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Page 1: Elementary contents (weight percentage) in extraterrestrial minerals and terrestrial basalts

Nordic winter school on Astrobiology

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Elementary contents (weight Elementary contents (weight percentage) in extraterrestrial percentage) in extraterrestrial

minerals and terrestrial basaltsminerals and terrestrial basalts

0

10

20

30

40

50

SiO2 TiO2 Al2O3 FeO MgO CaO Na2O

Lunar soil Chondrites Terrstial basalts

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Perseus hardware (Exobiology Perseus hardware (Exobiology experiment) onboard MIR space experiment) onboard MIR space

stationstation

Mounted hardware (core module)

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Principal scheme of sample cavity in Principal scheme of sample cavity in Perseus hardwarePerseus hardware

MgF2 glass

Dry films (samples)

Experimental tube

Dry films (samples)

MgF2

glass

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A

A

B

C

D DD

Outside container, placed on the outer surface of Outside container, placed on the outer surface of Kosmos-2044 spacecraftKosmos-2044 spacecraft; ;

(A) (A) Baseplate with sample holdersBaseplate with sample holders. (B) . (B) Temperature sensorTemperature sensor. . (C) (C) Gamma radiation dosimeter Gamma radiation dosimeter (D) (D) Dry samples (Uridine + Dry samples (Uridine +

inorganic phosphateinorganic phosphate. . Flight duration - Flight duration - 14 14 daysdays, , temperature variations fromtemperature variations from -13 -13ооС С

toto +67 +67оо..

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Meduza cassette device for outside Meduza cassette device for outside samples exposuresamples exposure

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Nucleoside Products analyzed

Salut-7, 13 months

Salut-7, 16 months

MIR, 113 days Cosmos-2044* Bion-11** (14 days)

Ado 5 0.12 0.10 0.10 3.2323c 0.06 0.04 0.05 1.12

2 0.09 0.07 0.01 0.823 0.05 0.03 0.03 0.71

35c 0.01 0.01 0.08 0.01Total yield 0.33 0.25 0.27 5.8

Ado decay 51 58 50 51

dAdo 5 0.07 0.05 0.01 1.873 0.06 0.03 0.008 0.48

35c 0.03 0.02 Traces tracesTotal yield 0.16 0.10 0.018 2.35

dAdo decay 79 80 80 46

Cyt 5 0.14 0.11 Not exposed 2.68

23c 0.10 0.10 0.94

2 0.04 0.03 0.61

3 0.02 0.01 0.55

35c traces traces traces

Total yield 0.30 0.25 4.78

Cyd decay 64 76 66

Urd 5 0.08 0.100 0.07 1.2023c traces 0.001 traces 0.05

2 0.05 0.030 0.03 0.083 0.03 0.020 0.01 0.05

35c traces traces traces tracesTotal yield 0.16 0.15 0.11 2.10

Urd decay 70 65 70 65

*Experiments were performed for uridine (Urd) only

**Experiments were performed for adenosine (Ado), deoxyadenosine (dAdo) and cytosine (Cyt) 

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Formation of 5’UMP (in % of the initial Formation of 5’UMP (in % of the initial uridine amount) in different radiation uridine amount) in different radiation

conditionsconditions

1,2

4

2,7

1,5

0,150

1

2

3

4Kosm

os

2044

Heatn

g

VU

V 1

45

nm

gam

ma

radia

tion

UV 2

54

nm

5'UMP

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Principal scheme of sample cavity in Principal scheme of sample cavity in the experimental hardwarethe experimental hardware

Mercury lamp

(254 nm) +250C;

4.4*107J*m-2

Sample exposed (solid film, 1 cm2)

MgF2 glass

CO2, N2, O2

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Confocal microscope imaging of Confocal microscope imaging of irradiated pelliclesirradiated pellicles

Filaments of Filaments of adenosine shaped adenosine shaped

as branches as branches without any without any

mineral inclusions mineral inclusions (up) and with (up) and with

lunar soil particles lunar soil particles (down) (down)

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Formation of 5’AMP and survival of initial Formation of 5’AMP and survival of initial AMP in laboratory experimentsAMP in laboratory experiments

B – in absence of lunar soil,

C – in presence of lunar soil

Time, hoursTime, hours

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Formation of 5’AMP and survival of initial Formation of 5’AMP and survival of initial AMP in laboratory experimentsAMP in laboratory experiments

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Aminoacids: experimental Aminoacids: experimental objectivesobjectives

To To simulate some Martian environmental simulate some Martian environmental factors in laboratory conditionsfactors in laboratory conditionsTo study the influenceTo study the influence of Martian soil of Martian soil analogues (limonite and analogues (limonite and basalt) basalt) over over destruction of peptides irradiated by UV destruction of peptides irradiated by UV 254254

To evaluate the effect of different To evaluate the effect of different type of type of atmospheres on prebiotic synthesis of atmospheres on prebiotic synthesis of organic molecules organic molecules To reveal the action of different Martian soil To reveal the action of different Martian soil components over prebiotic synthesiscomponents over prebiotic synthesis

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Surface atmospheric pressure: ~6.1 mb (about 1/150th that Surface atmospheric pressure: ~6.1 mb (about 1/150th that of Earth's) of Earth's) Surface gas density: ~0.020 kg/mSurface gas density: ~0.020 kg/m3 3

Atmospheric scale height: 11.1 km Atmospheric scale height: 11.1 km Average temperature: ~210 K (-63 degrees Celsius) Average temperature: ~210 K (-63 degrees Celsius) Wind speeds: 2-7 m/s (summer), 5-10 m/s (fall), 17-30 m/s Wind speeds: 2-7 m/s (summer), 5-10 m/s (fall), 17-30 m/s (dust storm) (dust storm)

Carbon Dioxide (COCarbon Dioxide (CO22) - 95.32% (percentage by moles): ) - 95.32% (percentage by moles):

Nitrogen (NNitrogen (N22) - 2.7) - 2.7; ; Argon (Ar) - 1.6% Argon (Ar) - 1.6% ; ; Oxygen (OOxygen (O22) - ) -

0.13%0.13%; ; Carbon Monoxide (CO) - 0.08% Carbon Monoxide (CO) - 0.08% Minor (pMinor (pppm): Water (Hm): Water (H22O) – 210O) – 210; ; Nitrogen Oxide (NO) – Nitrogen Oxide (NO) –

100100; ; Neon (Ne) - 2.5Neon (Ne) - 2.5; ; Krypton (Kr) - 0.3Krypton (Kr) - 0.3; ; Xenon (Xe) - 0.08 Xenon (Xe) - 0.08

Current Martian atmospheric data

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0

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SiO2 TiO2 Al2O3 Fe2O3 MgO CaO Na2O MnO

MARTIAN SOIL* Tiatia basalt

*The chemical composition was determined by the two Viking Landers and by the Pathfinder rover (average of about 5 sites at the Pathfinder landing site Science, volume 278, December 5, 1997)

PProperties and percentages ofroperties and percentages of Martian soilMartian soil

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Stability of Phe irradiated by VUVStability of Phe irradiated by VUV254254 in presence of in presence of

Martian soil analoguesMartian soil analogues

B – in the absence of minerals; C – In association with limonite D – in association with basalt

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Formation of polypeptides after UVFormation of polypeptides after UV254254 exposure of dry films Phe+Glyexposure of dry films Phe+Gly

B – in the absence of minerals; C – In association with limonite D – in association with basalt

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Formation of dipeptides(GG) after UVFormation of dipeptides(GG) after UV254254

exposure of dry samplesexposure of dry samples

B – in the absence of minerals; C – In association with limonite D – in association with basalt

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Stability of Phe and Gly after 5 Stability of Phe and Gly after 5 months of irradiation associated with months of irradiation associated with

different minerals (% of the initial different minerals (% of the initial amount) amount)

39,648,04

39,6

50,02 47

57,0249,63

58,16

0

10

20

30

40

50

60Fel

d

spar

No

min

eral

Lim

onit

e

Bas

alt

GLY PHE

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49,643,3

30,95

4733,06

26,450

20

40

60

CO2 N2 O2

No mineral

BasaltNo mineral

Basalt

Photochemical survival of Phe in different Photochemical survival of Phe in different type of atmospherestype of atmospheres

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Interaction of montmorillonite (Interaction of montmorillonite ((Na,K,Ca)(Аl,Fe,Мg)(Na,K,Ca)(Аl,Fe,Мg)[(Si,Al)[(Si,Al)44OO1010](OH)](OH)22*nH*nH22O)O) catalytic cites and catalytic cites and

aminoacid molecules leading to the aminoacid molecules leading to the peptide bond peptide bond formationformation

а – Formation of catalytically active cites on the mineral surface. Activation of amino acid molecules occurs

on the edges of clay particles, enriched by AlO- groups.

в – Activation of functional groups of

zwitterions. Proton removal from aminogroup to AlO- of montmorillonite leads to the

formation of nucleophilic amino group, required for

dipeptide formation.с – Overall scheme of

peptide bond formation. Final dimerization reaction involves

to neighbor activated aminoacid molecules.

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BBasic asic conclusionsconclusions

The amplification of molecular structure could occur The amplification of molecular structure could occur under the action of VUV radiation leading to the under the action of VUV radiation leading to the formation of natural substancesformation of natural substances. . Lunar soil (CI), Murchison(CM2) and Allende (CV3) Lunar soil (CI), Murchison(CM2) and Allende (CV3) meteorites promote synthesis of polypeptides and meteorites promote synthesis of polypeptides and nucleotidesnucleotides..Solid-phase synthesis of important organic substances Solid-phase synthesis of important organic substances could occur at the surfaces of comets, asteroids, could occur at the surfaces of comets, asteroids, meteorites and dust particles (small Solar system meteorites and dust particles (small Solar system bodies)bodies)..Minerals of extraterrestrial origin exhibited protective Minerals of extraterrestrial origin exhibited protective properties against cosmic radiation thus allowing properties against cosmic radiation thus allowing protobiomolecules to survive during long-duration space protobiomolecules to survive during long-duration space journeyjourney..Biological important substances could have been Biological important substances could have been transported safely to the Earth surface during the transported safely to the Earth surface during the prebiotic period of its evolution and later contribute into prebiotic period of its evolution and later contribute into further evolving of organic matterfurther evolving of organic matter..Such an approach could help in solving the paradox of Such an approach could help in solving the paradox of quick life origin at the early Earthquick life origin at the early Earth. .


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