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PubMed2001

Very Early Nimodipine Use in Stroke (VENUS): a randomized, double-blind, placebo-controlled trial.

BACKGROUND AND PURPOSE: The Very Early Nimodipine Use in Stroke (VENUS) trial was designed to test the hypothesis that early treatment with nimodipine has a positive effect on survival and functional outcome after stroke. This was suggested in a previous meta-analysis on the use of nimodipine in stroke. However, in a recent Cochrane review we were unable to reproduce these positive results. This led to the early termination of VENUS after an interim analysis. METHODS: In this randomized, double-blind, placebo-controlled trial, treatment was started by general practitioners or neurologists within 6 hours after stroke onset (oral nimodipine 30 mg QID or identical placebo, for 10 days). Main analyses included comparisons of the primary end point (poor outcome, defined as death or dependency after 3 months) and secondary end points (neurological status and blood pressure 24 hours after inclusion, mortality after 10 days, and adverse events) between treatment groups. Subgroup analyses (on final diagnosis and based on the per-protocol data set) were performed. RESULTS: At trial termination, after inclusion of 454 patients (225 nimodipine, 229 placebo), no effect of nimodipine was found. After 3 months of follow-up, 32% (n=71) of patients in the nimodipine group had a poor outcome compared with 27% (n=62) in the placebo group (relative risk, 1.2; 95% CI, 0.9 to 1.6). A treatment effect was not found for secondary outcomes and in the subgroup analyses. CONCLUSIONS: The results of VENUS do not support the hypothesis of a beneficial effect of early nimodipine in stroke patients.

Acute Disease↗
PubMed1985

Spectra of simulated lightning on Venus, Jupiter, and Titan.

Laser-induced plasmas in various gas mixtures were used to simulate lightning in other planetary atmospheres. This method of simulation has the advantage of producing short-duration, high-temperature plasmas free from electrode contamination. The laser-induced plasma discharges in air are shown to accurately simulate terrestrial lightning and can be expected to simulate lightning spectra in other planetary atmospheres. Spectra from 240 to 880 nm are presented for simulated lightning in the atmospheres of Venus, Earth, Jupiter, and Titan. The spectra of lightning on the other giant planets are expected to be similar to that of Jupiter because the atmospheres of these planets are composed mainly of hydrogen and helium. The spectra of Venus and Titan show substantial amounts of radiation due to the presence of carbon atoms and ions and show CN Violet radiation. Although small amounts of CH4 and NH3 are present in the Jovian atmosphere, only emission from hydrogen and helium is observed. Most differences in the spectra can be understood in terms of the elemental ratios of the gas mixtures. Consequently, observations of the spectra of lightning on other planets should provide in situ estimates of the atmospheric and aerosol composition in the cloud layers in which lightning is occurring. In particular, the detection of inert gases such as helium should be possible and the relative abundance of these gases compared to major constituents might be determined.

Ammonia↗
PubMed1993

Fractionation of hydrogen and deuterium on Venus due to collisional ejection.

The fractionation factor f is important for interpreting the current escape fluxes of H and D on Venus and how the D/H ratio has evolved. The escape flux is currently governed by the two processes of charge exchange and collisional ejection by fast oxygen atoms. Using a best-fit parameterized equation for the O-H scattering angle phase function, more accurate branching ratios for the oxygen ion dissociation and including the effects of the initial energy and momentum of the ions and electrons, as well as for the hydrogen and deuterium gas, we have reanalyzed the collisional ejection process. Our analysis produces improved values for the efficiency of H and D escape as a function of the ionospheric temperature. From our results we propose the reduction of the hydrogen flux for collisional ejection from 8 to 3.5 x 10(6) cm-2 s-1. Assuming that collisions leading to escape occur mostly in the region between 200 and 400 km, the revised D/H fractionation factor due to collisional ejection is 0.47, where previously the process had been considered completely discriminating against deuterium escape (or f approximately 0.) The resulting deuterium flux is 3.1 x 10(4) cm-2 s-1, roughly 6 times the flux due to charge exchange, making collisional ejection the dominant escape mechanism for deuterium on Venus.

Atmosphere↗
PubMed1987

Determination of O2(a1 delta g) and O2(b1 sigma+ g) yields in the reaction O + ClO --> Cl + O2: implications for photochemistry in the atmosphere of Venus.

A discharge flow apparatus with chemiluminescence detector has been used to study the reaction O + ClO --> Cl + O2, where O2 = O2(a1 delta g) or O2(b1 sigma+ g). The measured quantum yields for producing O2(a1 delta g) and O2(b1 sigma+ g) in the above reaction are less than 2.5 x 10(-2) and equal to (4.4 +/- 1.1) x 10(-4), respectively. The observed O2(a1 delta g) airglow of Venus cannot be explained in the context of standard photochemistry using our experimental results and those reported in recent literature. The possibility of an alternative source of O atoms derived from SO2 photolysis in the mesosphere of Venus is suggested.

Atmosphere↗
PubMed2002

Reassessing the possibility of life on venus: proposal for an astrobiology mission.

With their similar size, chemical composition, and distance from the Sun, Venus and Earth may have shared a similar early history. Though surface conditions on Venus are now too extreme for life as we know it, it likely had abundant water and favorable conditions for life when the Sun was fainter early in the Solar System. Given the persistence of life under stabilizing selection in static environments, it is possible that life could exist in restricted environmental niches, where it may have retreated after conditions on the surface became untenable. High-pressure subsurface habitats with water in the supercritical liquid state could be a potential refugium, as could be the zone of dense cloud cover where thermoacidophilic life might have retreated. Technology based on the Stardust Mission to collect comet particles could readily be adapted for a pass through the appropriate cloud layer for sample collection and return to Earth.

Earth, Planet↗
PubMed2025

Venus flytraps' metabolome analysis discloses the metabolic fate of prey animal foodstock.

Carnivorous plants such as the Venus flytrap Dionaea muscipula survive in nutrient-poor habitats by attracting and consuming animals. Upon deflection of the touch-sensitive trigger hairs, the trap closes instantly. Panicking prey repeatedly collides with trigger hairs, which activate the endocrine system: mechano- and chemosensors translate the information on the prey's nature, size, and activity into jasmonate-dependent lytic enzyme secretion. This digestive fluid gradually degrades its exoskeleton and internal tissues. The released substances are absorbed by glands covering the inner trap surface. To understand Dionaea's modification of metabolism upon prey consumption, we compared the metabolic profiles associated with secretion and insect feeding. In favor of digestive enzyme secretion, the abundance of most amino acids decreased after JA-stimulation without prey present. By contrast, insect feeding resulted in an increase in almost all amino acids within the trap. In agreement with the export of prey-derived nitrogen, the abundance of certain amino acids also increased in the petiole. In response to feeding with urea, chitin, nucleic acids, or phospholipids, the amino acid profile remained relatively unchanged. This might indicate that the alterations in the Venus flytrap's metabolism depend both on the type of substance and on its amount.

Droseraceae↗
PubMed1991

The dark side of Venus: near-infrared images and spectra from the Anglo-Australian observatory.

Near-infrared images and spectra of the night side of Venus taken at the Anglo-Australian Telescope during February 1990 reveal four new thermal emission windows at 1.10, 1.18, 1.27, and 1.31 micrometers, in addition to the previously discovered windows at 1.74 and 2.3 micrometers. Images of the Venus night side show similar bright and dark markings in all windows, but their contrast is much lower at short wavelengths. The 1.27-micrometers window includes a bright, high-altitude O2 airglow feature in addition to a thermal contribution from the deep atmosphere. Simulations of the 1.27- and 2.3 micrometers spectra indicate water vapor mixing ratios near 40 +/- 20 parts per million by volume between the surface and the cloud base. No large horizontal gradients in the water vapor mixing ratios were detected at these altitudes.

Astronomy↗
PubMed1999

Climate change as a regulator of tectonics on Venus.

Tectonics, volcanism, and climate on Venus may be strongly coupled. Large excursions in surface temperature predicted to follow a global or near-global volcanic event diffuse into the interior and introduce thermal stresses of a magnitude sufficient to influence widespread tectonic deformation. This sequence of events accounts for the timing and many of the characteristics of deformation in the ridged plains of Venus, the most widely preserved volcanic terrain on the planet.

Atmosphere↗
PubMed2001

Discovery of the atomic oxygen green line in the Venus night airglow.

Green line emission at 557.7 nanometers arising from the O(1S - 1D) transition of atomic oxygen has been observed on the nightside of Venus with HIRES, the echelle spectrograph on the W. M. Keck I 10-meter telescope. We also observe optical emissions of molecular oxygen, consistent with the spectra from the Venera orbiters, but our green line intensity is so high that we cannot explain how it could be inconspicuous in the Venera spectra. An upper limit for the intensity of the O(1D - 3P) oxygen red line at 630 nanometers has also been obtained. The large green/red ratio indicates that the source is not associated with the Venus ionosphere. An important conclusion is that observation of the green line in a planetary atmosphere is not an indicator of an atmosphere rich in molecular oxygen.

Atmosphere↗
PubMed2005

Amino acid recognition by Venus flytrap domains is encoded in an 8-residue motif.

A motif foramino acid recognition by proteins or domains of the periplasmic binding protein-like I superfamily has been identified. An initial pattern of 5 residues was based on a multiple sequence alignment of selected proteins of that fold family and on common structural features observed in the crystal structure of some members of the family [leucine isoleucine valine binding protein (LIVBP), leucine binding protein (LBP), and metabotropic glutamate receptor type 1 (mGlu1R) amino terminal domain)]. This pattern was used against the PIR-NREF sequence database and further refined to retrieve all sequences of proteins that belong to the family and eliminate those that do not belong to it. A motif of 8 residues was finally selected to build up the general signature. A total of 232 sequences were retrieved. They were found to belong to only three families of proteins: bacterial periplasmic binding proteins (PBP, 71 sequences), family 3 (or C) of G-protein coupled receptor (GPCR) (146 sequences), and plant putative ionotropic glutamate receptors (iGluR, 15 sequences). PBPs are known to adopt a bilobate structure also named Venus flytrap domain, or LIVBP domain in the present case. Family 3/C GPCRs are also known to hold such a domain. However, for plant iGluRs, it was previously detected by classical similarity searches but not specifically described. Thus plant iGluRs carry two Venus flytrap domains, one that binds glutamate and an additional one that would be a modulatory LIVBP domain. In some cases, the modulator binding to that domain would be an amino acid.

Amino Acid Motifs↗
PubMed2006

Occurrence of Perkinsus olseni in the Venus clam Protothaca jedoensis in Korean waters.

This is the first report of the occurrence of Perkinsus olseni in the Venus clam Protothaca jedoensis off the western and southern coasts of South Korea. Histological observations revealed Perkinsus-like organisms in the mantle, gills, digestive tubules, and gonad. Haemocytic infiltration and tissue necrosis were also observed in heavily infected clams. Hypnospore formation of the Perkinsus-like organism was confirmed with Ray's fluid thioglycollate medium assay (RFTM). When incubated in filtered and aerated seawater, the hypnospore gave rise to cell division and subsequently discharged hundreds of motile zoospores. Genus- and species-specific polymerase chain reaction (PCR) assays and the DNA sequences of the internal transcribed spacer region (ITS) of the Perkinsus sp. isolated from the Venus clam were identical to those of P. olseni reported from the Manila clam Venerupis (=Ruditapes)philippinarum. Based on the DNA sequences and microscopic data, the Perkinsus-like pathogen isolated from P. jedoensis was identified as P. olseni, which parasitizes the Manila clam in European and Asian waters and Haliotis rubra (abalone) in Australian waters. The prevalence and infection intensity of a clam population collected from Yosu, Korea, was determined using RFTM and Choi's 2M NaOH digestion technique. The intensities averaged 10,768 and 7438 Perkinsus cells per gram tissue in 2003 and 2004, and the prevalence ranged from 37.0 to 53.9%, respectively.

Animals↗
PubMed2005

How the Venus flytrap snaps.

The rapid closure of the Venus flytrap (Dionaea muscipula) leaf in about 100 ms is one of the fastest movements in the plant kingdom. This led Darwin to describe the plant as "one of the most wonderful in the world". The trap closure is initiated by the mechanical stimulation of trigger hairs. Previous studies have focused on the biochemical response of the trigger hairs to stimuli and quantified the propagation of action potentials in the leaves. Here we complement these studies by considering the post-stimulation mechanical aspects of Venus flytrap closure. Using high-speed video imaging, non-invasive microscopy techniques and a simple theoretical model, we show that the fast closure of the trap results from a snap-buckling instability, the onset of which is controlled actively by the plant. Our study identifies an ingenious solution to scaling up movements in non-muscular engines and provides a general framework for understanding nastic motion in plants.

Biomechanical Phenomena↗
PubMed2004

Laboratory evidence for a key intermediate in the Venus atmosphere: peroxychloroformyl radical.

For two decades, the peroxychloroformyl radical, ClC(O)OO, has played a central role in models of the chemical stability of the Venus atmosphere. No confirmation, however, has been possible in the absence of laboratory measurements for ClC(O)OO. We report the isolation of ClC(O)OO in a cryogenic matrix and its infrared and ultraviolet spectral signatures. These experiments show that ClC(O)OO is thermally and photolytically stable in the Venus atmosphere. These experimental discoveries validate the existence of ClC(O)OO, confirm several longstanding model assumptions, and provide a basis for the astronomical search for this important radical species.

Journal Article↗
PubMed2002

Crystal structure of venus, a yellow fluorescent protein with improved maturation and reduced environmental sensitivity.

Yellow emission variants of green fluorescent protein (GFP) have been found useful in a variety of applications in biological systems due to their red-shifted emission spectrum and sensitivity to environmental parameters, such as pH and ionic strength. However, slow maturation properties and new requirements for more intense fluorescence necessitated further mutagenesis studies of these proteins. Venus, a new variant with improved maturation and brightness, as well as reduced environmental dependence, was recently developed by introducing five mutations into the well characterized variant, enhanced yellow fluorescent protein (EYFP). In this paper, we present the crystal structure of Venus at 2.2 A resolution, which enabled us to correlate its novel features with these mutation points. The rearrangement of several side chains near the chromophore, initiated by the F46L mutation, was found to improve maturation at 37 degrees C by removing steric and energetic constraints, which may hinder folding of the polypeptide chain, and by accelerating the oxidation of the Calpha-Cbeta bond of Tyr(66) during chromophore formation. M153T, V163A, and S175G were also found to improve the rate of maturation by creating regions of greater flexibility. F64L induced large conformational changes in the molecule, leading to the removal of halide sensitivity by preventing ion access to the binding site.

Amino Acid Sequence↗
PubMed2005

A double mutation in the extracellular Ca2+-sensing receptor's venus flytrap domain that selectively disables L-amino acid sensing.

The extracellular Ca(2+)-sensing receptor is activated allosterically by l-amino acids, and recent molecular analysis indicates that amino acids are likely to bind in the receptor's Venus flytrap domain. In the current study we set out to identify residues in the VFT domain that specifically support amino acid binding and/or amino acid-dependent receptor activation. Herein we describe two mutations of the Ca(2+)-sensing receptor (CaR) Venus Flytrap domain, T145A and S170T, that specifically impair amino acid sensing, leaving Ca2+ sensing intact, as determined by receptor-dependent activation of intracellular Ca2+ mobilization in fura-2-loaded HEK293 cells. With respect to the wild-type CaR, T145A and S170T exhibited reduced sensitivity to l-Phe, and T145A also exhibited markedly impaired l/d selectivity. When combined, the double mutant T145A/S170T exhibited normal or near-normal sensitivity to extracellular Ca2+ but was resistant to l-Phe at concentrations up to 100 mm. We conclude that T145A/S170T selectively disables l-amino acid sensing and that the Ca2+ and l-amino acid-sensing functions of the CaR can be dissociated.

Allosteric Site↗
PubMed1996

Electrical Properties of the Venus Surface from Bistatic Radar Observations

A bistatic radar experiment in 1994, involving reception on Earth of a specularly reflected, linearly polarized 13-centimeter-wavelength signal transmitted from the Magellan spacecraft in orbit around Venus, has established that the surface materials viewed at low and intermediate altitudes on Venus have a relative dielectric permittivity of 4.0 ± 0.5. However, bistatic results for the Maxwell Montes highlands imply an electrically lossy surface with an imaginary dielectric permittivity of -i 100 ± 50, probably associated with a specific conductivity of about 13 mhos per meter. Candidates for highlands surface composition include ferroelectrics, a thin frost of elemental tellurium, or a plating of magnetite or pyrites.

Journal Article↗
PubMed2024

Comparative transcriptomics of Venus flytrap (Dionaea muscipula) across stages of prey capture and digestion.

The Venus flytrap, Dionaea muscipula, is perhaps the world's best-known botanical carnivore. The act of prey capture and digestion along with its rapidly closing, charismatic traps make this species a compelling model for studying the evolution and fundamental biology of carnivorous plants. There is a growing body of research on the genome, transcriptome, and digestome of Dionaea muscipula, but surprisingly limited information on changes in trap transcript abundance over time since feeding. Here we present the results of a comparative transcriptomics project exploring the transcriptomic changes across seven timepoints in a 72-hour time series of prey digestion and three timepoints directly comparing triggered traps with and without prey items. We document a dynamic response to prey capture including changes in abundance of transcripts with Gene Ontology (GO) annotations related to digestion and nutrient uptake. Comparisons of traps with and without prey documented 174 significantly differentially expressed genes at 1 hour after triggering and 151 genes with significantly different abundances at 24 hours. Approximately 50% of annotated protein-coding genes in Venus flytrap genome exhibit change (10041 of 21135) in transcript abundance following prey capture. Whereas peak abundance for most of these genes was observed within 3 hours, an expression cluster of 3009 genes exhibited continuously increasing abundance over the 72-hour sampling period, and transcript for these genes with GO annotation terms including both catabolism and nutrient transport may continue to accumulate beyond 72 hours.

Droseraceae↗
PubMed2004

Economic analysis of VenUS I, a randomized trial of two bandages for treating venous leg ulcers.

BACKGROUND: The study investigated the cost-effectiveness of four-layer and short-stretch compression bandages for treating venous leg ulcers. METHODS: Cost-effectiveness and cost-utility analyses were performed using patient-level data collected alongside the VenUS I leg ulcer study. The perspective for the economic analysis was that of the UK National Health Service (NHS) and Personal Social Service. The time horizon for the analysis was 1 year after recruitment. Health benefit was measured as differences in ulcer-free days and quality-adjusted life years (QALYs). RESULTS: The mean healing time for ulcers treated with four-layer bandages was 10.9 (95 per cent confidence interval (c.i.) -6.8 to 29.1) days less than that for ulcers treated with short-stretch bandages. Mean average difference in QALYs between compression systems was -0.02 (95 per cent c.i. -0.08 to 0.04). The four-layer bandage cost a mean of pound 227.32 (95 per cent c.i. pound 16.53 to pound 448 .30) less per patient per year than the short-stretch bandage. CONCLUSION: On average, four-layer bandaging was associated with greater health benefits and lower costs than short-stretch bandaging.

Adult↗