Impact of ultrasounds and high voltage electrical discharges on physico-chemical properties of rapeseed straw's lignin and pulps.

In this study, ultrasound (US) and high voltage electrical discharges (HVED) were combined with chemical treatments (soda or organosolv) for rapeseed straw delignification. Delignification was improved by both physical pretreatments. US increased the extractability of hemicelluloses and HVED induced a partial degradation of cellulose. Best synergies were observed for HVED-soda and US-organosolv treatments. The obtained lignin fractions were characterized with 13C NMR and 2D 1H-13C HSQC. It was observed that the physical treatments affected the syringyl/guaiacyl (S/G) ratios. The values of S/G were ≈1.19, 1.31 and 1.75 for organosolv, HVED-organosolv and US-organosolv processes, suggesting recondensation reactions. The lignin fractions obtained from HVED-organosolv treatment contained less quantity of p-coumaric acid and ferulic acid as compared to those extracted by US-organosolv. Thermogravimetric analysis (TGA) revealed a better heat resistance of physically extracted lignins as compared to the control. The enzymatic digestibility increased by 24.92% when applying HVED to mild organosolv treatment.

A new gamma-ray burst classification scheme from GRB 060614.

Gamma-ray bursts (GRBs) are known to come in two duration classes, separated at approximately 2 s. Long-duration bursts originate from star-forming regions in galaxies, have accompanying supernovae when these are near enough to observe and are probably caused by massive-star collapsars. Recent observations show that short-duration bursts originate in regions within their host galaxies that have lower star-formation rates, consistent with binary neutron star or neutron star-black hole mergers. Moreover, although their hosts are predominantly nearby galaxies, no supernovae have been so far associated with short-duration GRBs. Here we report that the bright, nearby GRB 060614 does not fit into either class. Its approximately 102-s duration groups it with long-duration GRBs, while its temporal lag and peak luminosity fall entirely within the short-duration GRB subclass. Moreover, very deep optical observations exclude an accompanying supernova, similar to short-duration GRBs. This combination of a long-duration event without an accompanying supernova poses a challenge to both the collapsar and the merging-neutron-star interpretations and opens the door to a new GRB classification scheme that straddles both long- and short-duration bursts.

An origin for short gamma-ray bursts unassociated with current star formation.

Two short (< 2 s) gamma-ray bursts (GRBs) have recently been localized and fading afterglow counterparts detected. The combination of these two results left unclear the nature of the host galaxies of the bursts, because one was a star-forming dwarf, while the other was probably an elliptical galaxy. Here we report the X-ray localization of a short burst (GRB 050724) with unusual gamma-ray and X-ray properties. The X-ray afterglow lies off the centre of an elliptical galaxy at a redshift of z = 0.258 (ref. 5), coincident with the position determined by ground-based optical and radio observations. The low level of star formation typical for elliptical galaxies makes it unlikely that the burst originated in a supernova explosion. A supernova origin was also ruled out for GRB 050709 (refs 3, 31), even though that burst took place in a galaxy with current star formation. The isotropic energy for the short bursts is 2-3 orders of magnitude lower than that for the long bursts. Our results therefore suggest that an alternative source of bursts--the coalescence of binary systems of neutron stars or a neutron star-black hole pair--are the progenitors of short bursts.

A short gamma-ray burst apparently associated with an elliptical galaxy at redshift z = 0.225.

Gamma-ray bursts (GRBs) come in two classes: long (> 2 s), soft-spectrum bursts and short, hard events. Most progress has been made on understanding the long GRBs, which are typically observed at high redshift (z approximately 1) and found in subluminous star-forming host galaxies. They are likely to be produced in core-collapse explosions of massive stars. In contrast, no short GRB had been accurately (< 10'') and rapidly (minutes) located. Here we report the detection of the X-ray afterglow from--and the localization of--the short burst GRB 050509B. Its position on the sky is near a luminous, non-star-forming elliptical galaxy at a redshift of 0.225, which is the location one would expect if the origin of this GRB is through the merger of neutron-star or black-hole binaries. The X-ray afterglow was weak and faded below the detection limit within a few hours; no optical afterglow was detected to stringent limits, explaining the past difficulty in localizing short GRBs.

The heating of gas in a galaxy cluster by X-ray cavities and large-scale shock fronts.

Most of the baryons in galaxy clusters reside between the galaxies in a hot, tenuous gas. The densest gas in their centres should cool and accrete onto giant central galaxies at rates of 10-1,000 solar masses per year. No viable repository for this gas, such as clouds or new stars, has been found. New X-ray observations, however, have revealed far less cooling below X-ray temperatures than expected, altering the previously accepted picture of cooling flows. As a result, most of the gas must be heated to and maintained at temperatures above approximately 2 keV (ref. 3). The most promising heating mechanism is powerful radio jets emanating from supermassive black holes in the central galaxies of clusters. Here we report the discovery of giant cavities and shock fronts in a distant (z = 0.22) cluster caused by an interaction between a radio source and the hot gas surrounding it. The energy involved is approximately 6 x 10(61) erg, the most powerful radio outburst known. This is enough energy to quench a cooling flow for several Gyr, and to provide approximately 1/3 keV per particle of heat to the surrounding cluster.

1H-NMR on line monitoring of water activity during lipase catalysed esterification.

1H-NMR spectroscopy is used to determine simultaneously the water activity (aw) and the time course of an esterification reaction catalysed by a lipase. Chemical shifts signals of hydroxylic hydrogens in fast exchange (i.e the average hydroxylic signal of acid, alcohol and water) varies with water activity and ester content. Calibration curves have been established from model media composed of the substrates and various ester contents, at different water activities, in order to mimic a reaction medium. One relationship is established between water activity, hydroxylic hydrogen signal chemical shift and ester content. In order to estimate the water activity evolution as a function of time, this last relationship is applied to the hydroxylic hydrogen chemical shift measured in a reaction medium where the Rhizomucor miehei lipase in a powder form is suspended in the liquid substrates. This alternative way of determining the water activity based on hydroxylic hydrogen chemical shift presents some advantages over more classical means, i.e. time saved and inaccuracies avoided by monitoring without handling the sample.

NMR on-line monitoring of esterification catalyzed by cutinase.

A nuclear magnetic resonance (NMR) method has been developed to monitor on-line lipase-catalyzed esterification reactions without the need to sample the reaction medium. The technique, through (1)H NMR, measures the concentrations of alcohol, ester, hydroxylic hydrogens in the organic phase, and hydroxylic hydrogens in the aqueous phase, if any. Also, the chemical shift evolution of the two types of hydroxylic hydrogens has been followed, providing information on water content of the organic phase and on the appearance of a distinct aqueous phase. As far as (13)C NMR is concerned, it has been possible to measure, first the acid and the ester concentrations in the carbonyl region, and second, the alcohol and the ester concentrations in the methylene region. All (1)H and (13)C results are in agreement with one another. Furthermore, NMR allows for the choice of detection zone. Preliminary studies on the solid phase proved the presence of much more water in the solid phase than in the organic phase, and also gave evidence of the existence of two types of esters, one in the organic phase, mainly associated with the acid, and the other one not associated with the acid, most probably entrapped within the solid enzyme.

Water activity by 1H nuclear magnetic resonance spectroscopy: application to the study of water exchange in biphasic media.

The water activity (alpha w) of the liquid phase is investigated by means of 1H NMR for both monophasic and biphasic systems. The chemical shift or the area of the signal of the hydroxylic hydrogens is compared to calibration curves obtained from mixtures equilibrated at different water activities, thus allowing determination of the alpha w of the system. The chemical shift varies linearly as a function of the alpha w of the system. Through simple calculation the hydroxylic hydrogen concentration obtained from the area gives the water concentration in the medium; the sorption curve is thus obtained through NMR. The application of this method to a biphasic system composed of a liquid phase (an equimolar mixture of acid-alcohol) and a solid phase (a lipase), equilibrated separately at two different water activities, gives information on the water exchange between both phases during the lag phase of the esterification reaction. Light and slow water exchanges are observed from the solid phase at high alpha w toward the liquid phase at low alpha w. The lag phase of the esterification reaction is too short for the water activity equilibrium to be reached before the reaction starts.