FREE RADICAL OXIDATION AND ERYTHROCYTE AGGREGATION AFTER THERMIC INJURY EFFECT OF ALPHATOCOPHEROL

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EFFECT OF LIPID PEROXIDE OXIDATION ON ERYTHROCYTE FLEXIBILITY IN BURNS AND ALPHA-TOCOFEROL TREATMENT

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PLATELET AGGREGATION AFTER EXPERIMENTAL BURN INJURY AND THERAPY

Based on data concerning the coagulation changes after thermal injury the authors studied platelet aggregation after burn and its treatment. Severe thermal injury of Ha and lib degree was inflicted in white male rats (200 ±20 g b. m.) under aether anaesthesia. It ranged over 17,5 ± 2,5 % of the body surface. The animals were divided into the following groups: 1) burned non-treated; 2) burned and treated with Sol. Hartmanni (Hr), 3) burned and treated with Hemodex (Hx), and 4) controls. The treatment was intraperitoneally carried out immediately after the injury as well as on 6th and 24th hour after it. An elevation of the platelet aggregation for all the groups on the 24th hour after the injury was established

ALPHA-TOCOPHEROL STABILIZES ERYTHROCYTE MEMBRANE DURING THE EARLY STAGE AFTER THERMAL TRAUMA

Standard thermal trauma of 3rda - 3rdb degree, of 15-20 per cent of body surface was induced on white male Wistar rats narcotized with thiopental The changes of the concentration of thioharhituric acid (TBA)- reactive products, the activity of some antioxidant enzymes such as superoxide dismutase (SOD), glucose-6-phosphate dehydrogenase (G-6-PD), and catalase as well as the percentage of haemolysis were investigated during the early post-burn period (24, 48, and 72 hours after burning). It was demonstrated that erythrocyte haemolysis increased along with activation of lipid peroxidation (LPO) after thermic injury. Alpha-tocopherol treatment in a dose of 20 mg/kg body mass reduced the elevated levels of TBA-reactive products and enhanced erythrocytic antioxidant defence and resistance. It could be clarified that LPO activation played an important role in the haemolysis and that alpha-tocopherol stabilized erythrocyte membrane after burns

SOME THROMBOCYTIC AND ERYTHROCYTIC PARAMETERS AFTER BURNING (EXPERIMENTAL INVESTIGATIONS)

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Spatially resolved observations of a split-band coronal type-II radio burst

Context. The origin of coronal type-II radio bursts and of their band-splitting are still not fully understood. Aims. To make progress in solving this problem on the basis of one extremely well observed solar eruptive event. Methods. The relative dynamics of multi-thermal eruptive plasmas, observed in detail by the SDO/AIA and of the harmonic type-II burst sources, observed by the NRH at ten frequencies from 445 to 151 MHz, is studied for the partially behind the limb event on 3 November 2010. Special attention is given to the band-splitting of the burst. Analysis is supplemented by investigation of coronal hard X-ray (HXR) sources observed by the RHESSI. Results. It is found that the flare impulsive phase was accompanied by the formation of a double coronal HXR source, whose upper part coincided with the hot (T~10 MK) eruptive plasma blob. The leading edge (LE) of the eruptive plasmas (T~1-2 MK) moved upward from the flare region with the speed of v=900-1400 km/s. The type II burst source initially appeared just above the LE apex and moved with the same speed and in the same direction. After about 20 s it started to move about twice faster, but still in the same direction. At any given moment the low frequency component (LFC) source of the splitted type-II burst was situated above the high frequency component (HFC) source, which in turn was situated above the LE. It is also found that at a given frequency the HFC source was located slightly closer to the photosphere than the LFC source. Conclusions. The shock wave, which could be responsible for the observed type-II radio burst, was initially driven by the multi-temperature eruptive plasmas, but later transformed to a freely propagating blast shock wave. The most preferable interpretation of the type-II burst splitting is that its LFC was emitted from the upstream region of the shock, whereas the HFC - from the downstream region.Comment: 14 pages, 10 figure

On the Nature and Genesis of EUV Waves: A Synthesis of Observations from SOHO, STEREO, SDO, and Hinode

A major, albeit serendipitous, discovery of the SOlar and Heliospheric Observatory mission was the observation by the Extreme Ultraviolet Telescope (EIT) of large-scale Extreme Ultraviolet (EUV) intensity fronts propagating over a significant fraction of the Sun's surface. These so-called EIT or EUV waves are associated with eruptive phenomena and have been studied intensely. However, their wave nature has been challenged by non-wave (or pseudo-wave) interpretations and the subject remains under debate. A string of recent solar missions has provided a wealth of detailed EUV observations of these waves bringing us closer to resolving their nature. With this review, we gather the current state-of-art knowledge in the field and synthesize it into a picture of an EUV wave driven by the lateral expansion of the CME. This picture can account for both wave and pseudo-wave interpretations of the observations, thus resolving the controversy over the nature of EUV waves to a large degree but not completely. We close with a discussion of several remaining open questions in the field of EUV waves research.Comment: Solar Physics, Special Issue "The Sun in 360",2012, accepted for publicatio

Models and data analysis tools for the Solar Orbiter mission

Context. The Solar Orbiter spacecraft will be equipped with a wide range of remote-sensing (RS) and in situ (IS) instruments to record novel and unprecedented measurements of the solar atmosphere and the inner heliosphere. To take full advantage of these new datasets, tools and techniques must be developed to ease multi-instrument and multi-spacecraft studies. In particular the currently inaccessible low solar corona below two solar radii can only be observed remotely. Furthermore techniques must be used to retrieve coronal plasma properties in time and in three dimensional (3D) space. Solar Orbiter will run complex observation campaigns that provide interesting opportunities to maximise the likelihood of linking IS data to their source region near the Sun. Several RS instruments can be directed to specific targets situated on the solar disk just days before data acquisition. To compare IS and RS, data we must improve our understanding of how heliospheric probes magnetically connect to the solar disk.Aims. The aim of the present paper is to briefly review how the current modelling of the Sun and its atmosphere can support Solar Orbiter science. We describe the results of a community-led effort by European Space Agency's Modelling and Data Analysis Working Group (MADAWG) to develop different models, tools, and techniques deemed necessary to test different theories for the physical processes that may occur in the solar plasma. The focus here is on the large scales and little is described with regards to kinetic processes. To exploit future IS and RS data fully, many techniques have been adapted to model the evolving 3D solar magneto-plasma from the solar interior to the solar wind. A particular focus in the paper is placed on techniques that can estimate how Solar Orbiter will connect magnetically through the complex coronal magnetic fields to various photospheric and coronal features in support of spacecraft operations and future scientific studies.Methods. Recent missions such as STEREO, provided great opportunities for RS, IS, and multi-spacecraft studies. We summarise the achievements and highlight the challenges faced during these investigations, many of which motivated the Solar Orbiter mission. We present the new tools and techniques developed by the MADAWG to support the science operations and the analysis of the data from the many instruments on Solar Orbiter.Results. This article reviews current modelling and tool developments that ease the comparison of model results with RS and IS data made available by current and upcoming missions. It also describes the modelling strategy to support the science operations and subsequent exploitation of Solar Orbiter data in order to maximise the scientific output of the mission.Conclusions. The on-going community effort presented in this paper has provided new models and tools necessary to support mission operations as well as the science exploitation of the Solar Orbiter data. The tools and techniques will no doubt evolve significantly as we refine our procedure and methodology during the first year of operations of this highly promising mission.Peer reviewe