Search results for "SIP"

showing 10 items of 1280 documents

Introduction To Multimedia Sip User Agents

2007

Settore ING-INF/03 - TelecomunicazioniUser Agent SIP Protocol
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Water-siphon test associated to barium study in the diagnosis of Gastro-Esophageal Reflux: a novel statistical approach

2010

Settore MED/18 - Chirurgia GeneraleReflusso gastroesofageo barium study Water siphon test
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Incremento dei livelli di 17-idrossiprogesterone in pazienti con sclerosi multipla in età pediatrica

2009

Settore MED/38 - Pediatria Generale E Specialisticasclerosi multipla 17-idrossiprogesterone
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Shock formation in the dispersionless Kadomtsev-Petviashvili equation

2016

The dispersionless Kadomtsev-Petviashvili (dKP) equation $(u_t+uu_x)_x=u_{yy}$ is one of the simplest nonlinear wave equations describing two-dimensional shocks. To solve the dKP equation we use a coordinate transformation inspired by the method of characteristics for the one-dimensional Hopf equation $u_t+uu_x=0$. We show numerically that the solutions to the transformed equation do not develop shocks. This permits us to extend the dKP solution as the graph of a multivalued function beyond the critical time when the gradients blow up. This overturned solution is multivalued in a lip shape region in the $(x,y)$ plane, where the solution of the dKP equation exists in a weak sense only, and a…

Shock formationFOS: Physical sciencesGeneral Physics and AstronomyKadomtsev–Petviashvili equation01 natural sciencesCritical point (mathematics)010305 fluids & plasmasDissipative dKP equation[ MATH.MATH-AP ] Mathematics [math]/Analysis of PDEs [math.AP]Mathematics - Analysis of PDEsMethod of characteristicsPosition (vector)[MATH.MATH-MP]Mathematics [math]/Mathematical Physics [math-ph]0103 physical sciencesFOS: Mathematics[MATH.MATH-AP]Mathematics [math]/Analysis of PDEs [math.AP]0101 mathematicsSettore MAT/07 - Fisica MatematicaMathematical PhysicsMathematical physicsMathematicsCusp (singularity)Multiscales analysisdispersionless Kadomtsev-Petviashvili equation; dissipative dKP equation; multiscales analysis; shock formationPlane (geometry)Multivalued functionApplied Mathematics010102 general mathematics[ MATH.MATH-MP ] Mathematics [math]/Mathematical Physics [math-ph]Statistical and Nonlinear PhysicsMathematical Physics (math-ph)Nonlinear Sciences::Exactly Solvable and Integrable SystemsDispersionless Kadomtsev-Petviashvili equationDissipative systemAnalysis of PDEs (math.AP)
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3D simulations of microquasar jets in clumpy stellar winds

2011

High-mass microquasars consist of a massive star and a compact object, the latter producing jets that will interact with the stellar wind. The evolution of the jets, and ultimately their radiative outcome, could depend strongly on the inhomogeneity of the wind, which calls for a detailed study. The hydrodynamics of the interaction between a jet and a clumpy wind is studied, focusing on the global wind and single clump-jet interplay. We have performed, using the code \textit{Ratpenat}, three-dimensional numerical simulations of a clumpy wind interacting with a mildly relativistic jet, and of individual clumps penetrating into a jet. For typical wind and jet velocities, filling factors of abo…

Shock wavePhysicsHigh Energy Astrophysical Phenomena (astro-ph.HE)Jet (fluid)010308 nuclear & particles physicsAstrophysics::High Energy Astrophysical PhenomenaFOS: Physical sciencesAstronomy and AstrophysicsAstrophysicsAstrophysics::Cosmology and Extragalactic AstrophysicsCompact starDissipationKinetic energy01 natural sciences13. Climate actionSpace and Planetary ScienceSpeed of sound0103 physical sciencesRadiative transferAstrophysics::Solar and Stellar AstrophysicsHigh Energy Physics::ExperimentAstrophysics - High Energy Astrophysical Phenomena010303 astronomy & astrophysicsAstrophysics::Galaxy AstrophysicsO-type star
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Capturing shock waves in inelastic granular gases

2005

Shock waves in granular gases generated by hitting an obstacle at rest are treated by means of a shock capturing scheme that approximates the Euler equations of granular gas dynamics with an equation of state (EOS), introduced by Goldshtein and Shapiro [J. Fluid Mech. 282 (1995) 75-114], that takes into account the inelastic collisions of granules. We include a sink term in the energy balance to account for dissipation of the granular motion by collisional inelasticity, proposed by Haff [J. Fluid Mech. 134 (1983) 401-430], and the gravity field added as source terms. We have computed the approximate solution to a one-dimensional granular gas falling on a plate under the acceleration of grav…

Shock wavePhysicsNumerical AnalysisEquation of statePhysics and Astronomy (miscellaneous)Applied MathematicsInelastic collisionEnergy balanceGas dynamicsDissipationComputer Science ApplicationsEuler equationsComputational Mathematicssymbols.namesakeClassical mechanicsGravitational fieldModeling and SimulationsymbolsJournal of Computational Physics
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Dissipative shock waves in all-normal-dispersion mode-locked fiber lasers

2014

4 pags.; 4 figs.; OCIS codes: (140.4050) Mode-locked lasers; (140.3510) Lasers, fiber.

Shock wavePhysicsSpectral shape analysisbusiness.industryLasersLasers; fiber Mode-locked lasersDissipationMode-locked lasersAtomic and Molecular Physics and OpticsBurgers' equationOpticsFiber laserDissipative systemDispersion (water waves)businessPhotonic-crystal fiberfiber
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Radio polarization maps of shell-type SNRs II. Sedov models with evolution of turbulent magnetic field

2017

Polarized radio emission has been mapped with great detail in several Galactic supernova remnants (SNRs), but has not yet been exploited to the extent it deserves. We have developed a method to model maps of the Stokes parameters for shell-like SNRs during their Sedov evolution phase. At first, 3-dimensional structure of a SNR has been computed, by modeling the distribution of the magnetohydrodynamic parameters and of the accelerated particles. The generation and dissipation of the turbulent component of magnetic field everywhere in SNR are also considered taking into account its interaction with accelerated particles. Then, in order to model the emission, we have used a generalization of t…

Shock waveRadiation mechanisms: non-thermalAstrophysics::High Energy Astrophysical PhenomenaFOS: Physical sciencesCosmic rayAstrophysics01 natural sciencessymbols.namesake0103 physical sciencesFaraday effectStokes parameters010306 general physics010303 astronomy & astrophysicsISM: supernova remnantAstrophysics::Galaxy AstrophysicsPhysicsHigh Energy Astrophysical Phenomena (astro-ph.HE)Astronomy and AstrophysicsAstronomy and AstrophysicDissipationAcceleration of particlePolarization (waves)Cosmic rayMagnetic fieldSupernovaShock waveSpace and Planetary SciencesymbolsAstrophysics - High Energy Astrophysical Phenomena
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Measurements of Silicon Photomultipliers Responsivity in Continuous Wave

2012

SiPM Silicon Photomultiplier SPAD Responsivity Photodiode Continuous Wave Quantum Detector
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N-on-P and P-on-N Silicon Photomultipliers: Responsivity comparison in the continuous wave regime

2013

We report on the electrical and optical comparison, in continuous wave regime, of two novel classes of silicon photomultipliers fabricated in planar technology on silicon P-type and Ntype substrate respectively. A physical explanation of the experimental results is provided.

SiPM Silicon Photomultiplier SPAD Responsivity Photodiode Continuous Wave Quantum DetectorSettore ING-INF/01 - Elettronica
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