Expanded Bed Adsorption Of Bromelain (e.c. 3.4.22.33) From Ananas Comosus Crude Extract

This work focuses on the adsorption of Bromelain in expanded bed conditions, such as the adsorption kinetics parameters. The adsorption kinetics parameters showed that after 40 minutes equilibrium was achieved and maximum adsorption capacity was 6.11 U per resin mL. However, the maximum adsorption capacity was only determined by measuring the adsorption isotherm. Only by the Langmuir model the maximum adsorption capacity, Qm, and dissociation constant, kd, values could be estimated as 9.18 U/mL and 0.591, respectively, at 25°C and 0.1 mol/L phosphate buffer pH 7.5. A column made of glass with an inner diameter of 1 cm was used for the expanded bed adsorption (EBA). The residence time was reduced 10 fold by increasing the expansion degree 2.5 times; nonetheless, the plate number (N) value was reduced only 2 fold. After adsorption, the bromelain was eluted in packed bed mode, with a downward flow. The purification factor was about 13 fold and the total protein was reduced 4 fold. 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N–O bearing molecules produced by radiolysis of N2O and N2O:CO2 ices

International audienceN2O and CO2 can be formed in the interstellar space and in ices on the surface of outer solar system bodies, such as Pluto and Triton. Energetic ions can simulate the energy transfer processes that occur by cosmic ray irradiation of interstellar ices, comets, and icy solar system bodies. Proceeding systematic research, pure nitrous oxide (N2O) ice, and nitrous oxide and carbon dioxide (CO2) ice mixture were irradiated at 11 K with MeV-nitrogen (N+) and -xenon (Xe23+) ion beams. The chemical and physical effects induced by ion irradiation on the N2O ice and the N2O:CO2 ice mixture are compared. The formation and dissociation cross sections scale with the electronic stopping power (Se) roughly as σ ∼ a Sen, where n ∼ 3/2. The n power law is helpful for predicting the N2O formation and dissociation cross-sections for other ion beam projectiles and energies; these predictions will allow estimating the effects of the entire cosmic ray radiation field

Radiolysis of NH3:CO ice mixtures – implications for Solar system and interstellar ices

International audienceExperimental results on the processing of NH3:CO ice mixtures of astrophysical relevance by energetic (538 MeV 64 Ni 24+) projectiles are presented. NH 3 and CO are two molecules relatively common in interstellar medium and Solar system; they may be precursors of amino acids. 64 Ni ions may be considered as representative of heavy cosmic ray analogues. Laboratory data were collected using mid-infrared Fourier transform spectroscopy and revealed the formation of ammonium cation (NH + 4), cyanate (OCN −), molecular nitrogen (N 2), and CO 2. Tentative assignments of carbamic acid (NH 2 COOH), formate ion (HCOO −), zwitterionic glycine (NH + 3 CH 2 COO −), and ammonium carbamate (NH + 4 NH 2 COO −) are proposed. Despite the confirmation on the synthesis of several complex species bearing C, H, O, and N atoms, no NO bearing species was detected. Moreover, parameters relevant for computational astrophysics, such as destruction and formation cross-sections, are determined for the precursor and the main detected species. Those values scale with the electronic stopping power (S e) roughly as σ ∼ a S n e , where n ∼ 3/2. The power law is helpful for predicting the CO and NH 3 dissociation and CO 2 formation cross-sections for other ions and energies; these predictions allow estimating the effects of the entire cosmic ray radiation field

Destruction of CO ice and formation of new molecules by irradiation with 28 keV O6+ ions

International audienceThe effect of solar wind on cometary ice was studied by using oxygen ions with energy near to that corresponding to their maximum abundance in space for bombarding CO ice. This gas was condensed on a CsI substrate at 14 K and irradiated by 28 keV 18O6+ ions up to a final fluence of 1.3 x 1016 cm-2. We have used a methodology in which the sputtering yields, the destruction rate of CO, and the rate of formation of new molecular species are determined by Fourier transform infrared spectroscopy (FTIR). In the current experiment, the condensation of a thin water ice film has prevented the CO sputtering. Quantities such as the dissociation yield, Yd (the number of ice molecules destroyed or dissociated per projectile impact), and the formation yield, Yf (the number of daughter molecules of a given species formed per projectile) are found to be more appropriate and useful than using an integrated or average cross section, since the projectiles are slowing down in the ice from their initial energy until zero velocity (implantation)

Compaction of porous ices rich in water by swift heavy ions

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Swift heavy ion modifications of astrophysical water ice

International audienceIn the relatively shielded environments provided by interstellar dense clouds in our Galaxy, infraredastronomical observations have early revealed the presence of low temperature (10–100 K) ice mantlescovering tiny grain ‘‘cores” composed of more refractory material. These ices are of specific interestbecause they constitute an interface between a solid phase under complex evolution triggered by energeticprocesses and surface reactions, with a rich chemistry taking place in the gas phase. The interstellarice mantles present in these environments are immersed, in addition to other existing radiations fields, ina flux of cosmic ray particles that can produce new species via radiolysis processes, but first affects theirstructure, which may change and also induces desorption of molecules and radicals from these grains.Theses cosmic rays are simulated by swift ions in the laboratory for a better understanding of astrophysicalprocesses