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

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).

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

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  1. Elementary contents (weight percentage) in extraterrestrial minerals and terrestrial basalts Nordic winter school on Astrobiology

  2. Perseus hardware (Exobiology experiment) onboard MIR space station Mounted hardware (core module) Nordic winter school on Astrobiology

  3. Principal scheme of sample cavity in Perseus hardware MgF2 glass Dry films (samples) Experimental tube MgF2 glass Dry films (samples) Nordic winter school on Astrobiology

  4. Outside container, placed on the outer surface of Kosmos-2044 spacecraft; (A) Baseplate with sample holders. (B) Temperature sensor. (C) Gamma radiation dosimeter (D) Dry samples (Uridine + inorganic phosphate. Flight duration - 14 days, temperature variations from -13оС to +67о. D D D A B A C Nordic winter school on Astrobiology

  5. Meduza cassette device for outside samples exposure Nordic winter school on Astrobiology

  6. Table 1 Quantitative yield of nucleotides (in % from initial nucleoside) synthesized in course of experiments performed at Earth orbit 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 3.23 23c 0.06 0.04 0.05 1.12 2 0.09 0.07 0.01 0.82 3 0.05 0.03 0.03 0.71 35c 0.01 0.01 0.08 0.01 Total yield 0.33 0.25 0.27 5.8 Ado decay 51 58 50 51 dAdo 5 0.07 0.05 0.01 1.87 3 0.06 0.03 0.008 0.48 35c 0.03 0.02 Traces traces Total 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 23c 0.10 0.10 0.94 2 0.04 0.03 0.61 3 0.02 0.01 0.55 35c traces traces traces Total yield 0.30 0.25 4.78 Cyd decay 64 76 66 Urd 5 0.08 0.100 0.07 1.20 23c traces 0.001 traces 0.05 2 0.05 0.030 0.03 0.08 3 0.03 0.020 0.01 0.05 35c traces traces traces traces Total yield 0.16 0.15 0.11 2.10 Urd decay 70 65 70 65 Nordic winter school on Astrobiology *Experiments were performed for uridine (Urd) only **Experiments were performed for adenosine (Ado), deoxyadenosine (dAdo) and cytosine (Cyt)

  7. Nordic winter school on Astrobiology

  8. Formation of 5’UMP (in % of the initial uridine amount) in different radiation conditions Nordic winter school on Astrobiology

  9. Mercury lamp (254 nm) +250C; 4.4*107J*m-2 CO2, N2, O2 Sample exposed (solid film, 1 cm2) MgF2 glass Principal scheme of sample cavity in the experimental hardware Nordic winter school on Astrobiology

  10. Confocal microscope imaging of irradiated pellicles • Filaments of adenosine shaped as branches without any mineral inclusions (up) and with lunar soil particles (down) Nordic winter school on Astrobiology

  11. Formation of 5’AMP and survival of initial AMP in laboratory experiments Time, hours Time, hours B – in absence of lunar soil, C – in presence of lunar soil Nordic winter school on Astrobiology

  12. Formation of 5’AMP and survival of initial AMP in laboratory experiments Nordic winter school on Astrobiology

  13. Aminoacids: experimental objectives • To simulate some Martian environmental factors in laboratory conditions • To study the influence of Martian soil analogues (limonite and basalt) over destruction of peptides irradiated by UV 254 • To evaluate the effect of different type of atmospheres on prebiotic synthesis of organic molecules • To reveal the action of different Martian soil components over prebiotic synthesis Nordic winter school on Astrobiology

  14. Current Martian atmospheric data Surface atmospheric pressure: ~6.1 mb (about 1/150th that of Earth's) Surface gas density: ~0.020 kg/m3 Atmospheric scale height: 11.1 km Average temperature: ~210 K (-63 degrees Celsius) Wind speeds: 2-7 m/s (summer), 5-10 m/s (fall), 17-30 m/s (dust storm) • Carbon Dioxide (CO2) - 95.32% (percentage by moles): Nitrogen (N2) - 2.7; Argon (Ar) - 1.6% ; Oxygen (O2) - 0.13%; Carbon Monoxide (CO) - 0.08% • Minor (ppm): Water (H2O) – 210; Nitrogen Oxide (NO) – 100; Neon (Ne) - 2.5; Krypton (Kr) - 0.3; Xenon (Xe) - 0.08 Nordic winter school on Astrobiology

  15. Properties and percentages of Martian soil *The chemical compositionwas 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) Nordic winter school on Astrobiology

  16. Stability of Phe irradiated by VUV254 in presence of Martian soil analogues B – in the absence of minerals; C – In association with limonite D – in association with basalt Nordic winter school on Astrobiology

  17. Formation of polypeptides after UV254 exposure of dry films Phe+Gly B – in the absence of minerals; C – In association with limonite D – in association with basalt Nordic winter school on Astrobiology

  18. Formation of dipeptides(GG) after UV254 exposure of dry samples B – in the absence of minerals; C – In association with limonite D – in association with basalt Nordic winter school on Astrobiology

  19. Stability of Phe and Gly after 5 months of irradiation associated with different minerals (% of the initial amount) Nordic winter school on Astrobiology

  20. Photochemical survival of Phe in different type of atmospheres Nordic winter school on Astrobiology

  21. Interaction of montmorillonite ((Na,K,Ca)(Аl,Fe,Мg)[(Si,Al)4O10](OH)2*nH2O) catalytic cites and aminoacid molecules leading to the peptide bond formation 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 toAlO- 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. Nordic winter school on Astrobiology

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

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