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Cysteine S–H bonds have a spectroscopically convenient stretching frequency of ∼2550 cm−1. However, their cross section is low, and the band can be strongly broadened in heterogeneous environments, making detection very challenging. With two-dimensional infrared (2D-IR) setups achieving ever higher sensitivities in recent years, systematic use of the weak cysteine sulfhydryls (Cys–SHs) absorption band is now within reach, even at low millimolar protein concentrations. Here, we demonstrate the capabilities of Cys–SH as an intrinsic 2D-IR label in pyruvate oxidase from E. coli, an enzyme with ten cysteines in its native sequence. 1D-IR measurements on the wild-type and individual cysteine knock-out variants show that two such residues have especially narrow SH signatures, caused by their intrahelical hydrogen bonding. 2D-IR analysis of these bands reveals an extraordinarily high anharmonicity (∼110 cm−1) and a long vibrational lifetime (∼4 ps). This allows monitoring spectral diffusion via center line slope analysis for up to 10 ps—separately for both the ground and excited states. The unique spectroscopic features and its ease of introduction make Cys–SH a useful IR spectroscopic label.

Despite a developing understanding of how landscape level processes moderate biodiversity patterns and ecosystem functioning, key questions remain unresolved, therefore limiting our ability to manage for biodiversity conservation and ecosystem functioning at the most appropriate scales. These questions have remained unanswered because studies in agricultural landscapes generally over-emphasize alpha diversity within managed land uses, and are focused at scales that are irrelevant to species studied. We argue that the key to resolving unanswered questions in landscape-moderated effects on biodiversity and ecosystem functioning lies in establishing the distribution of available species and functions across the landscape and between land uses, and in understanding how this distribution of species varies with changing landscape context. We emphasize the need for studies that empirically test the mechanisms underpinning landscape-moderated effects on biodiversity and ecosystem function and link these with ecosystem service delivery. We facilitate this approach by outlining the empirical investigations that will lead to a better understanding of biodiversity patterns and ecosystem functioning at the landscape scale, and we highlight statistical approaches to support these different approaches to sampling. Our paper is divided in four sections: (A) we identify where and why gaps exist in our mechanistic understanding of landscape level processes, by reviewing current hypotheses; (B) we outline why, and how, landscape level research would benefit from shifting the focus to the distribution and partitioning of species and functions within a landscape; (C) we outline why, and how, larger scale processes, such as dispersal and meta-population dynamics need to be addressed in a more interactive fashion; and finally, (D) we round out by highlighting the experimental settings where landscape effects most urgently need testing.

Coronagraphs observe coronal mass ejections (CMEs) and driven shocks in white light images.From these observations the shocks speed and the shocks standoff distance from the CMEs leading edge can be derived. Using these quantities, theoretical relationships between the shocks Alfvenic Mach number MA and standoff distance, and empirical radial profiles for the solar wind velocity and number density, the radial magnetic field profile upstream of the shock can be calculated. These profiles cannot be measured directly. We test the accuracy of this method for estimating the radial magnetic field profile upstream of the shock by simulating a sample CME that occurred on 29 November 2013 using the three-dimensional (3-D) magnetohydrodynamic Block-Adaptive-Tree-Solar wind-Roe-Upwind-Scheme code, retrieving shock-CME standoff distances from the simulation, and comparing the estimated and simulated radial magnetic field profiles. We find good agreement between the two profiles (within +/-30%) between 1.8 and 10R.Our simulations confirm that a linear relationship exists between the standoff distance and the inverse compression ratio at the shock. We also find very good agreement between the empirical and simulated radial profiles of the number density and speed of the solar wind and inner corona.

Coronal mass ejections (CMEs) are major transient phenomena in the solar corona that are observed with ground-based and spacecraft-based coronagraphs in white light or with in situ measurements by spacecraft. CMEs transport mass and momentum and often drive shocks. In order to derive the CME and shock trajectories with high precision, we apply the graduated cylindrical shell (GCS) model to fit a flux rope to the CME directed toward STEREO A after about 19:00 UT on 29 November 2013 and check the quality of the heliocentric distance-time evaluations by carrying out a three-dimensional magnetohydrodynamic (MHD) simulation of the same CME with the Block Adaptive Tree Solar-Wind Roe Upwind Scheme (BATS-R-US) code. Heliocentric distances of the CME and shock leading edges are determined from the simulated white light images and magnetic field strength data. We find very good agreement between the predicted and observed heliocentric distances, showing that the GCS model and the BATS-R-US simulation approach work very well and are consistent. In order to assess the validity of CME and shock identification criteria in coronagraph images, we also compute synthetic white light images of the CME and shock. We find that the outer edge of a cloud-like illuminated area in the observed and predicted images in fact coincides with the leading edge of the CME flux rope and that the outer edge of a faint illuminated band in front of the CME leading edge coincides with the CME-driven shock front.

Coronal mass ejections (CMEs) are frequently associated with shocks and type II solar radio bursts. Despite involving fundamental plasma physics and being the archetype for collective radio emission from shocks, type II bursts have resisted detailed explanation for over 60 years. Between 29 November and 1 December 2013 the two widely separated spacecraft STEREO A and B observed a long lasting, intermittent, type II radio burst from ≈4 MHz to 30 kHz (harmonic), including an intensification when the CME-driven shock reached STEREO A. We demonstrate the first accurate and quantitative simulation of a type II burst from the high corona (near 11 solar radii) to 1 AU for this event with a combination of a data-driven three-dimensional magnetohydrodynamic simulation for the CME and plasma background and an analytic quantitative kinetic model for the radio emission.

Type II solar radio bursts are often indicators for impending space weather events at Earth. They are consequences of shock waves driven by coronal mass ejections (CMEs) that move outward from the Sun. We simulate such type II radio bursts by combining elaborate three-dimensional (3-D) magnetohydrodynamic (MHD) predictions of realistic CMEs near the Sun with an analytic kinetic radiation theory developed recently. The simulation approach includes the reconstruction of initial solar magnetic fields, the dimensioning of the initial flux rope of the CME with STEREO spacecraft data, and the launch of the CME into an empirical data-driven corona and solar wind. In this paper, we simulate a complicated double CME event (a very fast CME followed by a slower CME without interaction) and the related coronal and interplanetary type II radio bursts that occurred on 7 March 2012. We extend our previous work to show harmonic and interplanetary emission as well as the simulation's surprising ability (for these events at least) for predicting emission for two closely spaced CMEs leaving the same active region. We demonstrate that the theory predicts well the observed fundamental and harmonic emission from ∼20 MHz to 50 kHz or from the high corona to near 1 AU. Specifically, the theory predicts flux, frequency, and time variations that are consistent with the presence or absence of observed type II emissions when interfering emissions are absent and are not inconsistent with observations when interfering type III bursts are present. The predicted and observed type II emission is predominantly fundamental for these two events. Harmonic emission occurs for the second CME only for a short time interval, when an extended shock has developed that can drive flank emission. The coronal and interplanetary emission follow closely hyperbolic lines in frequency-time space, consisting of a succession of islands of emission with varying intensity. The islands develop due to competition between the shock moving through varying coronal and solar wind magnetic field structures (e.g., loops and streamers), growth of the driven radio source due to the spherical expansion of the shock, and movement of the active radio sources from the shock's nose to its flanks.

Impending space weather events at Earth are often signaled by type II solar radio bursts. These bursts are generated upstream of shock waves driven by coronal mass ejections (CMEs) that move away from the Sun. We combine elaborate three-dimensional (3-D) magnetohydrodynamic predictions of realistic CMEs near the Sun with a recent analytic kinetic radiation theory in order to simulate two type II bursts. Magnetograms of the Sun are used to reconstruct initial solar magnetic and active region fields for the modeling. STEREO spacecraft data are used to dimension the flux rope of the initial CME, launched into an empirical data-driven corona and solar wind. We demonstrate impressive accuracy in time, frequency, and intensity for the two type II bursts observed by the Wind spacecraft on 15 February 2011 and 7 March 2012. Propagation of the simulated CME-driven shocks through coronal plasmas containing preexisting density and magnetic field structures that stem from the coronal setup and CME initiation closely reproduce the isolated islands of type II emission observed. These islands form because of a competition between the growth of the radio source due to spherical expansion and a fragmentation of the radio source due to increasingly radial fields in the nose region of the shock and interactions with streamers in the flank regions of the shock. Our study provides strong support for this theory for type II bursts and implies that the physical processes involved are understood. It also supports a near-term capability to predict and track these events for space weather predictions.

Non-Maxwellian electron distributions are observed widely throughout the solar system and are often well described as kappa distributions. This chapter addresses the importance of kappa distributions to the growth and damping of plasma waves (specifically Langmuir waves), the reflection of electrons from shocks, the evolution of electron beams, and the generation of type II and III solar radio bursts. Kappa distributions extend to much higher speeds and have many more fast particles than Maxwellians. Accordingly, kappa distributions lead to a much larger spontaneous emission of plasma waves and radio emissions produced by incoherent processes. Similarly, shocks that accelerate the background electrons have much higher numbers of fast electrons upstream for kappa-distributed electrons than for Maxwellian electrons, leading to stronger electron beams and stronger Langmuir waves and radio emissions. This is demonstrated theoretically for type II solar radio bursts. The extension of kappa distributions to larger speeds than for Maxwellian distributions leads to larger damping rates for electron beam-generated Langmuir waves. It also limits the relaxation of the beam to higher speeds and reduces energy transfers to the Langmuir waves and any radio emissions generated therefrom. These effects are demonstrated theoretically for type III solar radio bursts, allowing us to understand why kappa distributions for the background electrons lead naturally to faster beams with speeds of ≳0.5c and to the type III bursts being weaker, having faster frequency drift rates, and starting at lower frequencies for smaller values of the kappa index, κ.

Objectives To determine if proteinuria is more common in dogs with lymphoma when compared with healthy dogs and to assess the severity and frequency of proteinuria in dogs with lymphoma. Methods Determination of urine protein:creatinine ratio in 32 dogs with lymphoma compared with 30 healthy dogs. Results Canine patients with lymphoma are more likely to be proteinuric compared with healthy dogs. Proteinuria is common in dogs with lymphoma, although in most cases it is not severe. The presence of proteinuria is not linked with the stage or substage of lymphoma. Clinical Significance Mild proteinuria is a common finding in dogs with lymphoma. The clinical impact of the proteinuria is probably low.

Little information is available on the occurrence of neoplasms in dogs up to the age of 12 months. This is a retrospective review of histopathological diagnoses of neoplasia in dogs up to the age of 12 months based on biopsy specimens submitted to a commercial veterinary diagnostic laboratory in the United Kingdom between 1993 and 2008. In 20 280 histological submissions, 9522 neoplasms were identified. Canine cutaneous histiocytoma (n = 8465; 89%) was the most common histological type. Neoplasms other than histiocytoma (n = 1057; 11%) were grouped as benign epithelial (n = 375; 4%), haematopoietic (n = 229; 2%), benign mesenchymal (n = 145; 2%), miscellaneous (n = 118; 1%), non-hematopoietic malignant mesenchymal (n = 118; 1%) or malignant epithelial tumours (n = 72

Objectives: To determine which types of tumour occur in cats up to the age of 12 months based on biopsies submitted to Idexx Laboratories, Wetherby, UK. Methods: Retrospective review of histopathological diagnoses of tumours in cats up to the age of 12 months from biopsies received between September 1993 and March 2008. Results: A total of 4196 submissions from cats 12 months old or younger were identified; 233 biopsies (6%) were neoplastic and fulfilled the search criteria. Tumours were categorised as haematopoietic (n=73, 31%), malignant epithelial (n=44; 19%), malignant mesenchymal (n=38; 16%), benign epithelial (n=37; 16%), benign mesenchymal (n=30, 13%) and miscellaneous (n=11; 5%). The most frequent tumours were lymphoma (n=51; 22%), soft-tissue sarcoma (n=34; 15%), mast cell tumour (n=22; 9%) and squamous cell carcinoma (n=16; 7%). The most common tumour site was the skin and soft tissues (41% of tumours). In all, 164 neoplasms (70%) were malignant or had malignant potential. Clinical Significance: These data provide unique epidemiological information on a poorly characterised subgroup of feline cancer patients in the UK.

We use the observation of an Extreme Ultraviolet Imaging Telescope (EIT) wave in the lower solar corona, seen with the two Solar Terrestrial Relations Observatory (STEREO) spacecraft in extreme ultraviolet light on 2007 May 19, to model the same event with a three-dimensional (3D) time-depending magnetohydrodynamic (MHD) code that includes solar coronal magnetic fields derived with Wilcox Solar Observatory magnetogram data, and a solar wind outflow accelerated with empirical heating functions. The model includes a coronal mass ejection (CME) of Gibson and Low flux rope type above the reconstructed active region with parameters adapted from observations to excite the EIT wave. We trace the EIT wave running as circular velocity enhancement around the launching site of the CME in the direction tangential to the sphere produced by the wave front, and compute the phase velocities of the wave front. We find that the phase velocities are in good agreement with theoretical values for a fast magnetosonic wave, derived with the physical parameters of the model, and with observed phase speeds of an incident EIT wave reflected by a coronal hole and running at about the same location. We also produce in our 3D MHD model the observed reflection of the EIT wave at the coronal hole boundary, triggered by the magnetic pressure difference between the wave front hitting the hole and the boundary magnetic fields of the coronal hole, and the response of the coronal hole, which leads to the generation of secondary reflected EIT waves radiating away in different directions than the incident EIT wave. This is the first 3D MHD model of an EIT wave triggered by a CME that includes realistic solar magnetic field, with results comparing favorably to STEREO Extreme Ultraviolet Imager observations.

Snapping hip (Coxa saltans) is the abrupt sliding of the iliotibial tract over the greater trochanter. In the case of pain, which cannot be alleviated by a conservative treatment, an operation is advised. The methods of operation applied up to this day showed--especially because of their high recidive-quotas--great disadvantages. In a detailed post-operational check-up over the past 20 years the new method of "diagonal notching" (27 cases) developed at the Orthopedic Hospital Munchen-Harlaching was compared to the old method of fixing the tract according to M. Lange (24 cases). After "diagonal notching" the snapping occurred again seven times less than after fixing the tract. After "diagonal notching" only 4% of the patients had to be re-operated, however, after fixing the tract a re-operation was necessary on 38% of the patients. 91% of the patients were relieved from their pain almost completely after "diagonal notching", compared to only 50% after fixing the tract. Considering that the "diagonal notching" offers simple technics of operation and better results than other methods, the "diagonal notching" should be used as method of choice to eliminate a snapping hip.

Between 29 November and 1 December 2013 the two widely separated spacecraft STEREO A and B observed a long lasting, intermittent, type II radio burst for the extended frequency range ≈ 4 MHz to 30 kHz, including an intensification when the shock wave of the associated coronal mass ejection (CME) reached STEREO A. We demonstrate for the first time our ability to quantitatively and accurately simulate the fundamental (F) and harmonic (H) emission of type II bursts from the higher corona (near 11 solar radii) to 1 AU. Our modeling requires the combination of data-driven three-dimensional magnetohydrodynamic simulations for the CME and plasma background, carried out with the BATS-R-US code, with an analytic quantitative kinetic model for both F and H radio emission, including the electron reflection at the shock, growth of Langmuir waves and radio waves, and the radiations propagation to an arbitrary observer. The intensities and frequencies of the observed radio emissions vary hugely by factors ≈ 106 and ≈ 103, respectively; the theoretical predictions are impressively accurate, being typically in error by less than a factor of 10 and 20 %, for both STEREO A and B. We also obtain accurate predictions for the timing and characteristics of the shock and local radio onsets at STEREO A, the lack of such onsets at STEREO B, and the z-component of the magnetic field at STEREO A ahead of the shock, and in the sheath. Very strong support is provided by these multiple agreements for the theory, the efficacy of the BATS-R-US code, and the vision of using type IIs and associated data-theory iterations to predict whether a CME will impact Earth’s magnetosphere and drive space weather events.

Objective: To identify risk factors for refractory fever after subarachnoid hemorrhage (SAH), and to determine the impact of temperature elevation on outcome.Methods: We studied a consecutive cohort of 353 patients with SAH with a maximum daily temperature (Tmax) recorded on at least 7 days between SAH days 0 and 10. Fever (>38.3 °C) was routinely treated with acetaminophen and conventional water-circulating cooling blankets. We calculated daily Tmax above 37.0 °C, and defined extreme Tmax as daily excess above 38.3 °C. Global outcome at 90 days was evaluated with the modified Rankin Scale (mRS), instrumental activities of daily living (IADLs) with the Lawton scale, and cognitive functioning with the Telephone Interview of Cognitive Status. Mixed-effects models were used to identify predictors of Tmax, and logistic regression models to evaluate the impact of Tmax on outcome.Results: Average daily Tmax was 1.15 °C (range 0.04 to 2.74 °C). The strongest predictors of fever were poor Hunt-Hess grade and intraventricular hemorrhage (IVH) (both p < 0.001). After controlling for baseline outcome predictors, daily Tmax was associated with an increased risk of death or severe disability (mRS ≥ 4, adjusted OR 3.0 per °C, 95% CI 1.6 to 5.8), loss of independence in IADLs (OR 2.6, 95% CI 1.2 to 5.6), and cognitive impairment (OR 2.5, 95% CI 1.2 to 5.1, all p ≤ 0.02). These associations were even stronger when extreme Tmax was analyzed.Conclusion: Treatment-refractory fever during the first 10 days after subarachnoid hemorrhage (SAH) is predicted by poor clinical grade and intraventricular hemorrhage, and is associated with increased mortality and more functional disability and cognitive impairment among survivors. Clinical trials are needed to evaluate the impact of prophylactic fever control on outcome after SAH.

This report assesses the current status of research relating the origin at the Sun, the evolution through the inner heliosphere and the effects on the inner heliosphere of the interplanetary counterparts of coronal mass ejections (ICMEs). The signatures of ICMEs measured by in-situ spacecraft are determined both by the physical processes associated with their origin in the low corona, as observed by space-borne coronagraphs, and by the physical processes occurring as the ICMEs propagate out through the inner heliosphere, interacting with the ambient solar wind. The solar and in-situ observations are discussed as are efforts to model the evolution of ICMEs from the Sun out to 1 AU.

This chapter provides an overview of current efforts in the theory and modeling of CMEs. Five key areas are discussed: (1) CME initiation; (2) CME evolution and propagation; (3) the structure of interplanetary CMEs derived from flux rope modeling; (4) CME shock formation in the inner corona; and (5) particle acceleration and transport at CME driven shocks. In the section on CME initiation three contemporary models are highlighted. Two of these focus on how energy stored in the coronal magnetic field can be released violently to drive CMEs. The third model assumes that CMEs can be directly driven by currents from below the photosphere. CMEs evolve considerably as they expand from the magnetically dominated lower corona into the advectively dominated solar wind. The section on evolution and propagation presents two approaches to the problem. One is primarily analytical and focuses on the key physical processes involved. The other is primarily numerical and illustrates the complexity of possible interactions between the CME and the ambient medium. The section on flux rope fitting reviews the accuracy and reliability of various methods. The section on shock formation considers the effect of the rapid decrease in the magnetic field and plasma density with height. Finally, in the section on particle acceleration and transport, some recent developments in the theory of diffusive particle acceleration at CME shocks are discussed. These include efforts to combine self-consistently the process of particle acceleration in the vicinity of the shock with the subsequent escape and transport of particles to distant regions.

Het doel van het onderzoek was het klinische beloop van overspanning en verschillende klachten die de toestand van overspanning kenmerken, te beschrijven. Dit werd gedaan door middel van een longitudinaal, observationeel onderzoek bij patienten die vanwege de ernst of complexiteit van werkgerelateerde overspanningsklachten zijn verwezen voor gespecialiseerde psychotherapeutische behandeling. De mate van overspanning, comorbiditeit, ziekteverzuim, therapeutische en demografische kenmerken zijn gemeten met gevalideerde vragenlijsten op vier momenten: voor, na, en 3 en 9 maanden na afronding van de behandeling. Op basis van de Overspanningsklachtenlijst werd de gemiddelde Overspanningsscore berekend en werden de individuele klachten ingedeeld in cognitieve en emotionele klachten, en moeheid. Referentiewaarden voor overspanning (OS = 1,7 (SD 0,7)) en moeheid (2,7 (SD 1,1)) werden verzameld in een werkende populatie.

The interaction in the solar wind between two coronal mass ejections (CMEs) is investigated using numerical simulations. We show that the nature of the interaction depends on whether the CME magnetic structures interact, but in all cases the result is an equilisation of the speed of the two CMEs. In the absence of magnetic interaction, the forward shock of the faster trailing CME interacts with the slow leading CME, and accelerates it. When the two CMEs have magnetic fields with the same sense of rotation, magnetic reconnection occurs between the two CMEs, leading to the formation of a single magnetic structure: in the most extreme cases, one CME "eats" the other. When the senses of rotation are opposite, reconnection does not occur, but the CMEs collide in a highly non-elastic manner, again forming a single structure. The possibility of enhanced particle acceleration in such processes is assessed. The presence of strong magnetic reconnection provides excellent opportunities for the acceleration of thermal particles, which then form a seed population for further acceleration at the CME shocks. The presence of a large population of seed particles will thus lead to an overall increase in energetic particle fluxes, as suggested by some observations.

PEARLS  Hemodialysis (HD) has been associated with increases in intracranial pressure (ICP). Osmotic shifts occurring during HD are thought to be associated with the development of this phenomenon.  In comatose patients with acute brain injury, an elevation of ICP during HD may be associated with worse cerebral autoregulation. Continuous veno-venous hemofiltration (CVVH) may be a safer alternative in these patients. OYSTER  HD may increase ICP; therefore, caution should be exercised when HD is needed in patients with acute brain injury. CASE REPORT A 59-year-old man with hyperten

To analyze the impact of inflammation and negative nitrogen balance (NBAL) on nutritional status and outcomes after subarachnoid hemorrhage (SAH).This was a prospective observational study of SAH patients admitted between May 2008 and June 2012. Measurements of C-reactive protein (CRP), transthyretin (TTR), resting energy expenditure (REE), and NBAL (g/day) were performed over 4 preset time periods during the first 14 postbleed days (PBD) in addition to daily caloric intake. Factors associated with REE and NBAL were analyzed with multivariable linear regression. Hospital-acquired infections (HAI) were tracked daily for time-to-event analyses. Poor outcome at 3 months was defined as a modified Rankin Scale score ≥ 4 and assessed by multivariable logistic regression.There were 229 patients with an average age of 55 ± 15 years. Higher REE was associated with younger age (p = 0.02), male sex (p0.001), higher Hunt Hess grade (p = 0.001), and higher modified Fisher score (p = 0.01). Negative NBAL was associated with lower caloric intake (p0.001), higher body mass index (p0.001), aneurysm clipping (p = 0.03), and higher CRP:TTR ratio (p = 0.03). HAIs developed in 53 (23%) patients on mean PBD 8 ± 3. Older age (p = 0.002), higher Hunt Hess (p0.001), lower caloric intake (p = 0.001), and negative NBAL (p = 0.04) predicted time to first HAI. Poor outcome at 3 months was associated with higher Hunt Hess grade (p0.001), older age (p0.001), negative NBAL (p = 0.01), HAI (p = 0.03), higher CRP:TTR ratio (p = 0.04), higher body mass index (p = 0.03), and delayed cerebral ischemia (p = 0.04).Negative NBAL after SAH is influenced by inflammation and associated with an increased risk of HAI and poor outcome. Underfeeding and systemic inflammation are potential modifiable risk factors for negative NBAL and poor outcome after SAH.

The evolution of magnetic flux ropes in a sheared plasma flow is investigated. When the magnetic field outside the flux rope lies parallel to the axis of the flux rope, a flux rope of circular cross-section, whose centre is located at the midpoint of the shear layer, has its shape distorted, but remains in the shear layer. Small displacements of the flux-rope centre above or below the midpoint of the shear layer lead to the flux-rope being expelled from the shear layer. This motion arises because small asymmetries in the plasma pressure around the flux-rope boundary leads to a force that forces the flux rope into a region of uniform flow. When the magnetic field outside the flux rope lies in a plane perpendicular to the flux-rope axis, the flux rope and external magnetic field reconnect with each other, leading to the destruction of the flux rope.

Bioassay (P-388 lymphocytic leukemia cell line)-guided separation of an extract prepared from the bark and stem of the Sri Lankan tree Schleichera oleosa led to the isolation of seven cancer cell growth inhibitory hydroxylated sterols designated schleicherastatins 1-7 (1-7) and two related sterols, schleicheols 1 and 2 (8, 9). The structure of schleicherastatin 1 (1) was completely elucidated by X-ray crystal structure determination. Based upon that defined structure, the remaining new sterol structures were deduced by highfield (300 and 500 MHz) NMR and MS interpretations. In this new series of sterols, hydroxylation at C-22 appears to be important for promoting cancer cell growth inhibition.

Corotating interaction regions (CIRs) in the middle heliosphere have distinct morpholog- ical features and associated patterns of turbulence and energetic particles. This report summarizes current understanding of those features and patterns, discusses how they can vary from case to case and with distance from the Sun and possible causes of those variations, presents an analytical model of the morphological features found in earlier qualitative models and numerical simulations, and identifies aspects of the features and patterns that have yet to be resolved.

Corotating Interaction Regions (CIRs) form as a consequence of the compression of the solar wind at the interface between fast speed streams and slow streams. Dynamic interaction of solar wind streams is a general feature of the heliospheric medium; when the sources of the solar wind streams are relatively stable, the interaction regions form a pattern which corotates with the Sun. The regions of origin of the high speed solar wind streams have been clearly identified as the coronal holes with their open magnetic field structures. The origin of the slow speed solar wind is less clear; slow streams may well originate from a range of coronal configurations adjacent to, or above magnetically closed structures. This article addresses the coronal origin of the stable pattern of solar wind streams which leads to the formation of CIRs. In particular, coronal models based on photospheric measurements are reviewed; we also examine the observations of kinematic and compositional solar wind features at 1 AU, their appearance in the stream interfaces (SIs) of CIRs, and their relationship to the structure of the solar surface and the inner corona; finally we summarise the Helios observations in the inner heliosphere of CIRs and their precursors to give a link between the optical observations on their solar origin and the in-situ plasma observations at 1 AU after their formation. The most important question that remains to be answered concerning the solar origin of CIRs is related to the origin and morphology of the slow solar wind.

Termen zoals overspanning, surmenage, aanpassingsstoornis, burn-out of neurasthenie worden zowel in de literatuur als in het professionele spraakgebruik vaak als synoniemen gehanteerd. Hiermee wordt dan een syndroom van klachten bedoeld, dat kan voorkomen onder condities van chronische, psychosociale stress. De samenvattende en neutrale term ‘chronisch stresssyndroom’ – die overigens niet voorkomt in het psychiatrisch classificatiesysteem DSM-IV – zou, naar onze opvatting, een bruikbare pendant zijn voor de term ‘acuut stresssyndroom’, die er wel in voorkomt.

A variety of natural and artificial substrates were tested for their suitability as oviposition sites for the predatory anthocorid bug Orius insidiosus. The bugs oviposited into models of beans constructed from Parafilm, but none of the eggs laid into these models hatched. In choice tests, beans stems were preferred to both bean pods and potato sprouts. Hatching rates at 100% r.h. were highest (59%) for bean pods and significantly lower for both potato sprouts (39%) and bean stems (29%). At 60% r.h., hatching rates for bean pods (39%), bean stems (34%) and potato sprouts (33%) were similar. At 30% r.h. hatching rates for all three substrates were less than 15%. The results suggest that bean stems can be used successfully as an alternative to bean pods for the mass rearing of these biological control agents.

[1] Type II radio bursts drift in frequency as shock waves and coronal mass ejections (CMEs) move through the Sun's corona and the solar wind. This paper applies an extended analytic theoretical model for type II radio bursts to an MHD simulation of the rippled shock front found upstream of the flanks of a CME. The theory treats the acceleration of electrons at the shock, formation of electron beams, growth of Langmuir waves, and conversion of Langmuir energy into radiation. The extended theory is entirely analytic and includes kappa electron velocity distribution functions for the ambient plasma electrons and the shock-reflected electrons. It also includes the plateauing of the electron beam, which releases energy for the Langmuir waves. This paper presents and discusses our numerical results for synthetic radio source regions and synthetic dynamic spectra, gained by applying our radiation model to an MHD simulation of a shock driven by a CME. The investigation reveals strong emission upstream of the flanks of the shock. A complicated rippled shock geometry develops with embedded “ripples” that stimulate short-lived “bright spot” radio sources, which lead to complicated substructures in the dynamic spectrum, and more extended sources that usually have a weaker and more diffuse radio emission. The natural development of ripples on the shock provides a natural link between the ripple theory of Knock, Cairns, and colleagues and the bolt-on model presented here.

[1] Type II radio bursts drift in frequency as shock waves and coronal mass ejections (CMEs) move through the Sun's corona and the solar wind. This paper extends the theoretical models for type II radio bursts of Knock et al. (2001, 2003), Knock and Cairns (2005), Cairns and Knock (2006) and Schmidt and Gopalswamy (2008). The theory treats the acceleration of electrons at the shock, formation of electron beams, growth of Langmuir waves, and conversion of Langmuir energy into radiation. An entirely analytical and more general formalism is developed, which includes kappa electron velocity distribution functions for the plasma electrons and the shock-reflected electron beam. The radiation model also includes the plateauing of the electron beam, which releases energy for the Langmuir waves. This paper has two parts. First, the new entirely analytical formalism is presented. Second, first numerical results for synthetic radio images and synthetic dynamic spectra are discussed, gained by applying our radiation model to MHD simulations of a shock driven by a CME. The results are compared with earlier analytic approaches. This work is also applicable to other shock-related emissions in space and astrophysical plasmas.

Objective: Rebleeding of an aneurysm is a leading cause of morbidity and mortality after subarachnoid hemorrhage (SAH). Whereas numerous studies have demonstrated the risk factors associated with rebleeding, few data on complications of rebleeding, including its effect on the development of delayed cerebral ischemia (DCI), are available. Methods: A nested case-control study was performed on patients with rebleeding and control subjects matched for modified Fisher scale, Hunt-Hess grade, age, and sex previously entered into a prospective database. Rebleeding was defined as new hemorrhage apparent on repeat CT with or without new symptoms. Incidence and time course of DCI and hospital complications were compared. A secondary analysis of DCI and hospital complications was also performed on subjects surviving to postbleed day 7. Results: We identified 120 patients with rebleeding and 359 control subjects from 1996 to 2011. The rebleeding rate was 8.6%. In both the primary and secondary analyses, there was no difference in the incidence of DCI or its time course (29% vs 27%, p = 0.6; 7 ± 5 vs 7 ± 6 days, p = 0.9 for primary analysis; 39% vs 31%, p = 0.1, 7 ± 5 vs 7 ± 6 days, p = 0.6 for the secondary analysis). In a multivariate logistic regression model, rebleeding was associated with the complications of hyponatremia, respiratory failure, and hydrocephalus. Patients with rebleeding had higher rates of mortality, brain death, and poor outcomes. Conclusions: Rebleeding after SAH is associated with multiple medical and neurologic complications, resulting in higher morbidity and mortality, but is not associated with change of incidence or timing of DCI.

A pulse sequence is presented that extends the E.COSY concept to homonuclear relayed COSY experiments for the accurate measurement of homonuclear long-range J coupling constants. The method is applied to the measurement of coupling constants between HN and side-chain protons in proteins.

This study intends to develop a physiologic thumbprint for nonconvulsive seizures (NCSz) after acute brain injury. Abnormal electrographic brain activity including NCSz is common after acute brain injury and is associated with poor outcome. Mechanisms underlying this phenomenon are poorly understood but in animals periods of inadequate perfusion during seizures have been documented. In the present study we hope to gain better understanding of the relationship between abnormal electrographic patterns and brain homeostasis in patients with subarachnoid hemorrhage (SAH).

The concept of self-consistent J coupling evaluation exploits redundant structure information inherent in large sets of 3J coupling constants. Application to the protein Desulfovibrio vulgaris flavodoxin demonstrates the simultaneous refinement of torsion-angle values and related Karplus coefficients. The experimental basis includes quantitative coupling constants related to the polypeptide backbone φ torsion originating from a variety of heteronuclear 2D and 3D NMR correlation experiments, totalling 124 3J(HN,Hα), 129 3J(HN,C'), 121 3J(HN,Cβ), 128 3J(C'i-1,Hαi), 121 3J(C'i-1,C'i), and 122 3J(C'i-1,Cβi). Without prior knowledge from either X-ray crystallography or NMR data, such as NOE distance constraints, accurate φ dihedral angles are specified for 122 non-glycine and non-proline residues out of a total of 147 amino acids. Different models of molecular internal mobility are considered. The Karplus coefficients obtained are applicable to the conformational analysis of φ torsions in other polypeptides.

The Amphitheater Mountains synform on the southern flank of the Alaska Range in south-central Alaska provides one of the most complete sections of a Large Igneous Province worldwide, revealing, in near continuous section: basal mafic and ultramafic sill complexes, associated mafic and ultramafic rocks, lower submarine lavas, and overlying subaerial lavas. Three-dimensional (3D) modeling of gravity and magnetic data shows details of the Amphitheater Mountains structure, flood basalt thickness, and geometry of ultramafic sills. Modeling is based on a compilation of existing regional and newly-acquired high-resolution profile gravity data, a compilation of regional and high-resolution aeromagnetic surveys, and numerous rock-property data (including density, susceptibility, and magnetic remanence measurements of outcrops, hand samples, and drill cores). The final 3D model includes 12 layers with up to 2 km of Nikolai basalts in the center of the asymmetric, west-plunging, 50 km long Amphitheater synform. The western end of the synform appears to be terminated by a steep N-S structure. The outcropping Fish Lake and Tangle ultramafic sills, apparently connected beneath the surface, are traceable to 5 km depth, and modeling indicates variations in thickness (1 to 3 km), shape, and orientation which may identify paths of magma flow within the system.

The response of Trichogramma evanescens Westwood to various concentrations of hexane extracts from the scales of one of its hosts, the spruce budworm moth (Choristoneura fumiferana (Clemens)), was investigated. When placed on filter papers treated with hexane extracts of the moth scales, the wasps responded with two distinct phases of intensified searching behaviours. The first was characterized by a rapidly induced, transient klinokinetic response (decreased walking speed) lasting 10–20 s. This response had an abrupt threshold at scale extract concentrations between 0.05 and 0.5 mg/mL. After 15 s of exposure walking speeds subsequently recovered to rates similar to those of wasps walking on areas treated with hexane only (control). The second behaviour consisted of a persistent orthokinetic response (increased number of abrupt turns, greater than 70°), which resulted in the wasps remaining longer in the test arena. This increased retention on the patch was observed for extract concentrations below 0.05 mg/mL and appeared to be at least partially independent of changes in wasp velocity. Several parameters evaluated, including mean velocity, mean angular change, and fractal dimension, were highly variable within and between treatment groups, and showed no consistent pattern of response with dosage. In contrast, time spent on the patch and total distance travelled on the test area showed a significant correspondence to the dosage-dependent orthokinetic response of the wasps.

Water was evaporated from infective Trichostrongylus colubriformis larvae suspended in tap, distilled, and triple-distilled water, and the nematodes were then exposed to 50% and 70% relative humidity (RH) at 20 and 30 C. Sample groups were rehydrated for 4 h daily in similar quality water, observed for motility and counted, then returned to the same RH and temp and re-desiccated. Desiccation and rehydration were repeated until all motility ceased. Longest survival was 30 days at 20 C and 70% RH. In all temp and RH combinations, control (nondesiccated) and desiccated larvae survived longer in distilled or triple-distilled water than in tap water.