalts (Cretaceous ageabout 122 mln. y) also show “KREEP trend”. They belong to E-MORBs and have elevatedvalues of potassium, lithium, chlorine, REE, thorium. Elevated Fe/Mg (and siderofile
platinum group elements) also is in Ontong Java basalts [1]. All these chemical peculiarities
distinguish them from the younger N-MORBs of other parts of the Pacific Ocean (EPR, forexample). As all considered basalt melts of both bodies originate in asthenopheres, the older
parts of these melts derive from relatively earlier “cool” asthenosphere. It means that only
easily melted alkali and iron rich parts were involved in the process. Later on, significantly
heated asthenospheres produced enormous volumes of chemically different (less alkaline andmore magnesian) basalts. In this sense, rather impressive is a comparison of the lunar iron andthorium geochemical maps stressing coincidence of their anomalies in the Procellarum
KREEP terrain area (Fig. 1, 2).
The considered time development of basaltic magmatism could be paralleled with thedevelopment of alkaline terrestrial magmatism. Its earlier older parts often are more alkaline
than later Cenozoic parts. Famous large agpaitic massifs are mainly Proterozoic-Paleozoic inage. Again, early “cold” asthenosphere produces more easily melted relatively small alkalineparts than the later “hot” asthenosphere making large volumes of deeply melted moremagnesian less alkaline ones.
References:[1] Ely J.C. and Neal C.R. (2003) Using platinum-group elements to investigate the origin of
the Ontong Java Plateau, SW Pacific // Chemical Geology, v. 196, 235-25[2] Kochemasov G.G. (2016) The Moon and Phobos: specific responses of two satellites
moving off and nearer their respective planets // DPS 48/EPSC 11, Pasadena, Oct. 16-21,
2016, Bulletin of the American Astronomical Society, 2016, vol. 48, # 7, p. 175, Abstract
318.08, Session 318: Formation and Evolution of Planets and Satellites Posters.
[3] Kochemasov G.G. (2017) New planetology and geology: tectonic identity and principal
difference of terrestrial oceans and lunar basins // New Concepts in Global Tectonics (NCGT)
Journal, 2017, V. 5, # 1, p 131-133.

1

2

On the bulk silicate composition of carbonaceous chondrites
P. Futó1, A. Gucsik2
University of Debrecen, Department of Mineralogy and Geology, Debrecen, Egyetem tér 1. H-4032, Hungary(dvision@citromail.hu)
2
Wigner Research Center for Physics, Hungarian Academy of Sciences, Konkoly Thege Miklós 29-33., Budapest, Hungary
1Introduction:
The bulk compositions of the stony meteorites have been dominated by silicates and oxides. The one part of meteoritic
minerals came through different grade of the chemical and/or physical transformations during the formation of the SolarSystem. There are ancient mineral constituents, which survived the early stage of the evolution of the Solar-System and they
appears original form: presolar dust grains. Primitive meteorites contain presolar dust grains: silicates, oxides, nanodiamonds,
silicon carbide graphite, silicon nitride. The dominant sources of dust grains are the AGB stars and supernovae. The presolar
silicate abundance is greater than the abundances of other presolar minerals [1].
Carbonaceous chondrites (CC, c-chondrites) are primitive meteorites with significant silicate and oxide amounts, some of them
contain a relatively larger amount of elemental carbon (diamonds, graphite) and carbon-based compounds (silicon-carbide,
different organic compounds). They are composed mostly of chondrules, inclusions and the fine-grained matrix. C-chondrites
can be classified according to that their parent bodies formed in different regions of the early Solar-system. Accordingly,
different CC-groups may distinguished as CI, CM, CV, CO, CR, CK, and CH type chondrites [2]. The groups are further
divided into different subgroups.
Similarities and significant differences also appears in the abundances of given compounds in the different chondrites
depending on the formation conditions of their parent bodies. For instance, the bulk composition of Allende matrix is Fe-richobtained by Inoue et al. [3], the CM2 Murchison meteorite is an organic rich carbonaceous chondrite [4]. Chemical similarities
appear between CM and CO chondrite chondrules [5], while considerable differences show the Murchison (CM2) and the
Allende (CV3) chondrites in carbon content of the matrix.
In carbonaceous chondrites, highly forsteritic (Mg 2SiO4) olivine can be found for example in the chondrules, in the (Amoebid
Olivine Aggregates (AOA) and in the grains and aggregates embedded in the matrix. Fayalitic olivine (Fe 2SiO4) is also
identified in the mineral structures, but its amount is smaller than that of the forsterite. Enstatite (MgSiO 3) and ferrosillite(FeSiO3) are also known in the mineral textures of chondrites.
Bulk silicate composition of c-chondrites The investigation for characteristics of silicates based on in detail the Kaba primitiveCV3 c-chondrite [6], otherwise we studied the pure matrix material of the Allende CV3 c-chondrite with the concerning datautilized from the results of Inoue N. et al. 2004 [3]. We determined the Mg/Fe ratio in the silicates and the results have beensummarized in the Table 1.
Kaba (CV3)mineralstructure

Mineral sample

FeO(wt%)MgO(wt%)Mg/FePorphyritic Forsteritechondrule

Fo1-1

0.30

55

Mg0.993Fe0.007

Granularol-px
chondrule

Forsterite

Fo3-1

0.89

54.99

Mg0.98 Fe0.02

Forsterite

Fo3-2

1.02

54.70

Mg0.976Fe0.024

Isolatedolivinegrain

Forsterite

Fo8-2

0.21

56.91

Mg0.995Fe0.005

Comlicated Fayalite
aggregate

Fa9-2

68.05

0.26

Mg0.003Fe0.997

36.60

19.19

Mg0.407Fe0.593

Allende(CV3)Pure matrix

A1

Table 1. The FeO and the MgO abundances in different mineral structures of the Kaba meteorite (CV3) and in the bulk chemical compositionof the matrix of the Allende (CV3) chondrite. The Mg/Fe ratio is calculated from the basic data that are taken from Gucsik A. et al. (2013)
and from Inoue M. et al. (2004).

As seen in the Table 1, the mineral components of the Kaba meteorite is rich in highly forsteritic (Fo>0.99) olivines, while thebulk silicate composition of the Allende matrix enriched in iron. In fact, the mineral composition of chondritic meteorites has
been dominated by silicates. The elemental abundances of chondrites approximately consistent with the cosmic abundances of
elements and minerals. The high ratio of Mg, Si, and O in meteorites refers to the dominance of magnesium silicates for thecase of chemical characteristics of the Galaxy as opposed to the abundances of Fe-, Ca-, Al-silicates.
Summary: The carbonaceous chondrites are known to have been dominated by silicates but they may contain carbonaceous
mineral constituents in small amounts. The bulk composition of the planet-building materials in the most circumstellar
enviroments is assumed to be chondritic-like.

References[1] Nguyen A. N. et al., Characterization of presolar silicate and oxide grains in primitive carbonaceous chondrites, The
Astrophysical Journal 656, 1223-124, 2007. [2] Kallemeyn G.W. and J.T. Wasson, The compositional classification ofchondrites—I. The carbonaceous chondrite groups, Geochimica et Cosmochimica Acta , 45(7), 1217-1230, 1981. [3] Inoue N.
et al. EE abundances in the matrix of the Allende (CV) meteorite: Implications for matrix origin, Meteoritics & Planetary
Science 39,599-608, 2004. [4] Kebukawa Y. et al., Kinetics of organic matter degradation in the Murchison meteorite for theevaluation of parent-body temperature history, Meteoritics & Planetary Science 45, 99-113, 2010. [5] Schrader D. L. and J.
Davidson, CM and CO chondrites: A common parent body or asteroidal neighbors? Insights from chondrule silicates,
Geochimica et Cosmochimica Acta , 214, 157-171, 2017. [6] Gucsik A. et al., Cathodoluminescence microscopy andspectroscopy of forsterite from Kaba meteorite: An application to the study of hydrothermal alteration of parent body,
Meteoritics & Planetary Science 48, 2577-2596, 2013.

NASA Curation Preparation for Ryugu Sample Returned by JAXA’s Hayabusa2 Mission
Keiko Nakamura-Messenger1, Kevin Righter1, Christopher J. Snead2, Francis M. McCubbin1, Lisa F. Pace1, Ryan A. Zeigler1,& Cindy Evans1
1
NASA Johnson Space Center, Houston, TX USA, 2JETS at NASA Johnson Space Center, Houston, TX, USA
The NASA OSIRIS-REx and JAXA Hayabusa2 missions to near-Earth asteroids Bennu and Ryugu share similar
mission goals of understanding the origins of primitive, organic-rich asteroids. Under an agreement between JAXA and NASA,
there is an on-going and productive collaboration between science teams of Hayabusa2 [1] and OSIRIS-REx missions [2].
Under this agreement, a portion of each of the returned sample masses will be exchanged between the agencies and thescientific results of their study will be shared. NASA’s portion of the returned Hayabusa2 sample, consisting of 10% of the
returned mass, will be jointly separated by NASA and JAXA. The sample will be legally and physically transferred to NASA’s
dedicated Hayabusa2 curation facility at Johnson Space Center (JSC) no later than one year after the return of the Hayabusa2
sample to Earth (December 2020). The JSC Hayabusa2 curation cleanroom facility design has now been completed. In thesame manner, JAXA will receive 0.5% of the total returned OSIRIS-REx sample (minimum required sample to return 60 g,
maximum sample return capacity of 2 kg) from the rest of the specimen [2]. No later than one year after the return of the
OSIRIS-REx sample to Earth (September 2023), legal, physical, and permanent custody of this sample subset will betransferred to JAXA, and the sample subset will be brought to JAXA’s Extraterrestrial Sample Curation Center (ESCuC) at
Institute of Space and Astronautical Science, Sagamihara City Japan.
Both the Hayabusa2 sample to be sent to NASA and the OSIRIS-REx sample to be sent to JAXA will be unprocessed
and representative of the returned bulk sample. “Unprocessed” means that the sample will be handled in a way that minimizes
chemical and physical changes to the sample, including avoidance of harsh radiation and heating environments such as
electron beams and Raman microscopy. The exchange samples will also be protected from organic and other forms ofcontamination to the greatest extent possible. “Representative” means that the separated sample has, as well as can be
determined on the unprocessed sample, very similar characteristics to the bulk returned sample, including grain size, color, andother physical properties readily determined by optical observation.
The overarching objectives of NASA’s Hayabusa2 curation are to preserve and protect the returned Ryugu subset
samples to maximize the science return. Curation scientists at JSC together with ESCuC members and the OSIRIS-REx
science team have been working to identify requirements on contamination and sample environmental controls. The
Hayabusa2 curation requirements can be categorized into the following nine major responsibilities: 1) Contamination control,
2) Curation procedures for solid and gas samples from Ryugu surfaces, 3) Clean laboratory design and construction, 4).
Sample characterization for catalog (non-destructive organic-nonorganic lithology identification in a glovebox), 5) Sample
distribution, and 6) long term curation activity. Many of the aspects of NASA Hayabusa2 curation for the Ryugu samples are
already well developed and have strong heritage at JSC. Examples of existing knowledge and application in this area include
ppb level organic residue monitoring of the gaseous curation grade nitrogen, precision cleaning of ultrapure water circulatingin the clean labs, particle count monitoring, and metal material control for terrestrial trace element contamination control(Apollo, Genesis samples), and sample handling of small particles (cosmic dust, Stardust cometary particles, Hayabusa1
asteroid samples), to mm-cm sized rocks (Antarctic meteorites). The Hayabusa2 sample storage and handling facility at JSC
have been co-designed with the OSIRIS-REx sample curation clean facility to protect the samples from contamination, crosscontamination, temperature excursions, and moisture that could alter the sample. The construction of the facility will start in2018 [3].
As with every new extraterrestrial collection, returned primitive Ryugu samples bring special new requirements forpotentially organic rich samples. Hayabusa2 mission will attempt to collect three samples from the surface of the asteroid inorder to return a minimum of 100 mg of material. Prior to its third touchdown, Hayabusa2 will release an impactor to theasteroid that will create a small crater, possibly exposing more pristine materials from beneath the surface from which sample
collection may be attempted. Each of the three samples may have different characteristics and they should be properly handled
to preserve them. Hayabusa2 Science Team will attempt to extract the gas sample before opening the pneumatically sealed
sample container. JSC will develop the gas sample curation and handling technique under our advanced curation activity [4].
References: [1] Watanabe S. et al. (2017) Space Science Reviews, 208, 3-16. [2] Lauretta D.S. et al. (2017) Space Science
Reviews, in press. [3] Righter et al. (2017) this volume. [4] McCubbin F.M et al. (2017) this volume.

Current status of developments by the collaboration team with ESCuC/JAXA for curation works
and analysis of Hayabusa2 returned samples
M. Uesugi1, M. Ito2, N. Tomioka2, K. Uesugi1, A. Yamaguchi3, N. Imae3, T. Ohigashi4, Y. Karouji5, T. Yada6, and M. Abe6,
Japan Synchrotron Radiation Research Institute (JASRI/SPring-8) (uesugi@spring8.or.jp), 2Japan Agency for Marine-Earth
Science and Technology (JAMSTEC), 3National Institute of Polar Research (NIPR), 4Institute for Molecular Science (IMS),
5
Tokyo Metropolitan University, 6Japan Aerospace Exploration Agency (JAXA).

1Extraterrestrial sample curation center (ESCuC) of Japan aerospace exploration agency (JAXA) organized a special team forthe development of techniques and devices for the handling, transfer and analysis of samples returned by Hayabusa2 spacecraft,from 2015 under the agreements of collaboration. The special team constitutes of members of institutes those having state-ofthe-art analytical instruments and experiences of curatorial works of precious natural samples, but beyond the specialists of theextraterrestrial materials. Through the collaboration, we can introduce latest specialties and knowledges from diverse scientificand technological fields into the processes of analysis of Hayabusa2 returned samples [1,2].
So far, we finished the development sample transfer container for the inter-institute transfer, even international transfer ofsamples, without contamination of terrestrial materials and sample damages such as breaking and sample lost. We also
evaluated the sealing performance of the container and confirmed that it has enough sealing performance against even positive
pressure inside the container. The container, named as Facility to Facility Transfer Container (FFTC), is already available
commercially.
Currently, the team members are working for (1) development of sample holders for the sample transfer in high cleanness
environment, (2) development of devices for the atmosphere shielding environment for the sample handling, (3) developmentof sample holders applicable for multiple analytical methods, and (4) development of techniques for the evaluation ofcleanness of those developed materials and environments. Although those devices and techniques are still under development,
we already applied them for the analysis of samples in each institute, and evaluated its applicability and problem for the
analysis of Hayabusa2 returned samples.
We also started development of new analytical protocols of extraterrestrial materials, which includes method of sample
transfer, sample separation and data sharing, through the rehearsals of the curation works for the initial description of
Hayabusa2-returned samples using extraterrestrial materials. Currently, 5 Antarctic micrometeorites provided by national
institute of polar research (NIPR) were imaged by synchrotron radiation computed tomography (SR-CT) and x-ray diffraction(XRD) at SPring-8, and investigated by high resolution field emission scanning electron microscopy and energy dispersive
spectroscopy (FE-SEM-EDS) system at institute for molecular sciences (IMS). Through the series of non-destructive analysis,
we selected Antarctic micrometeorites those having similar characteristics of carbonaceous chondrites, and formed thinsections by focused ion beam (FIB) for the characterization of organic materials by scanning transmitted x-ray microscopy andnear edge x-ray absorption fine structure analysis (STXM-NEXAFS) at IMS, high resolution analysis by transmission electron
microscopy (TEM), and isotopic analysis of light elements such as hydrogen, carbon, nitrogen and oxygen by secondary ion
mass spectrometry (SIMS) at Japan agency for marine-earth science and technology (JAMSTEC).
In order to make possible such large scale collaboration for the series of sample analysis between institutes, we need toevaluate sample damages and contaminations through the analysis, and develop the methods for cleaning of sample holder andprotocols for suppressing sample damages, as well as sample transfer system. Sample holders are already under theexamination. So we can start the evaluation of cleanness and development of method for the cleaning of them by ultrasoniccleaning and acid-alkali cleaning [3,4]. We will start the development in this year, and will report the result near future.
Thus progress of our development is going along quite smoothly. We can share the result of our development withpreliminary examination team of Hayabusa2 sample analysis organized by Hayabusa2 project, and can make their start process
faster.
In future work, we will develop the cutting method of samples with low-contamination processes, including sample
mounting devices and handling method after the cutting. In order to include rare and trace element analysis using laser ablationinductively coupled plasma mass spectrometry (LA-ICP-MS) in our protocol, we will also start the development of sample
holders and examination of it, in parallel with the rehearsals of the initial description of Hayabusa2 returned samples.
References[1] Web page: https://hayabusaao.isas.jaxa.jp/curation/release/index.html (Japanese) [2] Uesugi M. et al. 2016. Abstract#1129-1100. Haybusa symp. 2016. [3] Karouji et al., 2014. Chikyu kagaku 48:211-220 (Japanese) [4] Ishibashi Y., Karouji Y.,
Fujimura A., Yada T., Uesugi M., Yakame S., Okada T., and Abe M. 2012. Asteroids, Comets, Meteors, abstract #6492

Systematic detection of carbonaceous phases in chondrites –request for sophisticated techniques for Hayabusa 2 particle analyses
V.H. Hoffmann1,2, T. Mikouchi3, M. Kaliwoda4, R. Hochleitner4Fac. Geosciences, Dep. Geo- and Environmental Sciences, Univ. Munich, 2Dep. Geosciences, Univ. Tübingen, Germany;3
Dep. Earth Planet. Science, Univ. Tokyo, Japan; 4Mineralogical State Collection, Munich, Germany.

1

The Asteroid Explorer “Hayabusa 2” is the successor of “Hayabusa” (MUSES-C), which for the first time ever returned
pristine samples from an asteroid [1]. 25143 “Itokawa” is a small Near-Earth S-type asteroid consisting mainly of ordinarychondrite type material [2, and refs herein]. The mission was a major step towards further elucidating the origin and formationof our solar system. The “Hayabusa 2” mission, launched in 2014, will target another Near-Earth asteroid, namely 162173“Ryugu” (1999 JU3) which is a C-type asteroid. To learn more about the formation and evolution of our solar system,
investigating different types of asteroids, namely S-, C-, and D-type, is mandatory. C-type asteroids such as “Ryugu” areinterpreted as more primordial bodies than for example “Itokawa” and are considered to contain more carbonaceous, organic or
hydrated mineral phases. Spectroscopical data show that this asteroid type might be closely related to primitive carbonaceouschondrites or comets in terms of material composition [3].
Very sophisticated techniques are required for the investigation of pristine “Ryugu” particles in our laboratories (return planedend of 2020). LASER Micro Raman Spectroscopy is perfectly suited for identifying and discriminating (extra-) terrestrial
mineralogy: (a) fully non-destructive (repeated experiments possible on one and the same spot under variable conditions), (b)investigations with high sensitivity and in parallel high resolution, optionally in 3 dimensions, (c) as a major advantage
experiments on pristine material without any preparation or coating, and (d) mineral polytypes (eg diamonds) can be welldiscriminated. Variable LASER frequencies allow to optimize and fine-tune the Raman system to specific sample andexperiment requirements. High resolution scanning can produce very detailed distribution maps of selected mineral phases.
Micron- or even nano-sized particles such as various diamond polytypes can be detected in this way. Within our Hayabusa
sample analyses project we have successfully applied LASER Micro Raman Spectroscopy on several individual Itokawa
particles [2].
Generally, the carbon-phase mineralogy has not really been investigated systematically in most meteorite types [4,5]. The main
focus was on ureilites and certain carbonaceous chondrites [4-7], and priority was set on graphitic components and diamonds.
The presence of very rare carbonaceous phases such as graphenes, fullerenes or nanotubes which can be exspected in a numberof meteorite types has not been investigated to our best knowledge. Therefore we have started detailed and systematicinvestigations on the carbon-phase mineralogy of a larger set of various stony meteorite types. Priority is presently set on thefollowing selected recent falls and finds [8-13]: (a) Ordinary chondrites Machtenstein H5 (find around 1956, classified 2014),
Braunschweig L6 (fall 2013), Stubenberg LL6 (fall 2016), and for comparison the HED meteorite Saricicek (howardite fall2015) as well as a large series of Almahata Sitta individuals [polymict ureilite, 12,13 and refs]. In our poster we will present
first detailed results concerning the carbon phase mineralogy in these meteorites and will also focus on hypotheses concerning
the possible formation processes of the meteoritic micro-nano diamonds [6,7,14,15]: (a) Chemical Vapor Deposition (CVD)and (b) shock metamorphism as optional in situ diamond producing processes, and (c) presolar diamonds of extrasolar origin(eg from supernovae explosions).
References[1] http://global.jaxa.jp/projects/sat/hayabusa2/: last visit 9/2017.
[2] Mikouchi T. et al., 2014. Earth, Planets, Space, 66, pp82.
[3] Norton R.O., 2002. The Cambridge Encyclopedia of Meteorites. Cambridge Univ. Press.
[4] Ramdohr P., 1973. The opaque phases in stony meteorites. Elsevier, New York.
[5] Makjanic et al., 1993. Meteor. 28, 63-70.
[6] Szurgot M. et al., 2006. Nanodiam, PWN, Warszawa, pp259.
[7] Karczemska A.T., 2010. J. Achievm. Mater. Man. Engineer. 43/1, 94-107.
[8] https://www.lpi.usra.edu/meteor/metbull.php: last visit 9/2017.
[9] Hochleitner R. et al., 2015. LPSC #2453.
[10] Hochleitner R. et al., 2015. LPSC #1471.
[11] Bischoff A. et al., 2017. Meteor. Planet. Sci. 1-21, doi: 10.1111/maps.12883.
[12] Hoffmann et al., 2017. LPSC #2365.
[13] Hoffmann et al., 2017. Metsoc #6290.
[14] Gucsik et al., 2008. LPSC #1201.
[15] Hus G.R., 2005. Elements 1, pp97-100.

Preliminary results of Sulfur speciation by µ-XANES and STXM in Extraterrestrial Organics
Motoo Ito1, Ryoichi Nakada1, Hiroki Suga2, Takuji Ohigashi3, Yu Kodama4 and Hiroshi Naraoka5
1
Kochi Institute for Core Sample Research, JAMSTEC, 2Hiroshima University
3
UVSOR Synchrotron, Inst. Mol. Sci., 4Marine Works Japan, 5Kyushu University
Sulfur is one of the major elements in terrestiral and extraterrestrial organics. The elemental compositions of theMurchison IOM (insolble organic matter) are proposed to be C100H70O22N3S7 [1] or C100H48N1.8O12S2 [2]. Because sulfur
shows a wide range in oxidation state (-2 to +6) with both electropositive and electronegative elements, both reduced andoxidized sulfur species have been found in various carbonaceous chondrites [3, 4]. Therefore, understanding of speciation of
sulfur and its distribution within organics in a carbonaceous chondrite is crucial to provide the secondary alteration processesof thermal metamorphism and aqueous alteration in the parent body.
X-ray absorption near edge spectroscopy (XANES) is a powerful analytical tool to characterize and quantify chemical
speciation, functional group and bonding environment of the sample. In the field of cosmochemistry, many researches werecarried out to identify functional groups of C, N and O in extraterrestrial organics (i.e., IOM in carbonaceous chondrites [5],cometary returned sample [6], organics found in Hayabusa Category-3 grains [7], organics in IDPs [8]). However, sulfur
study with XANES in the extraterrestrial organics is very rare [3, 9].
In this study, we report preliminary results of sulfur speciation measurements by K- and L3-edge XANES of the IOM
extracted from Asuka 881458 CM2 carbonaceous chondrite. We carried out X-ray fluorescence (XRF) mapping for S and Nwith a spatial resolution of 20 µm in the IOM (0.8 x 1 mm2) at BL27SU of SPring-8. We, then, conducted µ-XAFS (sulfur
K-edge) measurements to acquire point spectra (#1-#6 in Fig. 1). In addition, we have measured carbon K-edge and sulfur
L3-edge XANES spectra in the FIB section of the AA881459 IOM (8 x 20 µm2) using scanning transmission X-ray microscope(STXM) at Inst. Mole Sci. UVSOR
42 8   45 2
18 .
82 4. 18 5 Figure 2. Possible sulfur components in the extractedorganics from A881458 obtained by K?edge spectrum.
  
.
84
BL4U.
Spot1#• 0.8"x"1"mm
Low
High
Spot2#
Figure 1 shows S and N• 37"x"51"pixels"(20"µm/pixel)
Spot3#
Spot4#
S&XRF"image
N&XRF"image
S
Spot5#XRF images together with optical
Optical"microscope"Image
Spot6##6#6
microscope image of the sample on#1#1
the Si wafer. The distributions of#5#5
S and N are similar but slightly#2 #3 #4
#2 #3 #4
different abundances. We used
these images to determine XANES
1"mm
analysis spots in the sample (about
20 µm in size, #1 to #6 in Figure 1).
Measured S K-edge XANES spectra (#1 to #6) have deconvoluted with a least- Figure'3.'Sulfur'L.edge'STXM'image'and'SIM'image'square linear combination best fits to reference spectra of S contained organic and Low&High&
FIB section image
inorganic compounds. Figure 2 shows a radar diagram of possible S components
and their abundances in each spot (#1-#6). Each spot has different sulfur containedorganics and inorganics and their abundances. This suggested that extraterrestrialorganics is a complex mixture of several types of sulfur species. Our result is
consistent with previous works [3, 9]. S L3-edge XANES spectra of several Scontained organics with different species (lauryl sulfate, sodium methanesulfonate,
9 µm
L-cysteic acid and DL-methionine sulfone) were obtained as references. Figure 3 S"STXM&
image&
shows high-resolution (50 nm) S L3-edge STXM image of the FIB section of theAA881459 IOM. It is noted that S is homogeneously distribute and tiny S hot spots were observed within the sample.
However, it is difficult to deconvolute the L3-edge spectra of the sample based on fitting by a linear combination of standard
materials spectra because of lack of the S L3-edge spectra for reference materials at this moment.
2

4!aminothiophenol#
Trimethylsulfonium# 15#
4!nitrobenzen#
Thianthrene#
Anthraquinone#

Sulfoxide#

Sulfonate#

13#
11#

Aroma9c!SH1#

CysAlaAla#9#

pyrrho9te#

Cys9ne#7#5#pyrite#Dibenzothiophene#

3#

Polyphenylenesulﬁde#Dibenzyl#disulﬁde#

1#

!1#

PhCH2SPh#

Dibenzyl#sulﬁde#Octoclothepin#

Dihydrodibenzothiopin#

Na9ve!S#Na2SO4#

Na2SO3#DL!Methionine#
Methylsulfonium#
Methionine#
Methanesulfonic#acid#

DL!methionine#sulfone#

Dothiepin#

gypsum#

HOPhSPhOH#
Lauryl#sulfate#
L!cysteic#acid#

References: [1] Remusat, 2011. EPJ Web of Conferences 18:05002. [2] Gilmour, 2005. In Meteorites, comets and planets,
Treatise on Geochemistry, p.269. [3] Orthous-Daunay et al. 2010. EPSL, 300, 321−328. [4] Cooper et al. 1997. Science, 277,
1072−1074. [5] Cody et al. 2011. Meteor Planet Sci 43:353–365. [6] Sanford et al. 2006. Science, 314:1720–1724. [7] Yabuta
et al. 2014. EPS, 66, 156. [8] Flynn et al. 2003. Geochim Cosmochim Acta, 67, 4791–4806. [9] Bose et al. (2017) Meteor
Planet Sci, 52, 546−559.

The evolution of water-rich asteroids: Linking the mineralogy and spectroscopy of fully hydrated
CM carbonaceous chondrites
Helena Bates1,2, Ashley King1, Kerri Donaldson Hanna2, Neil Bowles2 and Sara Russell1
1
Mineral and Planetary Sciences Division, Natural History Museum, London, SW7 5BD, UK
2
Atmospheric, Oceanic and Planetary Physics, University of Oxford, Oxford, OX1 3PU, UK
Introduction: The C-complex asteroids (which include B, C, F and G-types [1]) are of interest because they arethought to be volatile-rich, and may be able to tell us about the evolution of water and organic compounds in the early Solar
System. Additionally, C-complex asteroids likely made a significant contribution to the volatile budget of the terrestrial planets[2,3]. Carbonaceous chondrite meteorites are physical samples of C-complex asteroids; linking laboratory spectra ofcarbonaceous chondrites to remote sensing observations of asteroids can therefore give insight into the processes, which occur
on primitive bodies in the Solar System.
Spectrally, many C-complex asteroids show evidence for aqueous alteration and links with CM and CI carbonaceouschondrites on their surfaces [4–7]. Most spectral links have been between the C-complex asteroids and moderately altered
CM2 chondrites. Although there have been limited studies on the association of these asteroids with fully hydrated (“type 1”)chondrites, Clark et al. [8] suggested a possible relationship between more aqueously altered CM and/or CI chondrites and thesurface mineralogy of the B-type, OSIRIS-REx target asteroid, Bennu.
The CM1 chondrites are among the most hydrated extra-terrestrial materials available to study; their precursor
mineral assemblages have been almost entirely transformed into secondary, hydrated phases. King et al. [9] investigated
CM1 and CM1/2 chondrites with the aim of establishing modal mineralogy and examining variations in the extent of aqueousalteration. In this study we collected reflectance spectra from the same powders used by King et al. [9] so that any spectral
trends could be put into context of the mineralogy and degree of aqueous alteration for each meteorite sample.
Experimental: The suite of meteorites investigated included six CM1/2 chondrites and four CM1 chondrites.
Approximately 100 mg of each sample was ground into a fine powder using an agate mortar and pestle to a particle size of <35µm. Infrared reflectance spectra of the powders were obtained using a Bruker VERTEX 70v Fourier Transform Infrared(FTIR) spectrometer at the University of Oxford, using a wide range MIR-FIR beam splitter and a room temperature
deuterated L-alanine doped tryglycine sulfate (RT-DLaTGS) detector to measure the reflectance between 6000 - 200 cm-1 (1.750 µm). All observations were obtained under vacuum (~5 hPa), at a resolution of 4 cm-1. In order to remove instrumental
effects, spectra were calibrated by dividing each meteorite spectrum with a spectrum of a gold calibration target,
Results & Discussion: Initial observations of the mid-infrared spectra show samples, which are mostly composed ofhydrated minerals, particularly serpentine-group phyllosilicates. Upon further investigation of individual spectral regions - the
3 µm band, 6 µm band, Christiansen features (CF: 7.5-9.5 µm), and the transparency features (TF: 10.5-14 µm) - different
phyllosilicate compositions and abundances resulted in different, distinguishable spectral features.
The 3 µm band centres are affected by the Fe-cronstedtite abundances in the samples, with higher abundances shifting
the feature to longer wavelengths. The 6 µm band features appear to reflect the anhydrous silicate content, with greater band
depths for higher olivine contents. The CFs are identified at similar wavelength positions for all samples (8.8 - 8.9 µm)
suggesting the meteorites have similar bulk mineralogy. The TFs were affected by the total phyllosilicate abundance, withhigher abundances shifting the peaks to shorter wavelengths.
The above conclusions resulted in splitting the meteorites into two groups. Group A samples had larger 6 µm bandfeatures, a 3 µm band centre, and TF peak at longer wavelengths (~2.8 µm and ~12.5 µm respectively). Group B samples had
smaller 6 µm band features, a 3 µm band centre, and TF peak at shorter wavelengths (~2.7 µm and ~11.6 µm respectively).
Group A samples represent the least altered CM1/2s, which have significant Fe-cronstedtite abundances of 30.8 –
36.9% and anhydrous olivine abundances of 18.2 – 19.6%. Group B samples represent the most altered CM1s, which havesignificant Mg-serpentine (52.4 – 71.6%) and low olivine abundances (3.6 – 8.0%). This study shows that slight variations inaqueous alteration might be discernible in current and future telescopic and space mission observations of C-complex asteroids.
References: [1] Tholen, D.J., 1984. [2] Alexander, D. et al., 2012 Science, 721. [3] Alexander, C.M.O., 2017
Philosophical Transactions of the Royal Society, 375. [4] Fornasier, S. et al., 1999 Astron. Astrophys. Suppl. Ser, 135:65. [5]Ziffer, J. et al., 2011 Icarus, 213: 538. [6] Cloutis, E.A. et al., 2011 Icarus, 216:309. [7] Takir, D. et al., 2015 Icarus, 257:185.
[8] Clark, B.E. et al., 2011 Icarus, 216:, 462. [9] King, A.J., P.F. Schofield, S.S. Russell, 2017 Meteoritics & Planetary
Science, 52:1197.

Current status of consortium study of silica-containing Hayabusa-returned particle.
M. Hashiguchi1, A. Miyake2, A. Tsuchiyama2, T. Nakamura3, M. Uesugi4, J. Matsuno2, A. Nakato2, T. Yada5, M.
Yoshitake5, T. Okada5, M. Abe5, and H. Yurimoto5, 6.
1
PTOC, Kyushu University (hashiguchi.minako.123@m.kyushu-u.ac.jp), 2Department of Geology and Mineralogy, Graduate School of Science, Kyoto University, 3Department of Earth Science, Tohoku University, 4 JASRI,
SPring-8, 5 ASRG, JAXA, 6 Natural History Sciences, Hokkaido University.
Introduction: About 730 particles of Hayabusa-returned sample of 10 to 300 µm size are collected by Extraterrestrial Sample Curation Center (ESCuC) in Astromaterials Science Research Group (ASRG) of JAXA, so far[1]. The preliminary examinations and international AOs revealed that Itokawa particles were equivalent toequilibrated LL chondrites [e.g. 2-10]. Some of the Hayabusa-returned particles show unique characteristics including mineralogy, composition, structure, and/or size. Therefore, consortium studies have been conducted byteam of ESCuC in order to obtain maximum scientific results from such particles [11-13].
We proposed a new consortium study of particle RB-QD04-0069 containing silica [14]. This is the only particle which contains silica coexist with other silicate minerals among catalogued Hayabusa-returned samples, sofar. Silica is widespread in ordinary chondrites, but its abundance is very low (usually < ~1 vol %) [15]. Therefore, the particle RB-QD04-0069 is precious and it should be investigated as consortium study. Evidence ofshock processes have been revealed from Hayabusa-returned particles by previous studies and shock and/or
thermal history of the particles were discussed [2, 8-10]. Because silica has many polymorph, it should be usefulindicator to constrain thermal and/or shock history of the particle [16]. In this paper, we report current status of
the consortium study of particle RB-QD04-0069.
Sample and Analytical flows: RB-QD04-0069 is a particle with a size of 33 µm, which was captured from thefirst touchdown site on Itokawa. The particle consists of olivine, high-Ca pyroxene, low-Ca pyroxene, plagioclase, and silica revealed by initial description by FE-SEM-EDS.
The XRD analysis will provide us crystallographic information of silica and other silicate minerals. Moreover, textural information of the particle will be obtained by the SR XCT imaging. After the synchrotron radiation
analyses, the particle will be embedded in epoxy resin EPON-812, followed by polishing until the surface of theparticle is exposed. Then, oxygen isotope compositions will be measured by SIMS in order to identify the originof the particle. Furthermore, FE-EMPA analysis and TEM observations will be carried out on the particle to obtain important constraints on formation condition of the particle, especially its shock and thermal history.
Current status: The particle RB-QD04-0069 was picked up from a slide glass in pure nitrogen-filled environment clean chamber in ESCuC by quartz glass probe using manipulator system last year. Then, the particle wastried to attach to the top of C fiber with epoxy resin Embed-812 using manipulator system in a clean booth at
ESCuC for Synchrotron radiation (SR) XRD analysis and SR XCT imaging. However, during the procedure, theparticle RB-QD04-0069 was failed to attach to C fiber and fell down on the slide glass or Al foil on heater used
for the handling.
By optical microscope and SEM-EDS analysis, three candidate particles were found from Al foil on theheater. We plan to analyze these candidate particles by detailed FESEM-EDS to narrow down the candidates.
Then, the surrounding region (Al foil) of the candidates will be cut by FIB at Kyoto University and attach themto C fiber using Pt depo for SR-XRD and XCT analysis to identify true particle using characteristics of silica,
olivine, pyroxene, and plagioclase.
References: [1] Yada T. et al. (2017) 80th MetSoc, #6204. [2] Nakamura T. et al. (2011) Science 333, 1113.
[3] Yurimoto H. et al. (2011) Science 333, 1116. [4] Ebihara M. et al. (2011) Science 333, 1119. [5] Noguchi T.
et al. (2011) Science 333, 1121. [6] Tsuchiyama A. et al. (2011) Science 333, 1125. [7] Nagao K. et al. (2011)
Science 333, 1128. [8] Zolensky M. et al. (2012) LPS XLIII #1477. [9] Mikouchi T. et al. (2014), EPS, 66, 82[10] Harries D. et al. (2016) EPSL, 337. [11] Yada T. et al. (2014) LPS XLIV #1759. [12] Uesugi M. et al.
(2014) 77th Ann. Meeting Meteorit. Soc., #5226. [13] Karouji Y. et al. (2014) 77th Ann. Meeting Meteorit. Soc.,#5240. [14] Hashiguchi M. et al. (2015) 78th MetSoc, #5193. [15] Hezel D. et al. (2006) GCA, 70, 1548. [16]Swamy V. et al., (1994) J. Geophys. Research. 99, 787.