COMBINING NON–DESTRUCTIVE MAGNETIC AND RAMAN SPECTROSCOPICAL ANALYSES FOR MARS SAMPLE RETURN –

POWERFUL TOOLS IN SITU AND IN LABORATORY.

References

Viktor H. Hoffmann1,2, M. Kaliwoda3, R. Hochleitner3, T. Mikouchi4, K. Wimmer51Faculty of Geosciences, Dep. Geo- and Environmental Sciences, Univ. Munich; 2Dep. Geociences, Univ. Tübingen/

Germany; 3Mineralogical State Collection Munich/Germany; 4Dep. Earth and Planetary Science, The Univ. of Tokyo/Japan; 5Ries Crater Museum, Nördlingen/Germany; Contact: vh.hoffmann@web.de

[1] Hoffmann V.H., et al., 2013. NIPR Antarctic Meteorite Conference, abstract. [2] Hoffmann V.H., et al., 2016. LPSC, #2482. [3] Mikouchi T. et al., 2014. Earth, Planets, Space, 66, pp82. [4] Hoffmann et al., 2017. LPSC #2365. 5] Hoffmann et al., 2017. Metsoc #6290. And references herein.

(2) Magnetic Signature of Martian Rocks – influence and role of (impact) shock

Planet Mars – State of the Art and Open Questions

Interior Sample3.71 (int)NAKMIL 03346Table 2: Magnetic data on Martian

meteorites – new samples.*Data from MetBull/Internet/Oral.

B-S: Basaltic ShergottiteP/L-S: Poikilitic Shergottite

OP-S: Olivine-Phyric ShergottiteMG-S: Microgabbroic Shergottite

Nak: NakhliteB-RB: Basaltic Regolith Breccia

3.83 (int)NAKMIL 090030

3.78 (int)NAKMIL 090032

3.84 (int)NAKMIL 090136

3.39B-SJaH 479

- 0.96~ 0.066.182.67P/L-SNWA 4797

3.06MG-SNWA 6963

2.86OP-SNWA 6162

- 0.96~ 0.8642.62.93OP-SNWA 5789

3.22B-SNWA 5990

3.16P/L SNWA 7397

4.23*B-SNWA 8159

3.14*P/L GRV 020090

3.81 (int)NAKNWA 5970

3.99NAKNWA 6148

3.93*NAKCaleta el Cobre

4.43B-RBNWA 8171

4.44*B-RBNWA 7034

4.48*B-RBRabt Sbayta 003

3.17MG-SNWA 7320

- 0.98~ 0.12.602.75P/L-SNWA 6342

- 0.88~ 0.1910.23.25MG-SNWA 7032

IRMs[10-3 Am2/kg]

REM S ValueLog MS

[10-9 m3/kg]TypeSample

Returned Samples from Planet Mars: (1) Role of Carbon PhasesVery sophisticated techniques are required for the investigation of pristine, particles on a planets surface or returned samples in our laboratories. Theobtained results – on site (Mars surface) and in laboratory are onlycomparable under condition that in both cases exactly the same analysestechniques are used, therefore developed in parallel:

LASER Micro Raman Spectroscopy is perfectly suited for systematically investigating (extra-) terrestrial materials under in situ conditions:

(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 (3D),

(c) as a major advantage experiments on pristine material without any preparation or coating,

(d) discrimination of mineral polytypes (eg various diamond or SiO2phases) which is otherwise highly complex or impossible,

(e) variable LASER frequencies / energy settings allow to optimize and fine-tune the Raman system to specific sample and experiment requirements,

(f) and in 3D mode detection of subsurface structures/phases or inclusions (solid/ liquid/gaseous components).

High resolution scanning can produce very detailed distribution maps of selected mineral phases. Micron- or even nano-sized particles can bedetected in this way. We have successfully applied LASER Micro RamanSpectroscopy on several individual Itokawa returned particles.

…… and todayand today

> 4 Gyrs ago (??) …> 4 Gyrs ago (??) …

Magnetic Field of Planet Mars

Mars …Mars …

?AccretionAccretion

DifferentiationDifferentiation

Magnetic dynamo FieldMagnetic dynamo FieldPlate tectonicsPlate tectonics

Dense and stable AtmosphereDense and stable Atmosphere

Surface liquid WaterSurface liquid Water

Prebiotic Structures, LifePrebiotic Structures, Life

YY

YY

Y (early)??Y (early)???? (early)?? (early)

?? (early?)?? (early?)

Episodic?Episodic?

????

EarthEarth MarsMarsPlanetaryPlanetaryHistoryHistory

Planetary magnetic fields Planetary magnetic fields -- important factors?important factors?

Origin of strong Martian crustal magnetic Origin of strong Martian crustal magnetic anomalies largely unknown!anomalies largely unknown!

Dynamo field (if so) strength, geometry, and durationDynamo field (if so) strength, geometry, and duration

Thickness of magnetic crust: Curie Thickness of magnetic crust: Curie -- depthdepth

Subsequent history such as impacts and tectonics Subsequent history such as impacts and tectonics

Material properties of magnetic crust (mineralogy / physics)Material properties of magnetic crust (mineralogy / physics)

Physics of prim./sec. magnetizing and Physics of prim./sec. magnetizing and recording processesrecording processes

Space conditions (minor atmosphere, low Space conditions (minor atmosphere, low –– temperature)temperature)

The presence of carbonaceous phases such as ACM (amor-phous carbonaceous matter), graphite or even diamonds has not been investigated systematically in Martian meteorites to our best knowledge. Therefore we have started detailed and systematic investigations on the carbon-phase mineralogy on a large set of meteorites from Mars.

Background of our studies in terms of Carbon phases is thesearch for traces of prebiotic structures, of extinct and extantlife on Mars which was started wiithin the ESA Extended-Mirasproject.

Another approach is focused on the mineralogical and magneticsignature of natural glasses, including glassy spherules, whichhave been reported in large numbers from the NASA Phoenixmission lander. The origin and likely formation processes of thestrongly magnetic spherules in the Northern Hemisphere of Marsare still matter of speculation.

Table 1: Summary of selected results obtained on someMartian meteorites: ACM: amorph. carbon. matter; G graphite.

1. Tissint Fall ACM, GOlivine-Phyric Shergottite

2. Yamato 000593 Find ACM, GNakhlite

3. SaU 060 Find ACM, GOlivine-Phyric Shergottite

4. NWA 8171 (and pairs) Find ACM, GBasaltic Regolith Breccia

5. NWA 7032 and 7320 Finds ACMMicrogabbroic Shergottites

6. KG 002 Find ACM, GBasaltic Shergottite

7. NWA 2737 Find ACM, GChassignite (shocked dunite)Figure 1: NWA 2737 – ACM and graphite (with olivine).

C-GOl

Figure 2:Tissint,30-45 GPapeak shock.

The effects of shock metamorphism have to be investigated systematically on Martian meteorites as well as on returned samples, on site and in the laboratory, to control the possible consequences for the magnetic record or chronology/dating. Deeper knowledge concerning peak shock pressures and temperatures and the related mineralogical alterations would allow critical evaluation of respective data (see eg. fig. 2, Raman Spectroscopy).

However, even more important will be studying shock effects directly on the carriers of the magnetic record (oxides, sulfides etc.) and the consequences for the (paleo-) magnetic information itself because our knowledge in this direction is quite poor presently.

During the last years a large number of new Martian meteorites have been reported (MetBull 2018), including several unique types such as NWA 7034 and pairs, the first basaltic regolith breccia.These findings significantly expand the number and weight of meteorites – rcok samples – from the Red Planet which we have in hands for present and future investigations. In table 2 (left side) we have summarized selected magnetic data of a set of new Martian meteorites.

Figure 2:NWA 8171 –unique basaltic regolithbreccia.

Figure 3: Magnetic experiments under space conditions are urgently required in order to understand the physical background of the magnetic record concerning the strong magnetic anomalies on the surface of Mars as well as the (paleo-) magnetic signature of Martian rocks and magnetic recorders. It would be storngly favorable to have a lander on one of these magnetic anomaly sites.

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