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Ingeo® PLA (polylactic acid) knitted fabric was scoured through an exhaust technique. The scouring was carried out with sodium carbonate in the presence of a detergent at various concentrations and temperatures. The scoured fabric was bleached with various oxidative bleaching agents. Bleaching was carried out with hydrogen peroxide, sodium chlorite and sodium hypochlorite. Hydrogen peroxide was applied by exhaust and cold pad batch (CPB) techniques. It was observed that during scouring PLA fabric was degraded at high alkali concentrations and processing temperatures. The scouring temperature above 60ºC proved to be deleterious due to the scouring solution penetrating into the polymer structure and damaged the fiber. Sodium chlorite and sodium hypochlorite caused little damage to the mechanical properties of PLA. Hydrogen peroxide when applied by the CPB technique did not reduce strength appreciably but when applied by the exhaust technique decreased the strength significantly. SEM analysis revealed that hydrogen peroxide caused holes and slit formation in the fiber structure.

Unambiguous knowledge of magnetic field structure and the electric current distribution is critical for understanding the origin, evolution, and related dynamic properties of magnetic flux ropes (MFRs). In this paper, a survey of 13 MFRs in the Earth's magnetotail are conducted by Cluster multipoint analysis, so that their force-free feature, i.e., the kind of magnetic field structure satisfying J x B = 0, can be probed directly. It is showed that the selected flux ropes with the bipolar signature of the south-north magnetic field component generally lie near the equatorial plane, as expected, and that the magnetic field gradient is rather weak near the axis center, where the curvature radius is large. The current density (up to several tens of nA/m(2)) reaches their maximum values as the center is approached. It is found that the stronger the current density, the smaller the angles between the magnetic field and current in MFRs. The direct observations show that only quasi force-free structure is observed, and it tends to appear in the low plasma beta regime (in agreement with the theoretic results). The quasi force-free region is generally found to be embedded in the central portion of the MFRs, where the current is approximately field aligned and proportional to the strength of core field. It is shown that similar to 60% of surveyed MFRs can be globally approximated as force free. The force-free factor a is found to be nonconstantly varied through the quasi force-free MFR, suggesting that the force-free structure is nonlinear.

Over the course of more than ten years in operation, the calibration parameters of the outboard fluxgate magnetometer (FGM) sensors on the four Cluster spacecraft are shown to be remarkably stable. The parameters are refined on the ground during the rigorous FGM calibration process performed for the Cluster Active Archive (CAA). Fluctuations in some parameters show some correlation with trends in the sensor temperature (orbit position). The parameters, particularly the offsets, of the Spacecraft1 (C1) sensor have undergone more long-term drift than those of the other spacecraft (C2, C3 and C4) sensors. Some potentially anomalous calibration parameters have been identified and will require further investigation in future. However, the observed long-term stability demonstrated in this initial study gives confidence in the relative accuracy of the Cluster magnetic field data. For the most sensitive ranges of the FGM instrument, the offset drift is typically 0.2 nT yr−1 in each sensor on C1 and negligible on C2, C3 and C4.

GKN is Britain's surviving top 50 company from 1905, a flourishing world top-player in automotive and aero components. This article traces 254 years of its development, domestically and internationally, drawing on corporate access and the author's worldwide field research since 1974, and three in-depth business histories including one by the co-author. Lessons confirm just some traits expected of successful ‘Built To Last’ (BTL) companies. However, GKN's ‘robust’ sustained strategy also reflects financial conservatism; constant adaptation to its historical and competitive context; highly proactive internationalisation and, from 1902 onwards, a determination to develop always at least ‘three major business legs’ to survive evolutionary processes as sectors mature and consolidate globally.

Magnetic disturbances caused by the Earth's ring current, particularly during storm time activity, have a dominant effect on the geomagnetic field. Strong currents and large kinetic and magnetic energies can change considerably local field geometry and depress the ground geomagnetic field. The multispacecraft magnetic measurements of Cluster allow extensive in situ coverage of the ring current. We select 48 storm time Cluster crossing events to investigate the variation of the local current density distribution and magnetic configuration of the ring current. We find direct evidence for the existence of an inner, eastward flowing current in addition to the dominant westward current, in the ring plane. The radius of curvature of the magnetic field lines (MFLs) is found to be increasingly reduced at all local times during increasing storm activity, changing the resulting ring current magnetic geometry considerably, where the MFL configuration and the azimuthal current density distribution are asymmetric with the local time. During similar storm activity the radius of curvature of the local MFLs, R-c, is smallest on the nightside to duskside, medium on the dawnside, and largest on the dayside. This change in geometry may have significant influence on the spatial distribution of the particles with various energies in the plasmasphere, ring current, and radiation belts.

Colouration of poly (lactic acid) textile materials using pigments is particularly interesting because of the commercial importance of pigment prints and the sensitivity of poly (lactic acid) fibres to aqueous treatment; however the processing requires optimisation because of the fibre's heat sensitivity. In this study, poly (lactic acid) fabrics were screen pigment printed and thermally cured at different temperatures, ranging from 120 °C to 150 °C, and curing times, from 3 min to 5 min. Surface sensitive X-ray Photoelectron Spectroscopy (XPS) was used to probe the nature of the outer 1–10 nm of the untreated and heat treated poly (lactic acid) surfaces, in order to characterise the surface functionalities and elemental composition. In addition, the effect of curing temperature and time on the performance characteristics of pigment printed poly (lactic acid) fabrics in terms of colour fastness, burst strength, abrasion resistance, Kawabata Evaluation System for Fabrics (KES-F) parameters and surface morphology were evaluated and optimum curing conditions for the pigment printing of poly (lactic acid) fabrics were established.

Dimethylol dihydroxyethylene urea (DMDHEU)-treated cotton fabrics were treated with alkali or alternatively acid followed by alkali for increasing time periods, and their effectiveness in removing the crosslinking agent was investigated by surface (X-ray photoelectron spectroscopy) analysis, bulk analysis, crease recovery angle performance and solubility in specific solvents. The cellulose yield after the chemical stripping processes was established and the effect of the acid and alkali treatments on the degree of polymerisation of the resultant cellulose determined. Surface and bulk analyses and solubility tests suggested that alkali alone could not remove the DMDHEU from the crease-resist-treated cotton fabric. However, a sequential acid/alkali treatment effectively removed the easy-care finish from the cotton fabric and produced a commercially viable yield of cellulose.

Magnetic-field measurements are essential to the success of many scientific space missions. Outside of the earth's magnetic field the biggest potential source of magnetic-field contamination of these measurements is emitted by the spacecraft. Spacecraft magnetic cleanliness is enforced through the application of strict ground verification requirements for spacecraft equipment and instruments. Due to increasingly strict AC magnetic-field requirements, many spacecraft units cannot be verified on the ground using existing techniques. These measurements must instead be taken close to the equipment under test (EUT) and then extrapolated. A traditional dipole power law of −3 (with a field fall-off proportional to r−3) cannot be applied at these close distances without risk of underestimating the field emitted by the EUT, but we demonstrate that a power law of −2 is too conservative. We propose a compromise that uses a power law of −2 up to a distance equal to 3 times the unit size, beyond which a dipole power law can be applied. When extrapolating from a distance of 0.20 m to 1.00 m from the centre of a 0.20 m wide EUT, we demonstrate that this method avoids an under prediction of the field, and is at least twice as accurate as performing the extrapolation with a fixed power law of −2.

The fine magnetic field structure of two successive plasmoids previously reported is investigated by magnetic rotation analysis using four Cluster satellite data. Between these two plasmoids, opposite trends of curvature radius (R-c) variations of the magnetic field lines from the boundary to the inner part are found. The different variations of R-c reflect that the two plasmoids have different magnetic configurations. The electric current density distributions for both plasmoids are found distinct. The B-y increase and abundant field-aligned currents in the narrow core region of the first plasmoid indicate that a possible magnetic flux rope (MFR) core exists inside. The results indicate that the first observed plasmoid is of a magnetic loop (ML) type (with possible MFR core) and the second plasmoid is of a magnetic flux rope (MFR) type. The coexistence of ML and MFR in the near-Earth plasma sheet may imply that multiple X line reconnection can occur by either an antiparallel or a component-parallel way.

The Performance of nano TiO2 with citric acid cross-linker was assessed by using pad-dry-cure method on cotton fabric. Significant increase in crease recovery performance was observed which was previously only associated with the lengthy ultraviolet irradiation process. The optimum amount of only 0.1 % nano TiO2 was needed with the citric acid to exhibit significant increase in easy care performance of the fabric. Typically, application of a cross-linker to cellulosics will impart a deleterious effect on the softness of the fabric; however, incorporation of nano-TiO2 with the citric acid cross-linker significantly improved the softness of the fabric which was reflected in the mean deviation of coefficient of friction (MMD) and interyarn friction (2HG5) KES-F values. In addition, there was improvement in tensile strength retention of the fabric as well.

Melt centrifugal spinning has been used to successfully produce nanofibres from compounds of polypropylene (PP) and multi-walled carbon nanotubes (MWNTs) at a concentration of 1%. The compounds were prepared either via twin screw compounding or by dissolution in decalin with sonication. Nanofibre production was conducted by centrifugal spinning in a Forcespinner™, a technology capable of producing nanofibres with a high material throughput. Processing via dissolution resulted in a reduction in the size of the MWNT agglomerations in the polymer, which led to a more uniform fibre morphology and a reduced incidence of bead defects as compared to products produced from the melt extrusion compound. The addition of a nonionic surfactant (Triton X-100) to the compound solution aided dispersion of the MWNTs as determined by optical light microscopy of thin cast films and produced fibres with the lowest mean diameter. The mean fibre diameter in the as-spun webs prepared by dissolution of PP in decalin with sonication was found to decrease with increasing spinneret speed; however, a similar trend was not observed for fibres generated from the melt compounded material.

The performance of the fluorocarbon based acrylate polymer, Genguard, was evaluated on cotton fabric. Genguard treated fabric exhibited good oil and water repellency rating before washing. However, rating was lost immediately after washing. In order to enhance the washing durability of the Genguard finish, citric acid was incorporated into the recipe as a formaldehyde free cross-linker. The combination of citric acid with fluorocarbon exhibited good improvement in the durability of the oil and water repellency rating after multiple washings. In addition, fabric treated with this novel combination demonstrated excellent increase in the easy care performance. Scanning electron microscope (SEM) was used to examine the surface of the fabric treated with Genguard and citric acid as a cross-linker.

Context. Strong electron cooling on the neutral gas in cometary comae has been predicted for a long time, but actual measurements of low electron temperature are scarce. Aims. Our aim is to demonstrate the existence of cold electrons in the inner coma of comet 67P/Churyumov-Gerasimenko and show filamentation of this plasma. Methods. In situ measurements of plasma density, electron temperature and spacecraft potential were carried out by the Rosetta Langmuir probe instrument, LAP. We also performed analytical modelling of the expanding two-temperature electron gas. Results. LAP data acquired within a few hundred km from the nucleus are dominated by a warm component with electron temperature typically 5–10 eV at all heliocentric distances covered (1.25 to 3.83 AU). A cold component, with temperature no higher than about 0.1 eV, appears in the data as short (few to few tens of seconds) pulses of high probe current, indicating local enhancement of plasma density as well as a decrease in electron temperature. These pulses first appeared around 3 AU and were seen for longer periods close to perihelion. The general pattern of pulse appearance follows that of neutral gas and plasma density. We have not identified any periods with only cold electrons present. The electron flux to Rosetta was always dominated by higher energies, driving the spacecraft potential to order − 10 V. Conclusions. The warm (5–10 eV) electron population observed throughout the mission is interpreted as electrons retaining the energy they obtained when released in the ionisation process. The sometimes observed cold populations with electron temperatures below 0.1 eV verify collisional cooling in the coma. The cold electrons were only observed together with the warm population. The general appearance of the cold population appears to be consistent with a Haser-like model, implicitly supporting also the coupling of ions to the neutral gas. The expanding cold plasma is unstable, forming filaments that we observe as pulses.

International audience; The plasma environment has been measured for the first time near the surface of a comet. This unique data set has been acquired at 67P/Churyumov–Gerasimenko during ESA/Rosetta spacecraft's final descent on 2016 September 30. The heliocentric distance was 3.8 au and the comet was weakly outgassing. Electron density was continuously measured with Rosetta Plasma Consortium (RPC)–Mutual Impedance Probe (MIP) and RPC–LAngmuir Probe (LAP) during the descent from a cometocentric distance of 20 km down to the surface. Data set from both instruments have been cross-calibrated for redundancy and accuracy. To analyse this data set, we have developed a model driven by Rosetta Orbiter Spectrometer for Ion and Neutral Analysis–COmetary Pressure Sensor total neutral density. The two ionization sources considered are solar extreme ultraviolet radiation and energetic electrons. The latter are estimated from the RPC–Ion and Electron Sensor (IES) and corrected for the spacecraft potential probed by RPC–LAP. We have compared the results of the model to the electron densities measured by RPC–MIP and RPC–LAP at the location of the spacecraft. We find good agreement between observed and modelled electron densities. The energetic electrons have access to the surface of the nucleus and contribute as the main ionization source. As predicted, the measurements exhibit a peak in the ionospheric density close to the surface. The location and magnitude of the peak are estimated analytically. The measured ionospheric densities cannot be explained with a constant outflow velocity model. The use of a neutral model with an expanding outflow is critical to explain the plasma observations.

International audience; The ESA's comet chaser Rosetta has monitored the evolution of the ionized atmosphere of comet 67P/Churyumov–Gerasimenko (67P/CG) and its interaction with the solar wind, during more than 2 yr. Around perihelion, while the cometary outgassing rate was highest, Rosetta crossed hundreds of unmagnetized regions, but did not seem to have crossed a large-scale diamagnetic cavity as anticipated. Using in situ Rosetta observations, we characterize the structure of the unmagnetized plasma found around comet 67P/CG. Plasma density measurements from RPC-MIP are analysed in the unmagnetized regions identified with RPC-MAG. The plasma observations are discussed in the context of the cometary escaping neutral atmosphere , observed by ROSINA/COPS. The plasma density in the different diamagnetic regions crossed by Rosetta ranges from ∼100 to ∼1500 cm −3. They exhibit a remarkably systematic behaviour that essentially depends on the comet activity and the cometary ionosphere expansion. An effective total ionization frequency is obtained from in situ observations during the high outgassing activity phase of comet 67P/CG. Although several diamagnetic regions have been crossed over a large range of distances to the comet nucleus (from 50 to 400 km) and to the Sun (1.25–2.4 au), in situ observations give strong evidence for a single diamagnetic region, located close to the electron exobase. Moreover, the observations are consistent with an unstable contact surface that can locally extend up to about 10 times the electron exobase.

International audience; The long duration of the Rosetta mission allows us to study the evolution of the diamagnetic cavity at comet 67P/Churyumov–Gerasimenko in detail. From 2015 April to 2016 February 665 intervals could be identified where Rosetta was located in a zero-magnetic-field region. We study the temporal and spatial distribution of this cavity and its boundary and conclude that the cavity properties depend on the long-term trend of the outgassing rate, but do not respond to transient events at the spacecraft location, such as outbursts or high neutral densities. Using an empirical model of the outgassing rate, we find a functional relationship between the outgassing rate and the distance of the cavity to the nucleus. There is also no indication that this unexpectedly large distance is related to unusual solar wind conditions. Because the deduced shape of the cavity boundary is roughly elliptical on small scales and the distances of the boundary from the nucleus are much larger than expected we conclude that the events observed by Rosetta are due to a moving instability of the cavity boundary itself.

Negative ion time of flight secondary ion mass spectrometry (ToF-SIMS) analysis of rigorously cleaned untreated, hydroxylamine and potassium hydroxide (KOH)-treated wool fabrics, produced with minimal finishing, has revealed the possible presence of hitherto unidentified bound acids at the surface of the wool fibre. Spectral peaks have been assigned to C8 through to C22 fatty acids, the odd numbered acids of which have been assigned to anteiso acids, (a), akin to the anteiso acid 18-methyleicosanoic acid known to be the dominant fatty acid bound to keratin fibre surfaces. This has included the assignment of some small peaks to hydroxylated aC18H36(OH)COS− and aC20H40(OH)COS− species, where the hydroxyl group is attached to the asymmetric 16 or 18 numbered carbon atom in the alkyl chain, respectively. The study has confirmed that many of the acids are bound to the fibre surface by thioester linkages (about 70%) and that the remainder is bound by oxygen ester acyl linkages. ToF-SIMS analysis of hydroxylamin...

The colour resulting from the laundering of cotton fabric is influenced by the nature of the dye, the detergent formulation and the physical structure of the fibre surface. In this study the effect of ISO (International Organisation for Standardization) 105 CO6 and ISO 105 CO9 wash fastness testing, with and without oxidant, and with and without stainless steel abrasive balls, on the colour of C.I. Sulphur Black 1 dyed cotton fabric was evaluated. The surface sensitive X-ray Photoelectron Spectroscopy (XPS) was used to probe the nature of the outer 3–10 nm of the cotton surface, characterise the surface functionalities and elemental composition and establish the durability of the surface dye to different washing regimes. In addition the effect of laundering and modification to the surface sulphur dye was related to colour through K / S and L * analysis.

Polyvinylpyrrolidone/1-triacontene (PVP/TA) copolymer fibre webs produced by centrifugal melt spinning were studied to determine the influence of jet rotation speed on morphology and internal structure as well as their potential utility as adsorbent capture media for disperse dye effluents. Fibres were produced at 72 C with jet head rotation speeds from 7000 to 15,000 r min-1. The fibres were characterised by means of SEM, XRD and DSC. Adsorption behaviour was investigated by means of an isothermal bottle point adsorption study using a commercial disperse dye, Dianix AC-E. Through centrifugal spinning nanofibers and microfibers could be produced with individual fibres as fine as 200–300 nm and mean fibre diameters of ca. 1–2 lm. The PVP/TA fibres were mechanically brittle with characteristic brittle tensile fracture regions observed at the fibre ends. DSC and XRD analyses suggested that this brittleness was linked to the graft chain crystallisation where the PVP/TA was in the form of a radial brush copolymer. In this structure, the triacontene branches interlock and form small lateral crystals around an amorphous backbone. As an adsorbent, the PVP/TA fibres were found to adsorb 35.4 mg g-1 compared to a benchmark figure of 30.0 mg g-1 for a granular-activated carbon adsorbent under the same application conditions. PVP/TA is highly hydrophobic and adsorbs disperse dyes through the strong ‘‘hydrophobic bonding’’ interaction. Such fibrous assemblies may have applications in the targeted adsorption and separation of non-polar species from aqueous or polar environments.

International audience; Turbulence Heating ObserveR (THOR) is a spacecraft mission dedicated to the study of plasma turbulence in near-Earth space. The mission is currently under study for implementation as a part of ESA Cosmic Vision program. THOR will involve a single spinning spacecraft equipped with state of the art instruments capable of sensitive measurements of electromagnetic fields and plasma particles. The sensitive electric and magnetic field measurements require that the spacecraft- generated emissions are restricted and strictly controlled; therefore a comprehensive EMC program has been put in place already during the study phase. The THOR study team and a dedicated EMC working group are formulating the mission EMC requirements already in the earliest phase of the project to avoid later delays and cost increases related to EMC. This article introduces the THOR mission and reviews the current state of its EMC requirements.

The common law remains one of the most important legacies we Americans received from our shared history and roots with England, and a birthright our citizens share with those of the United Kingdom. Not only did the common law serve as the model for our own jurisprudence, but generations of American lawyers, including many of our founding fathers, early presidents, and most eminent early jurists, were trained on Lord Coke's Commentary on Littleton and Report/ and understood and embraced Lord Coke's admonition to let not cases be committed

In-situ magnetic field measurements are of critical importance in understanding how the Sun creates and controls the heliosphere. To ensure the measurements are accurate, it is necessary to track the combined slowly-varying spacecraft magnetic field and magnetometer zero offset – the systematic error in the sensor measurements. For a 3-axis stabilised spacecraft, in-flight correction of zero offsets primarily relies on the use of Alfvénic rotations in the magnetic field. We present a method to automatically determine a key parameter related to the ambient compressional variance of the signal (which determines the selection criteria for identifying clear Alfvénic rotations). We apply our method to different solar wind conditions, performing a statistical analysis of the data periods required to achieve a 70% chance of calculating an offset using Helios datasets. We find that 70% of 40 min data periods in regions of fast solar wind possess sufficient rotational content to calculate an offset. To achieve the same 70% calculation probability in regions of slow solar wind requires data periods of 2 h duration. We also find that 40 min data periods at perihelion compared to 1 h and 40 min data periods at aphelion are required to achieve the same 70% calculation probability. We compare our method with previous work that uses a fixed parameter approach and demonstrate an improvement in the calculation probability of up to 10% at aphelion and 5% at perihelion.

On July 10, 2010, the ROSETTA spacecraft performed a flyby at asteroid (21)Lutetia at a solar distance of 2.72 AU. The spacecraft–asteroid distance at closest approach was 3120 km. The magnetometers onboard ROSETTA were operating but did not detect any conclusive signature of the asteroid. Any magnetic field signature which could possibly be attributed to the asteroid was below 1 nT. Consequently an upper limit for the global magnetic properties of asteroid (21)Lutetia could be derived: maximum dipole moment ≤ 1.0 × 10 12 A m 2 , global maximum magnetization ≤ 2.1 × 10 − 3 A / m , specific moment ≤ 5.9 × 10 − 7 A m 2 / kg . Draping of magnetic fields around the nucleus was sought, but evidence for this could not be clearly identified in the data. Plasma simulations taking into account the estimated upper limit of the magnetization and possible outgassing revealed interesting structures very close to the asteroid. The results obtained at Lutetia are contrasted with the results of other asteroid flyby results.

The ROSETTA mission to comet 67P/Churyumov-Gerasimenko presents us for the first time the opportunity to study the interior of a cometary nucleus. Information about the electrical conductivity and its distribution inside the nucleus can be derived by measuring the magnetic fields induced in the nucleus by variations of the interplanetary magnetic field. Due to the relatively small size of the nucleus, this task is not trivial and requires very precise magnetic field measurements. Here we analyze the response of a conductive nucleus to transient step-like magnetic field changes as well as the response in frequency domain to electromagnetic waves. For the nucleus we use a spherical model with either uniform conductivity or consisting of a core and an outer layer with different conductivities. The space outside of the nucleus is modeled either by highly conductive solar wind plasma or by zero conductivity void. Various combinations of conductivities, radii of the nucleus and of the core, and properties of the space outside the nucleus result in different inductive responses. Several such combinations which could be encountered by ROSETTA are studied in detail in order to estimate which conductivity ranges and core radii can be determined using the ROSETTA instruments and which mission operations would facilitate such measurements.

AXIOM (Advanced X-ray Imaging Of the Magnetosphere) is a concept mission which aims to explain how the Earth's magnetosphere responds to the changing impact of the solar wind using a unique method never attempted before; performing wide-field soft X-ray imaging and spectroscopy of the magnetosheath. magnetopause and bow shock at high spatial and temporal resolution. Global imaging of these regions is possible because of the solar wind charge exchange (SWCX) process which produces elevated soft X-ray emission from the interaction of high charge-state solar wind ions with primarily neutral hydrogen in the Earth's exosphere and near-interplanetary space.

The wash durability of the easy care finish Dimethylol Dihydroxyethylene Urea (DMDHEU) on cotton fabric under ISO 105 CO6 and CO9 test conditions and extended domestic laundering conditions was investigated by surface and bulk sensitive techniques, in particular X-ray photoelectron spectroscopy, elemental analysis and crease recovery angle performance. The presence of the finish was detected at the fibre surface through the N (1 s) photoelectron signal and saturation of the fibre surface with finish was demonstrated. The stability of the DMDHEU to ISO 105 CO6 and ISO 105 CO9 washing and domestic laundering was investigated and the durability of the DMDHEU finish on cotton demonstrated. The type of cross-linking between the DMDHEU and the cellulosic polymer chains was studied and related to the crease recovery performance. The implications for recycling of the treated fibre via fibre regeneration are discussed.

On 10th July 2010 the Rosetta spacecraft passed within 3160 km of asteroid 21 Lutetia during which seven instruments attempted to detect an exosphere. A comparison of the sensitivity is made between the different instruments based on a simple spherical out gassing point source model which was used to infer that the Lutetia exosphere production rate was determined by MIRO to be

The emergence of countries such as China and India and the general trend towards economic opening has led to announcements of global strategic intent by virtually all of the major companies in recent years (Grosse, 2005). However, a primary consideration in focusing specifically on the cross-border activities of banks emanated from the sheer size of their international activities. For example, a cursory examination of foreign assets as a percentage of total assets of the 30 largest banks reveals that they increased from 35 per cent in 1980 to over 38 per cent by 2003 (De Nicolo et al., 2004). Moreover, the absolute size of the foreign assets of these same banks increased 11-fold from $650 billion in 1990 to over $7,571 billion in 2000 (Slager, 2005). Prior to the credit crunch, the global banking sector was estimated to have had a market value in excess of $65,700 billion in 2005 (Datamonitor, 2006).

Planetary plasma and magnetic field environments can be studied by in situ measurements or by remote sensing. While the former provide precise information about plasma behaviour, instabilities and dynamics on local scales, the latter offers the global view necessary to understand the overall interaction of the magnetospheric plasma with the solar wind. Here we propose a novel and more elegant approach employing remote X-ray imaging techniques, which are now possible thanks to the relatively recent discovery of solar wind charge exchange X-ray emissions in the vicinity of the Earth's magnetosphere. We describe how an appropriately designed and located X-ray telescope, supported by simultaneous in situ measurements of the solar wind, can be used to image the dayside magnetosphere, magnetosheath and bow shock, with a temporal and spatial resolution sufficient to address several key outstanding questions concerning how the solar wind interacts with the Earth's magnetosphere on a global level. Our studies have led us to propose 'AXIOM: Advanced X-ray Imaging Of the Magnetosphere', a concept mission using a Vega launcher with a LISA Pathfinder-type Propulsion Module to place the spacecraft in a Lissajous orbit around the Earth - Moon L1 point. The model payload consists of an X-ray Wide Field Imager and an in situ plasma and magnetic field measurement package. This package comprises sensors designed to measure the bulk properties of the solar wind and to characterise its minor ion populations which cause charge exchange emission, and a magnetometer designed to measure the strength and direction of the solar wind magnetic field. We show simulations that demonstrate how the proposed X-ray telescope design is capable of imaging the predicted emission from the dayside magnetosphere with the sensitivity and cadence required to achieve the science goals of the mission., Published in Experimental Astronomy, Springer (40 pages, 14 figures, 5 tables). Updated version re-submitted to arXiv on 1 August 2011 (with corrected figure numbering and improved versions of Fig.s 4, 7, 10, 11); http://www.springerlink.com/openurl.asp?genre=article&id=doi:10.1007/s10686-011-9239-0 (published on-line, July 2011)

The comfort of textiles is important and one area under evaluation is the development and application of Phase Change Materials, PCMs, in order to impart thermal adaptability. PCMs research for textiles has also focused on the use of polyethylene glycol (PEG). While there is a good adhesion between fibre and PEG polymer for cotton and polyester fibres, polymer adhesion to wool fibres appears poor and loosely bound within the yarn and had dislodged and crumbled. Therefore in this paper, the effect of changing the wool fibre surface energy and surface charge, shrinkproofing, on performance properties of thermally adaptable wool fabrics were studied. Untreated, gaseous fluorinated, as well as Chlorine-Hercosett treated 100 % wool fabrics have been evaluated to obtain highly cross-linked PEG with acceptable fastness properties. The surface interface was effectively probed by XPS & ToF-SIMS and characterised the loss of surface lipids, the nature of the fibre oxidation and deposition of Hercosett polymer on the wool fibre. The results indicate the necessity of having high surface energy in order to obtain appropriate adhesion and binding higher amount of solid polymer to wool fibres which results in superior thermal activity, better durability, and enhancement in felting performance.

This project investigated whether a strategy framework such as the Balanced Scorecard (BSC), linked to a Performance Management System (PMS), would, compared to a more standard model of strategic planning, improve focus and research output by botanic gardens worldwide. The focus of the project shifted as the opportunity arose to develop an objective costing system linked to the related PMS, which allowed the researchers to posit that the BSC framework could provide a more effective contribution to governance. The research output was based on an in-depth case study at the Royal Botanic Garden Edinburgh employing documentary analysis and innovative action research techniques adopting a constructive approach. This paper has been adapted for Sibbaldia having previously been published by the Chartered Institute of Management Accountants (CIMA) Research Project R220 (Macnab et al., 2010).

This paper proposes a contextual approach to explaining differences in strategic investment decision (SID) making practices First, a systematic contextual framework is developed from the existing research literature Then this framework's potential for explaining differences in SID making practices is explored through 14 case studies of U K,US and Japanese companies from both stable and dynamic business sectors Our findings suggest substantial SID differences across our four contextual categories of market creators, value creators. refocusers and restructurers The differences relate to the emphasis on strategic versus financial considerations, the thoroughness and rigidity of financial analysis, the attitudes towards incorporating less easily quantifiable factors and the level of hurdle rates (C) 2010 Elsevier Ltd All rights reserved.

Sixty-five of the world’s largest family firms were compared against with those of a matched sample of 65 non-family firms. Contrary to previous studies, family firms here displayed higher profitability and a broadly positive (if slightly inconsistent) relationship between increasing family ownership levels and performance. Sales growth was also consistently higher over 20 years when averaged worldwide. Since other studies have mainly been restricted to single countries or regions, we further analysed differences across continents and country cultures. Within both North America and Europe family and non-family firms were equally profitable (though family firms grew relatively faster in North America). The same was true for ‘high-trust’ countries and also for Anglo-Saxon regions. However, in low-trust countries and also in more long-termist Asian countries, family firms performed better than non-family firms both in terms of profitability and sales growth.

The past few decades have seen a tremendous growth in work patterns that involve social actors from different cultural backgrounds interacting with one another, as shown by the increase in number and forms of international staff (Collings et al., 2007) or the rise in the formation of international joint ventures (Pothukuchi et al., 2002). Even actors whose scope of activity is limited to a domestic context are likely to be exposed to foreign cultures as they collaborate with coworkers, partners, suppliers and clients from different ethnic and cultural origins. Although research at the interface between the domestic and international context is still relatively scarce, for example as illustrated by the limited attention that local nationals have received in international assignment research (Toh and DeNisi, 2007; Vance and Ring, 1994), scholars widely agree that culture transcends and thus forms an integral part of many aspects in business. One stream of research has explored the multiple layers that constitute culture and that differ in terms of their degree of tangibility and visibility, distinguishing between observable artifacts and behaviors, deeper-level values and basic assumptions (e.g. Schein, 1992). In this vein, existing cross-cultural research has mainly conceptualized culture as a system of shared, underlying values that explain (Hofstede, 1980; Schwartz, 1994) but may also potentially vary from (House et al., 2004) behavioral practices. Another debate has centered on the multiple levels at which culture has been conceptualized to operate (Chao, 2000; Leung et al., 2005). It has been common to consider a hierarchy of levels in which lower levels are nested within higher levels, for example an individual working in a team that forms part of an organization that, in turn, operates in a specific national market. However, these scholars increasingly also point to the cross-level effects that occur when changes at one cultural level influence and reshape other levels. Although the resulting implications are highly relevant to the understanding of cultural phenomena at large, levels issues in cross-cultural research have thus far focused mainly on the different levels at which national culture influences behavioral outcomes, broadly distinguishing between individual, group, and organization-level effects. In this respect, national culture has been shown to have both direct and moderated effects on a wide range of individual and interpersonal attitudes, cognitions and behaviors (Tsui et al., 2007), impact on team processes (Gelfand et al., 2007) and influence various organizational systems, structures and practices, including capital International Journal of Cross Cultural Management 10(2) 131–136 a The Author(s) 2010 Reprints and permissions: sagepub.co.uk/journalsPermissions.nav DOI: 10.1177/1470595810376429 ccm.sagepub.com CCM International Journal of Cross Cultural Management

On day 7 May 2005, the plasma instruments on board Double Star TC1 and Cluster SC3 spacecraft register inside the magnetosheath, at 19:15:12 and 19:16:20 UT, respectively, a strong pressure pulse due to the impact of an interplanetary shock wave (IS) on the terrestrial bow shock. The analysis of this event provides clear and quantitative evidences confirming and strengthening some results given by past simulations and observational studies. In fact, here we show that the transmitted shock is slowed down with respect to the incident IS (in the Earth's reference frame) and that, besides the transmitted shock, the IS – bow shock interaction generates a second discontinuity. Moreover, supported also by a special set three-dimensional magnetohydrodynamic simulation, we discuss, as further effects of the interaction of the IS with the magnetosphere, other two interesting aspects of the present event, that is: the TC1 double crossing of the bow shock (observed few minutes after the impact of the IS) and the presence, only in the SC3 data, of a third discontinuity produced inside the magnetosheath.

The Mercury magnetospheric orbiter (MMO) of the Japanese–European BepiColombo mission carries a dual-sensor magnetometer, MMO/MGF. The sensors are of the classical fluxgate type mounted on a boom. For redundancy, each sensor carries its own electronics and is connected to a different data processing unit. MMO/MGF can sample the magnetic field at a rate of up to 128 Hz. The resulting comparatively high time resolution of the magnetic field measurements, i.e., down to 8 ms, will be necessary when studying the dynamics of and processes within the Hermean magnetosphere, since the Mariner 10 observations have shown that their typical time scales are much shorter than in the Earth's magnetosphere, by about a factor of 30. The high time resolution will also be very useful for studying the evolution of the still young solar wind plasma as well as interplanetary shocks at 0.3–0.46 AU. Of course, MMO/MGF is also well-prepared to assist the sister magnetometer aboard the Mercury planetary orbiter, MPO/MAG, in measuring Mercury's intrinsic magnetic field, in particular by helping to distinguish between temporal fluctuations and spatial variations.

Many variables have been studied, rather inconclusively, to determine behavioural differences of family firms and any impact on performance. This article focuses on just one under-researched variable: their international strategic choices or rather ‘configurations’. We compare 65 of the world’s top family firms with those of a matched sample of non-family firms. Results suggest that family firms’ ‘international ‘configurations’ were just as worldwide and profitable as those pursued by non-family firms. In the case of such large companies, researchers must consider this international dimension alongside other more acknowledged variables, if they are to advance understanding in this important emerging new field.

The physical and mechanical characteristics of hollow polyester fibres were compared with solid polyester fibres in order to establish their processing behaviour and performance characteristics. The effects of hollow fibres on fabric properties were investigated by using microscopy and tests of tensile and bursting strength, pilling, abrasion resistance, water vapour permeability, and handle. The results show that tensile strength of hollow polyester fibres and yarns are negatively affected by the cavity inside the fibre. Hollow fibres also have higher stiffness and resistance to bending at relaxed state. Fabrics made from hollow polyester/wool blends and pure wool fabrics show three distinguishable steps in pilling. During pilling, hollow fibres break before being pulled fully out of the structure, leading to shorter protruding fibres. Microscopy studies showed that the breakdown of hollow fibres started during entanglement by splitting along the helical lines between fibrils. KES results showed that the friction between fibres and the fibre shape are the most important parameters that determine the fabric low stress mechanical properties. However, in some aspects, the hollow structure of the fibre does not have a significant effect.

We present the first two-spacecraft near-simultaneous observations of the Martian bow shock (BS), magnetic pileup boundary (MPB) and photo-electron boundary (PEB) obtained by the plasma instruments onboard Rosetta and Mars Express during the Rosetta Mars flyby on February 25, 2007. Our observations are compared with shape models for the BS and MPB derived from previous statistical studies. The MPB is found at its expected position but the BS for this event is found significantly closer to the planet than expected for the rather slow and moderately dense solar wind. Cross-calibration of the density measurements on the two spacecraft gives a density profile through the magnetosheath, indicating an increasing solar wind flux during the Rosetta passage which is consistent with the multiple BS crossings at the Rosetta exit.

The interaction and the durability to laundering of a cationic β-cyclodextrin derivative applied to Tencel were examined by x-ray photoelectron spectroscopy (XPS). The N1(s) XPS spectra of the cationic β-cyclodextrin treated substrates revealed the presence of the applied finish on the fibre surface and that the durability of the applied finish to hand-wash was good. However, the cationic β-cyclodextrin derivative showed poor durability to the ISO CO6/C2S wash protocol. Copyright © 2009 John Wiley & Sons, Ltd.

The effect of sulfamic acid and urea treat- ments on the flame retardant properties of soybean fabric has been investigated by Limiting Oxygen Index (L.O.I.), Thermogravimetric Analysis (TGA), and X-ray Photoelec- tron Spectroscopy (XPS) in order to characterize both the bulk and surface properties. The sulfamic acid finish sig- nificantly reduced the soybean fabric flammability and appeared to function in the solid phase with increased char formation. Incorporation of urea into the formulation increased the level of reaction and associated weight gain. However, the wash durability of the sulfamic acid modifi- cation of the soybean fabric was limited, but after treat- ment with a cationic fixing agent, Matexil FC-ER signifi- cantly increased the wash fastness and related flame re- tardant effect. XPS analysis demonstrated the substantivity of the cationic fixing agent to soybean fiber surface and its binding effect on the sulfamate at the fiber surface. 2008 Wiley Periodicals, Inc. J Appl Polym Sci 109: 3590-3595, 2008

The equatorial and polar satellites of the Double Star Project (DSP) were launched successfully on December 29, 2003 and July 25, 2004, respectively, and both of them are operating smoothly. The DSP provides a good opportunity for investigating the structure of the magnetosphere. Based on the DSP data collected during 2004, we have surveyed the distribution of the magnetic fields and plasmas in the magnetosphere. It is found that: (1) Near the Earth’s equatorial plane within geocentric distances of less than 7 RE, the Earth’s magnetic field is dipolar. In the vicinity of the magnetopause, the magnetic field is enhanced by a factor of about 1.5, and on the nightside, the magnetic field can vary significantly from the Earth’s dipole field, likely caused by the presence of the near-Earth tail current sheet. (2) In the day-side magnetosheath, the electron and ion densities are usually both in the range of 10–30 cm−3; the ion and electron temperatures are usually about 200 and 50 eV, respectively. The flow pattern is usually smooth, with a low velocity in the subsolar region and with significantly higher velocities in the dawn and dusk flanks. (3) In the region between the magnetopause and plasmasphere the density is low, approximately 0.5–5 cm−3, and the temperature is high, about 1–10 keV for ions and 0.1–5 keV for electrons. The ion temperature has an apparent anisotropy, with the ratio of the perpendicular and parallel temperatures being about 1.0–1.3 for the night-and dusk-side magnetosphere and about 1.3–2.0 for the day-and dawn-side magnetosphere. There is an evident sunward convection of about 50 km/s in the magnetosphere. On the dawn side, the flow becomes somewhat turbulent, and in the vicinity of the night-noon meridian plane, the convection is rather slow. (4) The high-energy electrons with energies higher than 2 MeV are mainly located in the regions with 3 < L < 4.5; the size of the high-energy electrons area varies with time, it may expand and shrink occasionally according to different solar wind conditions and magnetic activities.

During the interval 06:14–07:30 UT on August 24, 2005, since the Earth’s magnetopause was suddenly compressed by the persistent high-speed solar wind stream with the southward component of the interplanetary magnetic field (IMF), the magnetopause moved inward for about 3.1 RE. Meanwhile, TC-1 satellite shifted from northern plasma sheet to the northern lobe/mantle region, although it kept inward flying during the interval 06:00–07:30UT. The shift of TC-1 from the plasma sheet to the lobe/mantle is caused by the simultaneous inward displacements of the plasma sheet and near-Earth lobe/mantle region, and their inward movement velocity is larger than the inward motion velocity of TC-1. The joint inward displacements of the magnetopause, the lobe/mantle region and the plasma sheet indicate that the whole magnetosphere shrinks inward due to the magnetospheric compression by the high-speed solar wind stream, and the magnetospheric ions are attached to the magnetic field lines (i.e. ‘frozen’ in magnetic field) and move inward in the shrinking process of magnetosphere. The large shrinkage of magnetosphere indicates that the near-Earth magnetotail compression caused by the strong solar wind dynamic pressure is much larger than its thickening caused by the southward component of the IMF, and the locations of magnetospheric regions with different plasmas vary remarkably with the variation of the solar wind dynamic pressure.

An event of Cluster-Double Star conjunction observations of magnetic reconnection at high latitude magnetopause nightside of both cusps and solar wind transport into magnetosphere caused by such reconnection process has been investigated. During northward IMF, Cluster/SC1 observed accelerated flows and ion heating associated with magnetic reconnection at high latitude magnetopause nightside of southern cusp. And Double Star observed cold dense solar wind plasma transported into dayside magnetosphere. The analysis on such conjunction observations shows that: (1) during northward IMF, magnetic reconnection occurs at high latitude nightside of southern cusp, accompanied by accelerated flows that are observed by Cluster/SC1; (2) the direction of the accelerated flows, with its sunward component Vx, dawnward component Vy, northward component Vz, is quite consistent with the theoretical anticipation under the condition of northward IMF with dawnward component By; (3) reconnection can heat plasma more in parallel direction than in perpendicular direction, to a level of about 4 keV; (4) with reconnection taking place at high latitude magnetopause nightside of the southern cusp, TC-1 observed cold and dense plasma transported into magnetosphere; (5) by reconnection at high latitude magnetopause nightside of both cusps, solar wind flux tube can be captured by magnetosphere and pulled into dayside magnetosphere. This event presents further observational evidence for magnetic reconnection at high latitude magnetopause nightside of both cusps as an important mechanism of solar wind transport into magnetosphere.

With the 4-s resolution data of the magnetometer and the ion plasma analyzer on TC-1 from June to November of each year during the period of 2004-2006, we statistically analyzed the occurrence rate of both convective and field-aligned bursty flows (FABFs). A near-Earth bursty bulk flow (NEBBF) occurred during both the quiet time and substorm process. In general, the magnetic field and the plasma density began oscillating with the appearance of the NEBBF associated with a distinct increase of the AE index. The increase of AE index during the NEBBF was more than 100 nT in both quiet time and substorm process. The statistical analysis indicated that the occurrence rates of the FABFs were nearly the same in the different stages of the AE index, but the occurrence rate of the NEBBFs was much higher in the growth stage of the AE index, indicating that the NEBBFs were directly related to the growth and expansion phases of the substorm. The observations suggested that the quite large number of BBFs from the mid magnetotail could enter into the near-Earth tail and play important role in triggering the substorm onset.

Based on measurements of FGM and HIA on board TC-1 at its apogee on September 14, 2004, we analyzed the ion high-speed flows in the near-Earth plasma sheet observed during the substorm expansion phase. Strong tailward high-speed flows (Vx ∼ −350 km/s) were first seen at about X ∼ −13.2 RE in near-Earth magnetotail, one minute later the flows reversed from tailward to earthward. The reversal process occurred quickly after the substorm expansion onset. The near-Earth magnetotail plasma sheet was one of key regions for substorm onset. Our analysis showed that the ion flow reversal from tailward to earthward was likely to be in close relation with the substorm expansion initiation and might play an important role in triggering the substorm expansion onset.

From June 1, 2004 to October 31, 2006, a total 465 high-speed flow events are observed by the TC-1 satellite in the near-Earth region (−13 RE < x < −9 RE, |Y