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Experimental studies on Hg 0 removal by CuCl 2 modified magnetospheres (Cu 6 –MF) injection were performed in an entrained flow reactor system. The factors affecting the Hg 0 removal efficiency were investigated, including the initial Hg 0 concentration, sorbent concentration in flue gas, sorbent particle size, sorbent residence time in flue gas, and flue gas temperature. The results indicated that, as the raise of initial Hg 0 concentration, the Hg 0 removal efficiency increased. The Hg 0 removal efficiency also increased with the increase of sorbent residence time and sorbent concentration in flue gas. When the residence time was 1.61 s and the sorbent concentration was 1.09 g/m 3 , the Hg 0 removal efficiency could reach to 80.6%. However, with the further increase of residence time and sorbent concentration, the Hg 0 removal efficiency did not increase continuously. The smaller particle size was favorable for the Hg 0 removal. In the industrial application, the particle size could be selected as 45–74 μm when comprehensively considering the Hg 0 removal efficiency, the cost of sorbent preparation, and other factors. The acid flue gases have negligible impacts on Hg 0 removal, while moisture plays a slightly negative role in Hg 0 removal under SFG atmosphere. With the superior Hg 0 removal performance, the Cu 6 –MF sorbent may presents great potentials for Hg 0 removal in coal-fired power plants. [ABSTRACT FROM AUTHOR]

The Hg 0 removal capacities of magnetospheres from fly ash collected from different power plants were investigated at a wide temperature range of 100–400 °C. The relationship between Hg 0 removal efficiency ( η T ) and iron content/species of magnetospheres was investigated. The magnetospheres attained the optimal Hg 0 removal capacity at 250 °C. The reaction temperature played an important role in Hg 0 adsorption and oxidation behaviors. At low reaction temperature (100 °C and 150 °C), the adsorption of Hg 0 played a predominant role in Hg 0 removal, while the Hg 0 removal mainly depended on the Hg 0 oxidation capacity at high temperature (200–400 °C). The Hg 0 removal capacity increased with the increase of iron content. The percentage of ferrospinel and hematite in magnetospheres is a key factor for determining the Hg 0 removal capacity as well. Hydrogen fluoride (HF) could remove the glass-phase materials on the magnetospheres and the active iron species embedded in the glass phase could be exposed and accessible. After fluorinated by HF, the Hg 0 removal capacity increased in different degree for different magnetospheres, which depended on the content of active iron species in raw magnetospheres. [ABSTRACT FROM AUTHOR]

The regeneration performance of spent catalyst after mercury removal as well as the involved reaction mechanism was investigated. The effects of restoration with or without O 2 and/or HCl, O 2 and HCl concentration, regeneration temperature, and heating rate on regeneration performance were studied, respectively. The results suggested that two steps were essential in the regeneration process: (1) releasing the sulfur and mercury species adsorbed on the catalyst; (2) restoring the surface chemistry of catalyst by O 2 and HCl. Optimal regeneration performance of spent catalyst was attained after thermal desorption at 400 °C and following by the restoration of O 2 and HCl. The changes in surface chemistry of catalyst revealed that the sulfur and mercury species could be fully released by heating at 400 °C, and the deactivated adsorption sites was exposed. With the assistance of O 2 and HCl, the surface chemistry of Cu and Cl was restored close to original CuCl 2 . Four cycles of mercury adsorption−catalyst regeneration showed that the mercury removal capacity did not vary appreciably with respect to fresh catalyst after multiple regeneration. [ABSTRACT FROM AUTHOR]

The Hg 0 adsorption and oxidation sites on the CuCl 2 -MF catalyst as well as the role of atomic Cu and Cl in Hg 0 removal were identified by a temperature programmed desorption (TPD) experiment. The reaction mechanism with the participation of O 2 and HCl was investigated. The changes in surface chemistry of fresh, spent and in situ pretreated catalyst with O 2 and/or HCl were investigated by EPR and XPS to better understand the intermediate reaction products and steps. The results suggested that different mercury adsorption sites are existed on the catalyst: Cl adsorption sites and Cu adsorption sites. The binding energy of mercury on the Cu adsorption sites is higher than that on the Cl adsorption sites. O 2 and HCl significantly affected the state of Cu and Cl on the spent catalyst. The interaction between Hg 0 and CuCl 2 with the participation of O 2 and/or HCl follows three steps mechanism: (1) the reduction of CuCl 2 to CuCl for the interaction with Hg 0 , (2) the reoxidation of CuCl for the interaction with O 2 forming an intermediate copper oxygen chloride species, (3) the rechlorination of oxychloride species resulting in the restoration of CuCl 2 . This demonstrated that the interaction between Hg 0 and CuCl 2 is a cycle when O 2 and HCl are contained in the reaction system. [ABSTRACT FROM AUTHOR]

To remove Hg 0 from coal combustion flue gas and eliminate secondary pollution of spent sorbent, a novel magnetic catalyst based on CuCl 2 modified magnetospheres from fly ash (CuCl 2 -MF) was developed. The solubility tests, electron paramagnetic resonance (EPR), X-ray diffraction (XRD), X-ray photoelectron spectroscopy (XPS), and physical property measurement system with vibrating sample magnetometer (PPMS-VSM) were employed to characterize the catalyst. The effects of CuCl 2 loading value and reaction temperature on Hg 0 removal performance were studied using a laboratory-scale fixed-bed reactor. The results suggested that the CuCl 2 loaded on the support is present mostly in an amorphous phase. Different copper coordinations are existed in the catalyst with different Cu loading: at low Cu loading, isolated Cu 2+ ions existed in a chlorine-free coordination; at high Cu loading, associated Cu 2+ ions existed in a chlorine-enriched coordination. The catalyst with optimal loading 6% CuCl 2 attained the highest Hg 0 removal efficiency (90.6%) at 150 °C. The chlorine-enriched coordination acted as the active adsorption sites for Hg 0 , while the chlorine-free coordination is inactive for Hg 0 removal. The CuCl 2 -MF catalyst showed good resistance to SO 2 for Hg 0 removal in the presence of HCl. Further, the management method for spent catalyst containing mercury was proposed, and the economic analysis of the technology was also conducted. [ABSTRACT FROM AUTHOR]

The magnetic properties of riverbed samples collected after the 2008 Tennessee Valley Authority (TVA) coal ash spill in Kingston, Tennessee are investigated. Coal ash persists in this fluvial environment because 400,000 m 3 of ash remains in areas that were not dredged. The magnetic fraction is low in comparison to other coal ash; 1.4 wt% in a sample from the failed ash storage cell increasing to 3.0 wt% in riverbed samples in the Emory River near the spill. Thermomagnetic analysis, XRD, SEM and polarized light microscopy identified magnetospheres with magnetite and maghemite from the Kingston coal ash as the magnetic carrier. Anthropogenic nonspherical magnetic particles are introduced from the industrialized Tennessee River watershed prior to reaching the Watts Bar Reservoir. A bivariate plot of anhysteretic remanent magnetization (ARM) versus mass-normalized low field magnetic susceptibility ( χ LF ) models the mixing of ash in the rivers, identifying both enrichment of magnetospheres by sorting near the spill and dilution with native sediment downstream. Concentration-dependent magnetic parameters in ash-bearing samples are approximately 2–56 times stronger than those of the ash-free watershed samples. This study supports the use of magnetic parameters to track the ash as it is eroded and transported 71 km downstream to the Watts Bar Dam and suggests that χ LF can be utilized to track the migration of coal ash in other river systems. [ABSTRACT FROM AUTHOR]

The Auroral Planetary Imaging and Spectroscopy (APIS) service, accessible online, provides an open and interactive access to processed auroral observations of the outer planets and their satellites. Such observations are of interest for a wide community at the interface between planetology, magnetospheric and heliospheric physics. APIS consists of (i) a high level database, built from planetary auroral observations acquired by the Hubble Space Telescope (HST) since 1997 with its mostly used Far-Ultraviolet spectro-imagers, (ii) a dedicated search interface aimed at browsing efficiently this database through relevant conditional search criteria and (iii) the ability to interactively work with the data online through plotting tools developed by the Virtual Observatory (VO) community, such as Aladin and Specview. This service is VO compliant and can therefore also been queried by external search tools of the VO community. The diversity of available data and the capability to sort them out by relevant physical criteria shall in particular facilitate statistical studies, on long-term scales and/or multi-instrumental multi-spectral combined analysis. [ABSTRACT FROM AUTHOR]

Nine magnetospheres samples were recovered by magnetic separation from fly ashes of typical coal-fired power plants in China and Russia, respectively. The physical-chemical characteristics of magnetospheres were investigated using particle size distribution instrument, BET surface area analyzer, physical property measurement system with vibrating sample magnetometer (PPMS-VSM), field emission scanning electron microscopy with energy-dispersive X-ray spectroscopy (FE-SEM-EDX), X-ray fluorescence (XRF), inductively coupled plasma mass spectrometry (ICP-MS), X-ray diffraction (XRD), and Mössbauer spectroscopy. The potential application and possible environmental concern of magnetospheres was also discussed. The results suggest that magnetospheres are superparamagnetism with a minimized coercivity and a negligible magnetization hysteresis. The iron species in magnetospheres mainly include Fe3O4, α-Fe2O3, γ-Fe2O3, Fe2+-silicate, Fe3+-silicate, and FeSi, while the content of each iron species are varied from different power plants. Magnetite (Fe3O4) is the dominant iron-bearing mineral, which governs the magnetic property of magnetospheres. The saturation magnetization of magnetospheres are proportion to their Fe3O4 content, and it can be described by the linear regression equations of [Ms]=−21.4+0.71 [Fe3O4] (R=0.89). The magnetism of magnetospheres are also determined by the quantity of elements substituted for Fe and their respective magnetic moments in the spinel structure. The siderophile elements (Cr, V, Co, Ni), chalcophile elements (Cu, Zn) and lithophile elements (In, U) are obviously enriched in magnetospheres. [ABSTRACT FROM AUTHOR]

To study the variations in the solar wind velocity during inferior conjunctions of Mercury and Earth, we analyzed 54 events in the period 1995-2012 by the superimposed epoch method. We have found a noticeable increase in the velocity both before and after the conjunctions as well as decrease in the velocity within 3-4 days after them (Mercury?s "shadow"). Variations of the solar wind density in 1997-2013 show a similar character, but their dispersion is substantially larger than for the velocity. The results obtained might be used to analyze variations and to improve a forecast of the solar wind velocity and density. [ABSTRACT FROM AUTHOR]

• Magnetospheres was modified through H 2 S as an efficient sorbent for Hg0. • Elemental sulfur derived from H 2 S oxidation was responsible high-efficient Hg0 adsorption. • Gaseous Hg0 was immobilized as stable HgS with extremely low leaching ratio. • The application route for Hg0 removal by using magnetospheres with suface sulfidation modification was proposed. Reduction of elemental mercury (Hg0) emission from coal-fired power plants is an enormous challenge. In this work, magnetospheres separated from fly ash was modified through H 2 S as an efficient sorbent (i.e., S-MS) for Hg0. Elemental sulfur with high affinity towards Hg0 was formed on the S-MS surface through selective catalytic oxidation of H 2 S. The sulfidation temperature played an important role in Hg0 adsorption over S-MS, ascribing to the variation of sulfur species on S-MS. The S-MS exhibited above 80% Hg0 adsorption efficiency with a sulfidation temperature of 150 °C for 30 min. The optimal Hg0 adsorption performance was obtained at 50 and 75 °C, implying that the S-MS could be adopted by injecting into the duct upstream of wet electrostatic precipitator (WESP) system. The gaseous Hg0 was immobilized by S-MS as stable mercury sulfide (HgS) owing to the presence of abundant sulfur species that is active for binding Hg0. The leaching ratio of mercury from spent S-MS in WESP effluent was as low as 1%, hence minimizing the secondary mercury pollution from the industrial waste. The cost analysis demonstrates that the mercury removal technology on the basis of magnetospheres adsorbents exhibited much superiority in operation cost compared with commercial activated carbon injection technology. Thus, the S-MS, with specific features, such as high Hg0 adsorption performance, minimized environmental hazardous and recyclability, displayed great potential in Hg0 sequestration. [ABSTRACT FROM AUTHOR]

Abstract: An estimated 229 000 m3 of coal fly ash remains in the river system after dredging to clean-up the 2008 Tennessee Valley Authority (TVA) spill in Kingston, Tennessee. The ash is heterogeneous with clear, orange and black spheres and non-spherical amorphous particles. Combustion produces iron oxides that allow low field magnetic susceptibility (χ LF) and percent frequency dependent susceptibility (χ FD%) to be used to discriminate between coal fly ash and sediments native to the watershed. Riverbed samples with χ LF greater than 3.0 × 10−6 m3/kg, have greater than 15% ash measured by optical point counting. χ LF is positively correlated with total ash, allowing ash detection in riverbed sediments and at depth in cores. The ratio of ash sphere composition is altered by river transport introducing variability in χ LF. Measurement of χ LF is inexpensive, non-destructive, and a reliable analytical tool for monitoring the fate of coal ash in this fluvial environment. [Copyright &y& Elsevier]

Abstract: We use the extensive database of magnetic observations from the Mars Global Surveyor to investigate magnetic disturbances in the Martian space environment statistically, both close to and far from crustal anomalies. We discuss the results in terms of possible ionospheric and magnetospheric currents, and use this to provide an estimate of the expected magnetic disturbances at the Martian surface. Far from crustal anomaly regions the expected magnetic disturbances originating from currents associated with the induced magnetosphere are very weak at the day-side, but most likely larger on the night-side. Close to crustal anomalies the expected surface perturbation is larger and more variable both in space and time. It is important to note that these variations are not confined to the intense crustal anomalies in the southern hemisphere, but occur in large parts of the equatorial region. The disturbances around medium intensity radial anomalies in the equatorial region appear to derive from local current loops or vortices around cusp-like radial fields, acting to partly cancel the crustal field. The radial perturbation is further found to depend on upstream solar wind dynamic pressure. We define a magnetic experiment at the martian surface, the Mars Surface Magnetic Observatory (MSMO) including the science objectives, science experiment requirements, instrument and basic operations. We find the experiment to be feasible within the constraints of proposed stationary landing platforms. [Copyright &y& Elsevier]

Abstract: The second and third flybys of Mercury by the MESSENGER spacecraft occurred, respectively, on 6 October 2008 and on 29 September 2009. In order to provide contextual information about the solar wind properties and the interplanetary magnetic field (IMF) near the planet at those times, we have used an empirical modeling technique combined with a numerical physics-based solar wind model. The Wang–Sheeley–Arge (WSA) method uses solar photospheric magnetic field observations (from Earth-based instruments) in order to estimate the inner heliospheric radial flow speed and radial magnetic field out to 21.5 solar radii from the Sun. This information is then used as input to the global numerical magnetohydrodynamic model, ENLIL, which calculates solar wind velocity, density, temperature, and magnetic field strength and polarity throughout the inner heliosphere. WSA-ENLIL calculations are presented for the several-week period encompassing the second and third flybys. This information, in conjunction with available MESSENGER data, aid in understanding the Mercury flyby observations and provide a basis for global magnetospheric modeling. We find that during both flybys, the solar wind conditions were very quiescent and would have provided only modest dynamic driving forces for Mercury''s magnetospheric system. [Copyright &y& Elsevier]

Abstract: In the solar system all planets that have significant magnetic fields also emit electron cyclotron radiation, usually near the auroral regions around the magnetic poles. In this study we use scaling laws based on solar system data to estimate the power and frequency of the auroral cyclotron emissions from interstellar planets (or sub-brown dwarfs). The emission can be powered either by motion of the planet through the interstellar plasma or by unipolar induction due to a moon. According to our results, in interstellar space the unipolar induction mechanism is potentially more effective than the motional emission mechanism. Typical emission power is around 1010–1012 W, but significantly stronger emissions are obtained in the most optimistic estimates. We have to conclude that detection of a rogue Jupiter would be very difficult, if not impossible with the radio telescopes available now or in the near future, but in very favorable conditions a much more massive and rapidly rotating (or otherwise strongly magnetized) gas giant with a large nearby moon could be detected up to pc distance with the square kilometer array. There may be a few thousand large enough interstellar planets this close to the solar system. For reference, we point out that according to previous studies some known hot Jupiters are expected to emit up to 1014–1016 W of cyclotron radiation, orders of magnitude more than the typical interstellar planets discussed here. However, these emissions have not yet been detected. [Copyright &y& Elsevier]

Abstract: On September 22, 2001 the Deep Space 1 spacecraft performed a flyby at comet 19P/Borrelly at a solar distance of 1.36AU leading the Earth by in longitude. The spacecraft–comet distance at closest approach was 2171km. The bow shock had a magnetic compression ratio of 2.5 at a distance of 147100km from the nucleus. Deep Space 1 first entered the sheath region essentially from the north polar region. Fluctuations from the cometary ion pickup were present throughout the sheath region and even well upstream of the shock, as expected. The magnetic field pileup region had a peak field strength of 83nT and was shown to be consistent with a pressure equal to the solar wind ram pressure. The peak field location was offset from the time of closest approach. It is uncertain whether this is a spatial or temporal variation. Draping of magnetic fields around the nucleus was sought, but evidence for this was not apparent in the data. A possible explanation is that the interplanetary solar wind was composed of turbulent short-scale fields, and thus the fields were not symmetric about the point of closest approach. During the flyby phase there were in general few intervals of ACE data where there were large scale Parker spiral fields. With the addition of plasma data, the shock properties are investigated. The characteristics of magnetic draping, pileup and fluctuations are explored. These comet 19P/Borrelly results are contrasted with other cometary flyby results. [Copyright &y& Elsevier]

Abstract: PAMELA is a satellite-borne experiment designed to make long duration measurements of the cosmic radiation in Low Earth Orbit. It is devoted to the detection of the cosmic-ray spectra in the 100MeV–300GeV range with primary scientific goal the measurement of antiproton and positron spectra over the largest energy range ever achieved. Other tasks include the search for antinuclei with unprecedented sensitivity and the measurement of the light nuclear component of cosmic rays. In addition, PAMELA can investigate phenomena connected with solar and Earth physics. The apparatus consists of: a Time of Flight system, a magnetic spectrometer, an electromagnetic imaging calorimeter, a shower tail catcher scintillator, a neutron detector and an anticoincidence system. In this work we present some measurements of galactic, secondary and trapped particles performed in the first months of operation. [Copyright &y& Elsevier]

Abstract: The relatively high contrast between planetary and solar low-frequency radio emissions suggests that the low-frequency radio range may be well adapted to the direct detection of exoplanets. We review the most significant properties of planetary radio emissions (auroral as well as satellite induced) and show that their primary engine is the interaction of a plasma flow with an obstacle in the presence of a strong magnetic field (of the flow or of the obstacle). Scaling laws have been derived from solar system planetary radio emissions that relate the emitted radio power to the power dissipated in the various corresponding flow–obstacle interactions. We generalize these scaling laws into a “radio-magnetic” scaling law that seems to relate output radio power to the magnetic energy flux convected on the obstacle, this obstacle being magnetized or unmagnetized. Extrapolating this scaling law to the case of exoplanets, we find that hot Jupiters may produce very intense radio emissions due to either magnetospheric interaction with a strong stellar wind or to unipolar interaction between the planet and a magnetic star (or strongly magnetized regions of the stellar surface). In the former case, similar to the magnetosphere–solar wind interactions in our solar system or to the Ganymede–Jupiter interaction, a hecto-decameter emission is expected in the vicinity of the planet with an intensity possibly 103–105 times that of Jupiter''s low frequency radio emissions. In the latter case, which is a giant analogy of the Io–Jupiter system, emission in the decameter-to-meter wavelength range near the footprints of the star''s magnetic field lines interacting with the planet may reach 106 times that of Jupiter (unless some “saturation” mechanism occurs). The system of HD179949, where a hot spot has been tentatively detected in visible light near the sub-planetary point, is discussed in some details. Radio detectability is addressed with present and future low-frequency radiotelescopes. Finally, we discuss the interests of direct radio detection, among which access to exoplanetary magnetic field measurements and comparative magnetospheric physics. [Copyright &y& Elsevier]

Abstract: Laboratory experiments using a plasma wind generated by laser-target interaction are developed to investigate the creation of a shock in front of the magnetosphere and the dynamo mechanism. Magnetic obstacles are placed in the plasma wind and measurements of the electron density gradients surrounding the obstacles are recorded. The experiments are analyzed with the methods used in theoretical simulation of the solar-wind-driven magnetosphere interactions. The proposed experiments are thought to be relevant to understanding the electron acceleration mechanisms at work in shock-driven magnetic dipole confined plasma surrounding compact magnetized stars and planets. Electron shock acceleration mechanisms are discussed in some detail. [Copyright &y& Elsevier]

Abstract: Saturn''s E ring is remarkable not only for its huge size. Based on optical measurements the ring was surprisingly found to mainly consist of ice particles of uniform size (radii between 0.3 and 2 microns) [Nicholson et al., 1996. Observations of Saturn''s ring-plane crossing in August and November. Science 272, 509–516], though the source of the ring, the icy moon Enceladus, feeds the ring with grains having a much broader mass distribution [Spahn et al., 1999. Dynamics of dust ejected from enceladus: application to the cassini dust detector. J. Geophys. Res. 104, 24111–24120]. Because of this contradiction, the mass distribution of the ring must be closely connected to the dynamics of the ring particles which is governed by the competition of various disturbing forces acting on the grains. It was realised early that the dynamics of the charged ring particles is strongly affected by electromagnetic forces as well as by plasma drag. Understanding the implications on the ring dynamics thus requires knowledge of the electrostatic equilibrium potential of the dust grains. The charge-sensitive grid system of the cosmic dust analyser (CDA) on the Cassini spacecraft allows an in situ determination of the charge of grains bigger than 2–3 microns. Since the CDA detector determines the grain mass simultaneously with the dust charge the electrostatic potential can be estimated as well. Here we report the first measurement of the electrostatic potential of E ring particles. Particles detected inside the orbit of Saturn''s moon Rhea were always found to be negatively charged, whereas grains outside Rhea''s orbit were on a positive potential of about 3V. Our results are in good agreement with measurements of the spacecraft potential by Cassini''s radio and plasma wave science (RPWS) investigation [Wahlund et al., 2005. The inner magnetosphere of Saturn: Cassini RPWS cold plasma results from the first encounter. Geophys. Res. Lett. 32]. Our analysis implies that the CDA dust analyser (DA) mass calibration by Göller and Grün [1998. Calibration of the Galileo/Ulysses dust detectors with different projectile materials and at varying impact angles. Planet. Space Sci. 37, 1197–1206] is applicable for ice particles. We achieved a good match between our findings and the model calculations of the grain potential when using new Cassini measurements of plasma properties within Saturn''s inner plasma sphere. Based on this we provide a realistic description for the grain potential needed for modelling the dynamics of Saturn''s E ring. [Copyright &y& Elsevier]

Abstract: The first comparative magnetospheres conference was held in Frascati, Italy thirty years ago this summer, less than half a year after the first spacecraft encounter with Jupiter’s magnetosphere (Formisano, V. (Ed.), The Magnetospheres of the Earth and Jupiter, Proceedings of the Neil Brice Memorial Symposium held in Frascati, Italy, May 28–June 1, 1974. D. Reidel Publishing Co., Boston, USA, 1975). Disputes highlighted various issues still being investigated, such as how plasma transport at Jupiter deviates from the prototypical form of transport at Earth and the role of substorms in Jupiter’s dynamics. Today there is a wealth of data on which to base the analysis, data gathered by seven missions that culminated with Galileo’s 8-year orbital tour. We are still debating how magnetic flux is returned to the inner magnetosphere following its outward transport by iogenic plasma. We are still uncertain about the nature of sporadic dynamical disturbances at Jupiter and their relation to terrestrial substorms. At Saturn, the centrifugal stresses are not effective in distorting the magnetic field, so in some ways the magnetosphere appears Earthlike. Yet the presence of plasma sources in the close-in equatorial magnetosphere parallels conditions at Jupiter. This suggests that we need to study both Jupiter and Earth when thinking about what to anticipate from Cassini’s exploration of Saturn’s magnetosphere. This paper addresses issues relevant to plasma transport and acceleration in all three magnetospheres. [Copyright &y& Elsevier]

Abstract: The deposition of energy, escape of atomic and molecular nitrogen and heating of the upper atmosphere of Titan are studied using a Direct Simulation Monte Carlo method. It is found that the globally averaged flux of deflected magnetospheric atomic nitrogen ions and molecular pickup ions deposit more energy in Titan''s upper atmosphere than solar radiation. The energy deposition in this region determines the atmospheric loss and the production of the nitrogen neutral torus. The temperature structure near the exobase is also calculated. It is found that, due to the inclusion of the molecular pickup ions more energy is deposited closer to the exobase than assumed in earlier plasma ion heating calculations. Although the temperature at the exobase is only a few degrees larger than it is at depth, the density above the exobase is enhanced by the incident plasma. [Copyright &y& Elsevier]

We review our present knowledge of plasma waves and non-thermal radio emissions at the outer planets. The review mainly concerns waves linked to electron dynamics. After a summary of the basics of radio and plasma wave modes as derived from the theory and from observations in the Earth''s vicinity, we discuss the counterpart of these waves as observed in outer planets'' magnetospheres. Plasma wave spectra display a remarkable overall similarity at all magnetized planets in spite of the very diverse magnetospheric configurations, emphasizing the importance of similar microphysics processes at all magnetized planets, in particular the outer giant planets. But the magnetospheres of the outer planets also give birth to a large diversity of radiosources, reflecting their complex structure (plasma reservoirs, gradients, regimes of fpe/fce, etc.) and dynamics (locations and distributions of energetic electrons). We discuss in more details these radio components, including their generation mechanisms. Emphasis is put on the direct generation of the very intense high latitude radio emissions, but conversion processes also occur in low latitude regions. The Earth stands as a reference in our comparative approach, but the study of radio and plasma waves at the outer planets allows to apply the concepts developed at Earth in different plasma environments, broadening the regime of plasma parameters involved in the generation of these waves. One specific Jovian radio component is identified (made of sporadic bursts), whose study could bring significant conceptual advances in the physics of the generation process involved. Finally, radio waves, because they can freely propagate far from their source regions, are of utmost importance as they allow for remote sensing of magnetospheric plasmas. [Copyright &y& Elsevier]

The MIMI CHEMS Instrument on the Cassini Orbiter detected Jovian pickup ions almost an AU upstream of Jupiter during the 2001 flyby. The clue to their planetary origin is the presence of singly ionized sulfur ions in quantities exceeding those expected from the interstellar gas entering the heliosphere (Nature 415 (2002) 994). Earlier modeling of the extended Jovian neutral gas disk suggested how the combination of the orbiting, localized Jovian source and interplanetary ionization processes should combine to produce a distinctive reservoir for heliospheric pickup ion production, different from its interstellar gas counterpart. Here the expected characteristics of pickup ions from the Jovian source are considered using a simplified model. The results provide an idea of the signatures in physical and phase space that reflect both the initial velocities and directionalities of the parent neutral population. Long-term measurements can easily test for these attributes given sufficient spatial and ion energy coverage. [Copyright &y& Elsevier]

The mercury removal performance of a low-cost recyclable CuCl 2 modified magnetospheres (Cu-MF) was investigated at a 50 MWth coal-fired power plant. An increase in the Cu-MF injection rate facilitated the mercury removal and recovery process. With the combination of the existing pollutant control devices and the Cu-MF injection, an overall mercury removal efficiency of 99.3% could be achieved. Under optimal conditions, the mercury emitted from the stack was reduced to 0.10 μg/m3. Most of the mercury in the flue gas migrated to the fly ash with the spent Cu-MF. Subsequently, through magnetic separation, 67.4% of the input mercury could be recovered. The comparison of experimental results showed that Cu-MF was more effective than fly ash in removing and recovering mercury from the flue gas. With the injection of Cu-MF, HgCl 2 was formed on the magnetospheres and was identified by the mercury-temperature-programmed decomposition (Hg-TPD) experiments. The magnetospheres with the lowest particle size showed the highest mercury removal capacity. This work is expected to provide valuable guidance for optimising the mercury removal technology in large scale commercial applications in future. [ABSTRACT FROM AUTHOR]