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Elementary contents (weight percentage) in extraterrestrial minerals and terrestrial basalts. Perseus hardware (Exobiology experiment) onboard MIR space station. Mounted hardware (core module). Principal scheme of sample cavity in Perseus hardware. MgF 2 glass. Dry films (samples). - PowerPoint PPT Presentation
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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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20
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40
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60
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. .