Understanding Of Chemical Evolution Research Articles

Affinity of Smectite and Divalent Metal Ions (Mg(2+), Ca(2+), Cu(2+)) with L-leucine: An Experimental and Theoretical Approach Relevant to Astrobiology.

Earth is the only known planet bestowed with life. Several attempts have been made to explore the pathways of the origin of life on planet Earth. The search for the chemistry which gave rise to life has given answers related to the formation of biomonomers, and their adsorption on solid surfaces has gained much attention for the catalysis and stabilization processes related to the abiotic chemical evolution of the complex molecules of life. In this communication, surface interactions of L-leucine (Leu) on smectite (SMT) group of clay (viz. bentonite and montmorillonite) and their divalent metal ion (Mg(2+), Ca(2+) and Cu(2+)) incorporated on SMT has been studied to find the optimal conditions of time, pH, and concentration at ambient temperature (298K). The progress of adsorption was followed spectrophotometrically and further characterized by FTIR, SEM/EDS and XRD. Leu, a neutral/non polar amino acid, was found to have more affinity in its zwitterionic form towards Cu(2+)- exchanged SMT and minimal affinity for Mg(2+)- exchanged SMT. The vibrational frequency shifts of -NH3 (+) and -COO(-) favor Van der Waal's forces during the course of surface interaction. Quantum calculations using density functional theory (DFT) have been applied to investigate the absolute value of metal ion affinities of Leu (Leu-M(2+) complex, M = Mg(2+), Ca(2+), Cu(2+)) with the help of their physico-chemical parameters. The hydration effect on the relative stability and geometry of the individual species of Leu-M(2+) × (H2O)n, (n =2 and 4) has also been evaluated within the supermolecule approach. Evidence gathered from investigations of surface interactions, divalent metal ions affinities and hydration effects with biomolecules may be important for better understanding of chemical evolution, the stabilization of biomolecules on solid surfaces and biomolecular-metal interactions. These results may have implications for understanding the origin of life and the preservation of biomarkers.

Extreme ultraviolet photolysis of CO2 ‐ H2O mixed ices at 10 K

Experimental results on the spectral identification of IR absorption features and the production and depletion column densities produced through EUV photolysis of H2O + CO2 (4:1) mixed ices at 10 K are reported. A tunable intense synchrotron radiation light source was employed to provide the required high flux EUV photons. In this study the photon wavelengths used to irradiate the icy sample were selected to coincide with the prominent solar lines at 58.4 nm and 30.4 nm. A FTIR spectrometer was employed to obtain the in situ IR absorbance spectra produced through EUV photolysis of a given ice sample. Photon‐induced chemical reaction products were primarily H2CO3 and CO. While new molecular species were formed, the original reactants were depleted, as expected. We report the yields for producing H2CO3 and CO and the yields for depleting the parent CO2 molecule through EUV photolysis of the mixed ices. We have searched for possible intermediate products H2CO and HCO, but could not positively identify their existences in the spectra. The results presented in this work are particular relevant to our understanding of chemical evolution and synthesis in H2O‐rich icy satellites of the giant planets, comets, the interstellar medium, molecular clouds, and protostellar regions.

Evolution of Gas and Dust in Circumstellar Disks

A clear understanding of the chemical processing of matter as it is transferred from a molecular cloud to a planetary system depends heavily on the physical conditions endured by gas and dust as these accrete onto a disk and are incorporated into planetary bodies. Reviewed here are astrophysical observations of circumstellar disks which trace their evolving properties. Accretion disks that are massive enough to produce a solar system like our own are typically larger than 100 AU. This suggests that the chemistry of a large fraction of the infalling material is not radically altered upon contact with a vigorous accretion shock. The mechanisms of accretion onto the star and eventual dispersal are not yet well understood, but timescales for the removal of gas and optically thick dust appear to be a few times 106 yrs. At later times, tenuous “debris disks” of dust remain around stars as old as a few times 108 yrs. Features in the morphology of the latter, such as inner holes, warps, and azimuthal asymmetries, are likely to be the result of the dynamical influence of large planetary bodies. Future observations will enlighten our understanding of chemical evolution and will focus on the search for disks in transition from a viscous accretion stage to one represented by a gas-free assemblage of colliding planetesimals. In the near future, comparative analysis of circumstellar dust and gas properties within a statistically significant sample of young stars at various ages will be possible with instrumentation such as SIRTF and SOFIA. Well-designed surveys will help place solar system analogs in a general context of a diversity of possible pathways for circumstellar evolution, one which encompasses the formation of stellar and brown-dwarf companions as well as planetary systems.

The organic chemistry and biology of the atmosphere of the planet Jupiter

In order to understand the chemical processes which may be taking place in the Jovian atmosphere, we have conducted a number of simulation experiments in the laboratory. These reactions appear to be significant for our understanding of chemical evolution and the nature and origin of organic matter in the universe. Mixtures of methane and ammonia in varying proportions have been exposed to electric discharges and the products analyzed. We have found that, as the methane and ammonia disappear, hydrogen cyanide and acetylene are to be built up. The analysis of the volatiles has also provided us with a wide range of aminonitriles. It is conceivable that some of these nitriles, on hydrolysis, will give rise to amino acids. On cyclization, some of them would provide the pathways for the origin of pyrimidines. A characteristic result of these reactions has also been the appearance of a red polymer which may have a bearing on the color in the red spots of Jupiter. Spectral analysis in the laboratory may provide some clues in our search for organic material in the Jovian atmosphere by orbiting spacecraft, or ground-based observations.