Search results for "45"

showing 10 items of 1896 documents

Epoxidation of benzo[a]pyrene-7,8-dihydrodiol by human CYP1A1 in reconstituted membranes. Effects of charge and nonbilayer phase propensity of the me…

2002

Human cytochrome P4501A1 (CYP1A1) is one of the key enzymes in the bioactivation of environmental pollutants such as benzo[a]pyrene (B[a]P) and other polycyclic aromatic hydrocarbons. To evaluate the effect of membrane properties and distinct phospholipids on the activity of human CYP1A1 purified insect cell-expressed human CYP1A1 and of human NADPH-P450 reductase were reconstituted into phospholipid vesicle membranes. Conversion rates of up to 36 pmol x min(-1) x pmol(-1) CYP1A1 of the enantiomeric promutagens (-)- and (+)-trans-7,8-dihydroxy-7,8-dihydro-B[a]P (7,8-diol) to the genotoxic diolepoxides were achieved. The highest rates were obtained when negatively charged lipids such as phos…

PhosphatidylethanolamineStereochemistryVesiclePhospholipidMembranes ArtificialPhosphatidylserineBiochemistryRecombinant ProteinsDihydroxydihydrobenzopyreneschemistry.chemical_compoundMembraneBiochemistrychemistryBenzo(a)pyrenepolycyclic compoundsCytochrome P-450 CYP1A1PyreneAnimalsEpoxy CompoundsHumansheterocyclic compoundsPhosphatidylinositolPhospholipidsEuropean journal of biochemistry
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An XMM-Newton and INTEGRAL view on the hard state of EXO 1745-248 during its 2015 outburst

2017

CONTEXT - Transient low-mass X-ray binaries (LMXBs) often show outbursts lasting typically a few-weeks and characterized by a high X-ray luminosity ($L_{x} \approx 10^{36}-10^{38}$ erg/sec), while for most of the time they are found in X-ray quiescence ($L_X\approx10^{31} -10^{33}$ erg/sec). EXO 1745-248 is one of them. AIMS - The broad-band coverage, and the sensitivity of instrument on board of {\xmm} and {\igr}, offers the opportunity to characterize the hard X-ray spectrum during {\exo} outburst. METHODS - In this paper we report on quasi-simultaneous {\xmm} and {\igr} observations of the X-ray transient {\exo} located in the globular cluster Terzan 5, performed ten days after the begin…

PhotonX-rays: BinarieAstrophysics::High Energy Astrophysical PhenomenaFOS: Physical sciencesTechniques: SpectroscopicAstrophysics::Cosmology and Extragalactic AstrophysicsAstrophysicsneutron; Techniques: Spectroscopic; X-rays: Binaries; X-rays: Bursts; X-rays: Individuals: EXO 1745-248; Astronomy and Astrophysics; Space and Planetary Science [Stars]01 natural sciencesIonization0103 physical sciencesX-rays: BurstAstrophysics::Solar and Stellar AstrophysicsEmission spectrum010303 astronomy & astrophysicsAstrophysics::Galaxy AstrophysicsHigh Energy Astrophysical Phenomena (astro-ph.HE)Physics010308 nuclear & particles physicsAstronomy and AstrophysicsRadiusAstronomy and AstrophysicStars: neutronNeutron starSpace and Planetary ScienceGlobular clusterElectron temperatureAstrophysics - High Energy Astrophysical PhenomenaX-rays: Individuals: EXO 1745-248Doppler broadening
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"Table 4" of "Backward electroproduction of pi0 mesons on protons in the region of nucleon resonances at four momentum transfer squared Q**2 = 1.0-Ge…

2005

Cross section SIG(T) + EPSILON*SIG(L) for COS(THETA*) = -0.825.

PhotoproductionComputingMilieux_THECOMPUTINGPROFESSIONElectron productionTheoryofComputation_ANALYSISOFALGORITHMSANDPROBLEMCOMPLEXITYE- P --> E- P PI0ComputingMethodologies_SYMBOLICANDALGEBRAICMANIPULATIONMathematicsofComputing_NUMERICALANALYSIS1.11-1.45ExclusiveInformationSystems_MISCELLANEOUSD2SIG/DOMEGADouble Differential Cross SectionGAMMA* P --> P PI0
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"Table 12" of "Backward electroproduction of pi0 mesons on protons in the region of nucleon resonances at four momentum transfer squared Q**2 = 1.0-G…

2005

Cross section SIG(TT) for COS(THETA*) = -0.825.

PhotoproductionElectron productionE- P --> E- P PI01.11-1.45ExclusiveD2SIG/DOMEGADouble Differential Cross SectionGAMMA* P --> P PI0
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"Table 8" of "Backward electroproduction of pi0 mesons on protons in the region of nucleon resonances at four momentum transfer squared Q**2 = 1.0-Ge…

2005

Cross section SIG(TL) for COS(THETA*) = -0.825.

PhotoproductionElectron productionE- P --> E- P PI01.11-1.45ExclusiveD2SIG/DOMEGADouble Differential Cross SectionGAMMA* P --> P PI0
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Hyperspectral terahertz microscopy via nonlinear ghost imaging

2020

Ghost imaging, based on single-pixel detection and multiple pattern illumination, is a crucial investigative tool in difficult-to-access wavelength regions. In the terahertz domain, where high-resolution imagers are mostly unavailable, ghost imaging is an optimal approach to embed the temporal dimension, creating a “hyperspectral” imager. In this framework, high resolution is mostly out of reach. Hence, it is particularly critical to developing practical approaches for microscopy. Here we experimentally demonstrate time-resolved nonlinear ghost imaging, a technique based on near-field, optical-to-terahertz nonlinear conversion and detection of illumination patterns. We show how space–time c…

Physics - Instrumentation and DetectorsComputer scienceTerahertz radiationFOS: Physical sciences02 engineering and technologyGhost imaging01 natural sciences010309 opticssymbols.namesakeOptics0103 physical sciencesMicroscopyCouplingbusiness.industryQC0454.T47Hyperspectral imagingInstrumentation and Detectors (physics.ins-det)QC0446.2021001 nanoscience & nanotechnologyAtomic and Molecular Physics and OpticsQC0350Electronic Optical and Magnetic MaterialsNonlinear systemWavelengthFourier transformComputer Science::Computer Vision and Pattern Recognitionsymbols0210 nano-technologybusinessOptics (physics.optics)Physics - Optics
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Positioning systems in Minkowski space-time: from emission to inertial coordinates

2009

The coordinate transformation between emission coordinates and inertial coordinates in Minkowski space-time is obtained for arbitrary configurations of the emitters. It appears that a positioning system always generates two different coordinate domains, namely, the front and the back emission coordinate domains. For both domains, the corresponding covariant expression of the transformation is explicitly given in terms of the emitter world-lines. This task requires the notion of orientation of an emitter configuration. The orientation is shown to be computable from the emission coordinates for the users of a `central' region of the front emission coordinate domain. Other space-time regions a…

Physics04.20.Cv95.10.JkInertial frame of reference45.20.DdPhysics and Astronomy (miscellaneous)Positioning systemAstrophysics::High Energy Astrophysical PhenomenaCoordinate systemMathematical analysisFOS: Physical sciencesGeneral Relativity and Quantum Cosmology (gr-qc)Domain (mathematical analysis)General Relativity and Quantum Cosmology04.20.-qTransformation (function)Orientation (geometry)Minkowski spaceCovariant transformation
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The influence of the solvent's mass on the location of the dividing surface for a model Hamiltonian

2019

The Transition State dividing surface is a key concept, not only for the precise calculation of the rate constant of a reaction, but also for the proper prediction of product ratios. The correct location of this surface is defined by the requirement that reactive trajectories do not recross it. In the case of reactions in solution the solvent plays an important role in the location of the dividing surface. In this paper we show with the aid of a model Hamiltonian that the effective mass of the solvent can dramatically change the location of the dividing surface. Keywords: Dynamical systems, Dividing surface, Reactions in solution, 2019 MSC: 00-01, 99-00

PhysicsDynamical systems theoryMathematical analysisSolvationlcsh:QD450-801General Physics and Astronomylcsh:Physical and theoretical chemistryDividing surfaceSurface reactionSistemes dinàmics diferenciablesChemical reactionlcsh:QC1-999Reactions in solutionSolventsymbols.namesakeReaction rate constantEffective mass (solid-state physics)Dynamical systemssymbolsPhysical and Theoretical ChemistryHamiltonian (quantum mechanics)lcsh:PhysicsFisicoquímica
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IGR J17451-3022: a dipping and eclipsing low mass X-ray binary

2016

In this paper, we report on the available X-ray data collected by INTEGRAL, Swift, and XMM-Newton during the first outburst of the INTEGRAL transient IGR J17451-3022, discovered in 2014 August. The monitoring observations provided by the JEM-X instruments on-board INTEGRAL and the Swift/XRT showed that the event lasted for about 9 months and that the emission of the source remained soft for the entire period. The source emission is dominated by a thermal component (kT~1.2 keV), most likely produced by an accretion disk. The XMM-Newton observation carried out during the outburst revealed the presence of multiple absorption features in the soft X-ray emission that could be associated to the p…

PhysicsHigh Energy Astrophysical Phenomena (astro-ph.HE)010308 nuclear & particles physicsAstrophysics::High Energy Astrophysical PhenomenaX-ray binaryFOS: Physical sciencesX-rays: individuals: IGR J17451-3022Astronomy and AstrophysicsAbsorption columnAstrophysicsAstronomy and AstrophysicOrbital periodX-rays: binarie01 natural sciencesSettore FIS/05 - Astronomia E AstrofisicaAccretion discSpace and Planetary ScienceIonization0103 physical sciencesThermalbinaries; X-rays: individuals: IGR J17451-3022; Astronomy and Astrophysics; Space and Planetary Science [X-rays]Astrophysics - High Energy Astrophysical PhenomenaLow MassAbsorption (electromagnetic radiation)010303 astronomy & astrophysics
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High-Energy pulse profile of the Transient X-ray Pulsar SAX J2103.5+4545

2005

In two recent INTEGRAL papers, Lutovinov et al. (2003) and Blay et al. (2004) report a timing and spectral analysis of the transient Be/X-ray pulsar SAX J2103.5+4545 at high energies (5--200 keV). In this work we present for the first time a study of the pulse profile at energies above 20 keV using INTEGRAL data. The spin-pulse profile shows a prominent (with a duty cycle of 14%) and broad (with a FWHM of ~ 51 s) peak and a secondary peak which becomes more evident above 20 keV. The pulsed fraction increases with energy from ~ 45% at 5--40 keV to ~ 80% at 40--80 keV. The morphology of the pulse profile also changes as a function of energy, consistent with variations in the spectral componen…

PhysicsX-rays : binariesScatteringAstrophysics::High Energy Astrophysical Phenomenapulsars : individual : SAX J2103.5+4545Astrophysics (astro-ph)Phase (waves)FOS: Physical sciencesAstronomy and AstrophysicsAstrophysicsRadiationAstrophysicsSpectral linePulse (physics)Full width at half maximumPulsarbinaries : closeSpace and Planetary Scienceclose; pulsars : individual : SAX J2103.5+4545; X-rays : binaries [binaries]X-ray pulsar
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