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Barber, Jacqueline Claire. "Hydrodynamics, heat transfer and flow boiling instabilities in microchannels." Thesis, University of Edinburgh, 2010. http://hdl.handle.net/1842/4000.
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Boiling in microchannels is a very efficient mode of heat transfer with high heat and mass transfer coefficients achieved. Less pumping power is required for two-phase flows than for single-phase liquid flows to achieve a given heat removal. Applications include electronics cooling such as cooling microchips in laptop computers, and process intensification with compact evaporators and heat exchangers. Evaporation of the liquid meniscus is the main contributor to the high heat fluxes achieved due to phase change at thin liquid films in a microchannel. The microscale hydrodynamic motion at the meniscus and the flow boiling heat transfer mechanisms in microchannels are not fully understood and are very different from those in macroscale flows. Flow instability phenomena are noted as the bubble diameter approaches the channel diameter. These instabilities need to be well understood and predicted due to their adverse effects on the heat transfer. A fundamental approach to the study of two-phase flow boiling in microchannels has been carried out. Simultaneous visualisation and hydrodynamic measurements were carried out investigating flow boiling instabilities in microchannels using two different working fluids (n-Pentane and FC-72). Rectangular, borosilicate microchannels of hydraulic diameter range 700-800 μm were used. The novel heating method, via electrical resistance through a transparent, metallic deposit on the microchannel walls, has enabled simultaneous heating and visualisation to be achieved. Images and video sequences have been recorded with both a high-speed camera and an IR camera. Bubble dynamics, bubble confinement and elongated bubble growth have been shown and correlated to the temporal pressure fluctuations. Both periodic and nonperiodic instabilities have been observed during flow boiling in the microchannel. Analysis of the IR images in conjunction with pressure drop readings, have allowed the correlation of the microchannel pressure drop to the wall temperature profile, during flow instabilities. Bubble size is an important parameter when understanding boiling characteristics and the dynamic bubble phenomena. In this thesis it has been demonstrated that the flow passage geometry and microchannel confinement effects have a significant impact on boiling, bubble generation and bubble growth during flow boiling in microchannels.
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Cai, Kai. "Three-dimensional hydrodynamics simulations of gravitational instabilities in embedded protoplanetary disks." [Bloomington, Ind.] : Indiana University, 2006. http://gateway.proquest.com/openurl?url_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:dissertation&res_dat=xri:pqdiss&rft_dat=xri:pqdiss:3229601.
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Thesis (Ph.D.)--Indiana University, Dept. of Astronomy, 2006."Title from dissertation home page (viewed July 11, 2007)." Source: Dissertation Abstracts International, Volume: 67-08, Section: B, page: 4472. Adviser: Richard H. Durisen.
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Murphy, Jeremiah Wayne. "Multi-dimensional Hydrodynamics of Core-collapse Supernovae." Diss., The University of Arizona, 2008. http://hdl.handle.net/10150/194155.
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Core-collapse supernovae are some of the most energetic events in the Universe, they herald the birth of neutron stars and black holes, are a major site for nucleosynthesis, influence galactic hydrodynamics, and trigger further star formation. As such, it is important to understand the mechanism of explosion. Moreover, observations imply that asymmetries are, in the least, a feature of the mechanism, and theory suggests that multi-dimensional hydrodynamics may be crucial for successful explosions. In this dissertation, we present theoretical investigations into the multi-dimensional nature of the supernova mechanism. It had been suggested that nuclear reactions might excite non-radial g-modes (the ε-mechanism) in the cores of progenitors, leading to asymmetric explosions. We calculate the eigenmodes for a large suite of progenitors including excitation by nuclear reactions and damping by neutrino and acoustic losses. Without exception, we find unstable g-modes for each progenitor. However, the timescales for growth are at least an order of magnitude longer than the time until collapse. Thus, the ε-mechanism does not provide appreciable amplification of non-radial modes before the core undergoes collapse. Regardless, neutrino-driven convection, the standing accretion shock instability, and other instabilities during the explosion provide ample asymmetry. To adequately simulate these, we have developed a new hydrodynamics code, BETHE-hydro that uses the Arbitrary Lagrangian-Eulerian (ALE) approach, includes rotational terms, solves Poisson’s equation for gravity on arbitrary grids, and conserves energy and momentum in its basic implementation. By using time dependent arbitrary grids that can adapt to the numerical challenges of the problem, this code offers unique flexibility in simulating astrophysical phenomena. Finally, we use BETHE-hydro to investigate the conditions and criteria for supernova explosions by the neutrino mechanism. We find that a critical luminosity/ mass-accretion-rate condition distinguishes non-exploding from exploding models in hydrodynamic 1D and 2D simulations. Importantly, the critical luminosity for 2D simulations is found to be ∼70% of the critical luminosity for 1D simulations. We identify the specifics ofmulti-dimensional hydrodynamic simulations that enable explosions at lower neutrino luminosities in 2D and discuss how these results might foreshadow successful explosions by eventual 3D radiation-hydrodynamic simulations.
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Hadley, Kathryn Z. 1955. "Linear stability analysis of nonaxisymmetric instabilities in self-gravitating polytropic disks." Thesis, University of Oregon, 2011. http://hdl.handle.net/1794/11253.
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xvii, 371 p. : col. ill.An important problem in astrophysics involves understanding the formation of planetary systems. When a star-forming cloud collapses under gravity its rotation causes it to flatten into a disk. Only a small percentage of the matter near the rotation axis falls inward to create the central object, yet our Sun contains over 99% of the matter of our Solar System. We examine how global hydrodynamic instabilities transport angular momentum through the disk causing material to accrete onto the central star. We analyze the stability of polytropic disks in the linear regime. A power law angular velocity of power q is imposed, and the equilibrium disk structure is found through solution of the time-independent hydrodynamic equations via the Hachisu self-consistent field method. The disk is perturbed, and the time-dependent linearized hydrodynamic equations are used to evolve it. If the system is unstable, the characteristic growth rate and frequency of the perturbation are calculated. We consider modes with azimuthal e im[varphi] dependence, where m is an integer and [varphi] is the azimuthal angle. We map trends across a wide parameter space by varying m , q and the ratios of the star-to-disk mass M * /M d and inner-to-outer disk radius r - /r + . We find that low m modes dominate for small r - /r + , increasing to higher r - /r + as M * /M d increases, independent of q . Three main realms of behavior are identified, for M * << M d , M * [approximate] M d and M * >> M d , and analyzed with respect to the I, J and P mode types as discussed in the literature. Analysis shows that for M * << M d , small r - /r + disks are dominated by low m I modes, which give way to high m J modes at high r - /r + . Low m J modes dominate M * [approximate] M d disks for small r - /r + , while higher m I modes dominate for high r - /r + . Behavior diverges with q for M * >> M d systems with high q models approximating M * [approximate] M d characteristics, while low q models exhibit m = 2 I modes dominating where r - /r + < 0.60.
Committee in charge: Raymond Frey, Chairperson; James Imamura, Advisor; Robert Zimmerman, Member; Paul Csonka, Member; Alan Rempel, Outside Member
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Simon, Jacob B., Philip J. Armitage, Andrew N. Youdin, and Rixin Li. "Evidence for Universality in the Initial Planetesimal Mass Function." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/626045.
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Planetesimals may form from the gravitational collapse of dense particle clumps initiated by the streaming instability. We use simulations of aerodynamically coupled gas-particle mixtures to investigate whether the properties of planetesimals formed in this way depend upon the sizes of the particles that participate in the instability. Based on three high-resolution simulations that span a range of dimensionless stopping times 6 X 10(-3) <= tau <= 2, no statistically significant differences in the initial planetesimal mass function are found. The mass functions are fit by a power law, dN/dM(p) proportional to M-p(-p), with p = 1.5-1.7 and errors of Delta p approximate to 0.1. Comparing the particle density fields prior to collapse, we find that the high-wavenumber power spectra are similarly indistinguishable, though the large-scale geometry of structures induced via the streaming instability is significantly different between all three cases. We interpret the results as evidence for a near-universal slope to the mass function, arising from the small-scale structure of streaming-induced turbulence.
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Nuruzzaman, Shelly. "Study of parametric and hydrodynamic instabilities in laser produced plasmas." Thesis, Imperial College London, 2000. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.391443.
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Kazeroni, Rémi. "Explosion asymétrique des supernovae gravitationnelles." Thesis, Université Paris-Saclay (ComUE), 2016. http://www.theses.fr/2016SACLS315/document.
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L'explosion en supernova gravitationnelle représente le stade ultime de l'évolution des étoiles massives.La contraction du cœur de fer peut être suivie d'une gigantesque explosion qui donne naissance à une étoile à neutrons.La dynamique multi-dimensionnelle de la région interne, pendant les premières centaines de millisecondes, joue un rôle crucial sur le succès de l'explosion car des instabilités hydrodynamiques sont capables de briser la symétrie sphérique de l'effondrement.Les mouvements transverses et à grande échelle générés par deux instabilités, la convection induite par les neutrinos et l'instabilité du choc d'accrétion stationnaire (SASI),augmentent l'efficacité du chauffage de la matière par les neutrinos au point de déclencher une explosion asymétrique et d'impacter les conditions de naissance de l'étoile à neutrons. Dans cette thèse, les instabilités sont étudiées au moyen de simulations numériques de modèles simplifiés.Ces modèles permettent une vaste exploration de l'espace des paramètres et une meilleure compréhension physique des instabilités, généralement inaccessibles aux modèles réalistes.L'analyse du régime non-linéaire de SASI établit les conditions de formation d'un mode spiral et évalue sa capacité à redistribuer radialement le moment cinétique.L'effet de la rotation sur la dynamique du choc d'accrétion est également pris en compte.Si la rotation est suffisamment rapide, une instabilité de corotation se superpose à SASI et impacte grandement la dynamique.Les simulations permettent de mieux contraindre l'importance des modes non-axisymétriques dans le bilan de moment cinétique de l'effondrement du cœur de fer en étoile à neutrons.SASI pourrait sous certaines conditions accélérer ou ralentir la rotation du pulsar formé dans l'explosion.Enfin, une étude d'un modèle idéalisé de la région de chauffage est menée pour caractériser le déclenchement non-linéaire de la convection par des perturbations telles que celles produites par SASI ou les inhomogénéités de combustion pré-effondrement.L'analyse de la dimensionnalité sur le développement de la convection permet de discuter l'interprétation des modèles globaux et met en évidence les effets bénéfiques de la dynamique tridimensionnelle sur le déclenchement de l'explosionA core-collapse supernova represents the ultimate stage of the evolution of massive stars.The iron core contraction may be followed by a gigantic explosion which gives birth to a neutron star.The multidimensional dynamics of the innermost region, during the first hundreds milliseconds, plays a decisive role on the explosion success because hydrodynamical instabilities are able to break the spherical symmetry of the collapse.Large scale transverse motions generated by two instabilities, the neutrino-driven convection and the Standing Accretion Shock Instability (SASI),increase the heating efficiency up to the point of launching an asymmetric explosion and influencing the birth properties of the neutron star.In this thesis, hydrodynamical instabilities are studied using numerical simulations of simplified models.These models enable a wide exploration of the parameter space and a better physical understanding of the instabilities, generally inaccessible to realistic models.The non-linear regime of SASI is analysed to characterize the conditions under which a spiral mode prevails and to assess its ability to redistribute angular momentum radially.The influence of rotation on the shock dynamics is also addressed.For fast enough rotation rates, a corotation instability overlaps with SASI and greatly impacts the dynamics.The simulations enable to better constrain the effect of non-axisymmetric modes on the angular momentum budget of the iron core collapsing into a neutron star.SASI may under specific conditions spin up or down the pulsar born during the explosion.Finally, an idealised model of the heating region is studied to characterize the non-linear onsetof convection by perturbations such as those produced by SASI or pre-collapse combustion inhomogeneities. The dimensionality issue is examined to stress the beneficial consequences of the three-dimensional dynamics on the onset of the explosion
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Simon, Jacob B., Philip J. Armitage, Rixin Li, and Andrew N. Youdin. "THE MASS AND SIZE DISTRIBUTION OF PLANETESIMALS FORMED BY THE STREAMING INSTABILITY. I. THE ROLE OF SELF-GRAVITY." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621219.
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We study the formation of planetesimals in protoplanetary disks from the gravitational collapse of solid over-densities generated via the streaming instability. To carry out these studies, we implement and test a particle-mesh self-gravity module for the ATHENA code that enables the simulation of aerodynamically coupled systems of gas and collisionless self-gravitating solid particles. Upon employment of our algorithm to planetesimal formation simulations, we find that (when a direct comparison is possible) the ATHENA simulations yield predicted planetesimal properties that agree well with those found in prior work using different numerical techniques. In particular, the gravitational collapse of streaming-initiated clumps leads to an initial planetesimal mass function that is well-represented by a power law, dN / dM(p) proportional to M-p(-p), with p similar or equal to 1.6 +/- 0.1, which equates to a differential size distribution of dN / dR(p) proportional to R-p(-q), with q similar or equal to 2.8 +/- 0.1. We find no significant trends with resolution from a convergence study of up to 512(3) grid zones and N-par approximate to 1.5 x 10(8) particles. Likewise, the power-law slope appears indifferent to changes in the relative strength of self-gravity and tidal shear, and to the time when (for reasons of numerical economy) self-gravity is turned on, though the strength of these claims is limited by small number statistics. For a typically assumed radial distribution of minimum mass solar nebula solids (assumed here to have dimensionless stopping time tau = 0.3), our results support the hypothesis that bodies on the scale of large asteroids or Kuiper Belt Objects could have formed as the high-mass tail of a primordial planetesimal population.
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Meyer, Christophe. "Experimental study of imprinting and hydrodynamic instabilities in laser and soft X-ray driven targets." Thesis, Imperial College London, 1998. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.298814.
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Riolfo, Luis Atilio. "Fingering instabilities in reactive and non ideal systems: an experimental approach." Doctoral thesis, Universite Libre de Bruxelles, 2013. http://hdl.handle.net/2013/ULB-DIPOT:oai:dipot.ulb.ac.be:2013/209515.
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Les instabilités de digitation sont des instabilités hydrodynamiques qui déforment l’interface entre deux fluides sous forme de doigts. Elles apparaissent lorsqu'un fluide plus mobile déplace un fluide moins mobile, ce qui peut être engendré par des gradients de densité (auquel cas on parlera de digitation de densité), de viscosité (digitation visqueuse) ou encore de tension de surface. Dans ce cadre, l’objectif de ce travail est d'étudier par une approche principalement expérimentale dans quelle mesure des réactions chimiques et des propriétés de mélange non idéal peuvent modifier voire induire de telles instabilités. Le but est de comprendre les dynamiques spatio-temporelles résultant de l’interaction entre réactions chimiques, diffusion, propriétés de mélange et instabilités de digitation. Pour ce faire, nous explorons expérimentalement et analysons à l’aide de modèles théoriques simples différentes dynamiques hydrodynamiquement instables dans des mélanges réactifs ou non idéaux. Nous étudions tout d’abord l’évolution de la zone de mélange non idéal entre deux fluides purs lorsque le fluide le moins dense est placé au dessus du fluide le plus dense dans le champ de gravité. Nous montrons que le fait que la densité du mélange évolue de manière non monotone en fonction de sa composition peut être la source de digitation de densité. Nous étudions ensuite l'influence de réactions chimiques simples sur la digitation de densité à l'interface entre fluides miscibles et partiellement miscibles, en clarifiant l’impact de la diffusion différentielle entre divers solutés de solutions réactives et du taux de miscibilité sur le phénomène de digitation. Dans le cas de la digitation de viscosité, nous analysons tout d'abord dans quelle mesure une réaction chimique, en induisant des profils de viscosité non monotones, peut accroître ou limiter le développement de la digitation visqueuse. Nous démontrons de plus que, dans le déplacement stable d'un fluide moins visqueux par un fluide plus visqueux, une réaction chimique peut générer de la digitation visqueuse en induisant des profils de viscosité non monotones. Enfin, nous explorons expérimentalement l’étalement de films minces réactifs sur des substrats solides. Nous démontrons que, dans certaines conditions, des réactions chimiques peuvent induire des flux convectifs de Marangoni liés à des gradients de tension superficielle qui déstabilisent le bord du film par digitation, produisant un motif fractal.
Doctorat en Sciences
info:eu-repo/semantics/nonPublished
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Klee, J., T. F. Illenseer, M. Jung, and W. J. Duschl. "The impact of numerical oversteepening on the fragmentation boundary in self-gravitating disks." EDP SCIENCES S A, 2017. http://hdl.handle.net/10150/625972.
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Context. Whether or not a self-gravitating accretion disk fragments is still an open issue. There are many different physical and numerical explanations for fragmentation, but simulations often show a non-convergent behavior for ever better resolution. Aims. We aim to investigate the influence of different numerical limiters in Godunov type schemes on the fragmentation boundary in self-gravitating disks. Methods. We have compared the linear and non-linear outcomes in two-dimensional shearingsheet simulations using the VANLE ER and the SUPERBEE limiter. Results. We show that choosing inappropriate limiting functions to handle shock-capturing in Godunov type schemes can lead to an overestimation of the surface density in regions with shallow density gradients. The effect amplifies itself on timescales comparable to the dynamical timescale even at high resolutions. This is exactly the environment in which clumps are expected to form. The effect is present without, but scaled up by, self-gravity and also does not depend on cooling. Moreover it can be backtracked to a well known effect called oversteepening. If the effect is also observed in the linear case, the fragmentation limit is shifted to larger values of the critical cooling timescale.
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Hammer, Michael, Kaitlin M. Kratter, and Min-Kai Lin. "Slowly-growing gap-opening planets trigger weaker vortices." OXFORD UNIV PRESS, 2017. http://hdl.handle.net/10150/623939.
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The presence of a giant planet in a low-viscosity disc can create a gap edge in the disc's radial density profile sharp enough to excite the Rossby wave instability. This instability may evolve into dust-trapping vortices that might explain the `banana-shaped' features in recently observed asymmetric transition discs with inner cavities. Previous hydrodynamical simulations of planet-induced vortices have neglected the time-scale of hundreds to thousands of orbits to grow a massive planet to Jupiter size. In this work, we study the effect of a giant planet's runaway growth time-scale on the lifetime and characteristics of the resulting vortex. For two different planet masses (1 and 5 Jupiter masses) and two different disc viscosities (alpha= 3 x 10-4 and 3 x 10-5), we compare the vortices induced by planets with several different growth time-scales between 10 and 4000 planet orbits. In general, we find that slowly-growing planets create significantly weaker vortices with lifetimes and surface densities reduced by more than 50 per cent. For the higher disc viscosity, the longest growth time-scales in our study inhibit vortex formation altogether. Additionally, slowly-growing planets produce vortices that are up to twice as elongated, with azimuthal extents well above 180. in some cases. These unique, elongated vortices likely create a distinct signature in the dust observations that differentiates them from the more concentrated vortices that correspond to planets with faster growth time-scales. Lastly, we find that the low viscosities necessary for vortex formation likely prevent planets from growing quickly enough to trigger the instability in self-consistent models.
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Lehmann, M. (Marius). "Waves in planetary rings:hydrodynamic modeling of resonantly forced density waves and viscous overstability in Saturn’s rings." Doctoral thesis, Oulun yliopisto, 2018. http://urn.fi/urn:isbn:9789526221168.
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Abstract
The present thesis investigates the dynamics of wave structures in dense planetary rings by employing hydrodynamic models, along with local N-body simulations of the particulate ring flow. The focus is on the large-scale satellite induced spiral density waves as well as on the free short-scale waves generated by the viscous overstability in Saturn's A and B rings.
An analytic weakly nonlinear model is derived by using perturbation theory based on multi-scale methods to compute the damping behavior of nonlinear spiral density waves in a planetary ring subject to viscous overstability. In order to study the complex spatio-temporal evolution of these wave structures, numerical schemes are developed to integrate the hydrodynamical equations in time on large radial domains, taking into account collective self-gravity forces of the ring material, as well as the forcing by an external satellite. The required numerical stability and accuracy is achieved by applying Flux-Vector-Splitting methods aligned with advanced shock-capturing techniques. The free short-scale overstable waves are also investigated with local N-body simulations of the sheared ring flow. In particular, the influence of collective self-gravity between the ring particles as well as the periodic forcing due to a nearby Lindblad resonance on the overstable wave pattern is considered.
The linear stability criterion for spiral density waves in Saturn’s rings is found to be identical to the condition for the onset of spontaneous viscous overstability in the limit of long wavelengths and agrees with the stability criterion for density waves derived by Borderies et al. within the streamline formalism. The derived nonlinear damping behavior of density waves can be very different from what has previously been thought. The role of collective self-gravity on the nonlinear evolution of short-scale overstable waves is determined, reconciling the partly contradicting results of previous studies. It is shown that collective self-gravity plays an important role in setting the length-scale on which the nonlinear overstable waves saturate in a planetary ring. A co-existence of spiral density waves and short-scale overstable waves is modeled in terms of one-dimensional large-scale hydrodynamical integrations.
Due to the restriction to one space dimension, certain terms in the hydrodynamical equations that arise from the spiral shape of a density wave need to be approximated based on the weakly nonlinear model. These integrations reveal that density waves and spontaneous viscous overstability undergo complex interactions. In particular it is found that, depending on the relative magnitude of the two wave structures, the presence of short-scale overstable waves can lead to a damping of an overstable density wave and vice versa, density waves can suppress overstability. The effect of a density wave on the viscous overstability is also studied in terms of a simplified axisymmetric model of a ring perturbed by a nearby Lindblad resonance. A linear hydrodynamic stability analysis and local N-body simulations of this model system conform the corresponding results of the large-scale hydrodynamical integrations.
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Lin, Min-Kai, and Andrew N. Youdin. "A Thermodynamic View of Dusty Protoplanetary Disks." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/626177.
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Small solids embedded in gaseous protoplanetary disks are subject to strong dust-gas friction. Consequently, tightly coupled dust particles almost follow the gas flow. This near conservation of the dust-to-gas ratio along streamlines is analogous to the near conservation of entropy along flows of (dust-free) gas with weak heating and cooling. We develop this thermodynamic analogy into a framework to study dusty gas dynamics in protoplanetary disks. We show that an isothermal dusty gas behaves like an adiabatic pure gas, and that finite dust-gas coupling may be regarded as effective heating/cooling. We exploit this correspondence to deduce that (1) perfectly coupled, thin dust layers cannot cause axisymmetric instabilities; (2) radial dust edges are unstable if the dust is vertically well-mixed; (3) the streaming instability necessarily involves a gas pressure response that lags behind dust density; and (4) dust-loading introduces buoyancy forces that generally stabilize the vertical shear instability associated with global radial temperature gradients. We also discuss dusty analogs of other hydrodynamic processes (e.g., Rossby wave instability, convective overstability, and zombie vortices) and how to simulate dusty protoplanetary disks with minor tweaks to existing codes for pure gas dynamics.
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Lin, Min-Kai, and Kaitlin M. Kratter. "ON THE GRAVITATIONAL STABILITY OF GRAVITO-TURBULENT ACCRETION DISKS." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621384.
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Low mass, self-gravitating accretion disks admit quasi-steady, "gravito-turbulent" states in which cooling balances turbulent viscous heating. However, numerical simulations show that gravito-turbulence cannot be sustained beyond dynamical timescales when the cooling rate or corresponding turbulent viscosity is too large. The result is disk fragmentation. We motivate and quantify an interpretation of disk fragmentation as the inability to maintain gravito-turbulence due to formal secondary instabilities driven by: (1) cooling, which reduces pressure support; and/or (2) viscosity, which reduces rotational support. We analyze the axisymmetric gravitational stability of viscous, non-adiabatic accretion disks with internal heating, external irradiation, and cooling in the shearing box approximation. We consider parameterized cooling functions in 2D and 3D disks, as well as radiative diffusion in 3D. We show that generally there is no critical cooling rate/viscosity below which the disk is formally stable, although interesting limits appear for unstable modes with lengthscales on the order of the disk thickness. We apply this new linear theory to protoplanetary disks subject to gravito-turbulence modeled as an effective viscosity, and cooling regulated by dust opacity. We find that viscosity renders the disk beyond similar to 60 au dynamically unstable on radial lengthscales a few times the local disk thickness. This is coincident with the empirical condition for disk fragmentation based on a maximum sustainable stress. We suggest turbulent stresses can play an active role in realistic disk fragmentation by removing rotational stabilization against self-gravity, and that the observed transition in behavior from gravito-turbulent to fragmenting may reflect instability of the gravito-turbulent state itself.
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Mamatsashvili, George. "Dynamics of perturbation modes in protoplanetary discs : new effects of self-gravity and velocity shear." Thesis, University of Edinburgh, 2011. http://hdl.handle.net/1842/5283.
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Protoplanetary discs, composed of gas and dust, usually surround young stellar objects and serve two main purposes: they determine the accretion of matter onto the central object and also represent sites of planet formation. The accretion proceeds through the transport of angular momentum outwards allowing the disc matter to fall towards the centre. A mechanism responsible for the transport can be turbulence, waves or other coherent structures originating from various instabilities in discs that could, in addition, play a role in the planet formation process. For an understanding of these instabilities, it is necessary to study perturbation dynamics in differentially rotating, or sheared media. Thus, this thesis focuses on new aspects in the perturbation dynamics in non-magnetised protoplanetary discs that arise due to their self-gravity and velocity shear associated with the disc’s differential rotation. The analysis is carried out in the framework of the widely employed local shearing box approximation. We start with 2D discs and then move on to 3D ones. In 2D discs, there are two basic perturbation types/modes – spiral density waves and vortices – that are responsible for angular momentum transport and that can also contribute to accelerating planet formation. First, in the linear regime, we demonstrate that the vortical mode undergoes large growth due to self-gravity and in this process generates density waves via shear-induced linear mode coupling phenomenon. This is noteworthy, because commonly only density waves are considered in self-gravitating discs. Then we investigate vortex dynamics in the non-linear regime under the influence of self-gravity by means of numerical simulations. It is shown that vortices are no longer well-organised and long-lived structures, unlike those occurring in non-self-gravitating discs. They undergo recurring phases (lasting for a few disc rotation periods) of formation, growth and eventual destruction. We also discuss the dust trapping capability of such transient vortices. Perturbation dynamics in 3D vertically stratified discs is richer, as there are more mode types. We first consider non-axisymmetric modes in non-self-gravitating discs and then only axisymmetric modes in the more complicated case when self-gravity is present. Specifically, in non-self-gravitating discs with superadiabatic vertical stratification, motivated by the recent results on the transport properties of incompressible convection, we show that when compressibility is taken into account, the non-axisymmetric convective mode excites density waves via the same shear-induced linear mode coupling mechanism mentioned above. These generated density waves transport angular momentum outwards in the trailing phase, and we suggest that they may aid and enhance the transport due solely to convection in the non-linear regime, where the latter becomes outward. In the final part of the thesis, we carry out a linear analysis of axisymmetric vertical normal modes in stratified self-gravitating discs. Although axisymmetric modes do not display shear-induced couplings, their analysis provides insight into how gravitational instabilities develop in the 3D case and their onset criterion. We examine how the structure of dispersion curves and eigenfunctions of 3D modes are influenced by self-gravity, which mode first becomes gravitationally unstable and thus determines the onset criterion and nature of the gravitational instability in stratified discs. We also contrast the more exact instability criterion obtained with our 3D model with that of density waves in 2D discs. Based on these findings, we discuss the origin of 3D behaviour of perturbations involving noticeable disc surface distortions, as seen in some numerical simulations of self-gravitating discs.
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Baehr, Hans, Hubert Klahr, and Kaitlin M. Kratter. "The Fragmentation Criteria in Local Vertically Stratified Self-gravitating Disk Simulations." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/626182.
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Massive circumstellar disks are prone to gravitational instabilities, which trigger the formation of spiral arms that can fragment into bound clumps under the right conditions. Two-dimensional simulations of self-gravitating disks are useful starting points for studying fragmentation because they allow high-resolution simulations of thin disks. However, convergence issues can arise in 2D from various sources. One of these sources is the 2D approximation of self-gravity, which exaggerates the effect of self-gravity on small scales when the potential is not smoothed to account for the assumed vertical extent of the disk. This effect is enhanced by increased resolution, resulting in fragmentation at longer cooling timescales beta. If true, it suggests that the 3D simulations of disk fragmentation may not have the same convergence problem and could be used to examine the nature of fragmentation without smoothing self-gravity on scales similar to the disk scale height. To that end, we have carried out local 3D self-gravitating disk simulations with simple beta cooling with fixed background irradiation to determine if 3D is necessary to properly describe disk fragmentation. Above a resolution of similar to 40 grid cells per scale height, we find that our simulations converge with respect to the cooling timescale. This result converges in agreement with analytic expectations which place a fragmentation boundary at beta(crit) = 3.
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Gérard, Thomas. "Theoretical study of spatiotemporal dynamics resulting from reaction-diffusion-convection processes." Doctoral thesis, Universite Libre de Bruxelles, 2011. http://hdl.handle.net/2013/ULB-DIPOT:oai:dipot.ulb.ac.be:2013/209861.
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Dans les réacteurs industriels ou dans la nature, l'écoulement de fluides peut être couplé à des réactions chimiques. Dans de nombreux cas, il en résulte l'apparition de structures complexes dont les propriétés dépendent entre autres de la géométrie du système.Dans ce contexte, le but de notre thèse a été d'étudier de manière théorique et sur des modèles réaction-diffusion-convection simples les propriétés de dynamiques spatio-temporelles résultant du couplage chimie-hydrodynamique.
Nous nous sommes focalisés sur les instabilités hydrodynamiques de digitation visqueuse et de densité qui apparaissent respectivement lorsqu'un fluide dense est placé au-dessus d'un fluide moins dense dans le champ de gravité et lorsqu'un fluide visqueux est déplacé par un fluide moins visqueux dans un milieu poreux.
En particulier, nous avons étudié les problèmes suivants:
- L'influence d'une réaction chimique de type A + B → C sur la digitation visqueuse. Nous avons montré que les structures formées lors de cette instabilité varient selon que le réactif A est injecté dans le réactif B ou vice-versa si ces réactifs n'ont pas un coefficient de diffusion ou une concentration initiale identiques.
- Le rôle de pertes de chaleur par les parois du réacteur dans le cadre de la digitation de densité de fronts autocatalytiques exothermiques. Nous avons caractérisé les conditions de stabilité de fronts en fonction des pertes de chaleur et expliqué l'apparition de zones anormalement chaudes lors de cette instabilité.
- L'influence de l'inhomogénéité du milieu sur la digitation de densité de solutions réactives ou non. Nous avons montré que les variations spatiales de perméabilité d'un milieu poreux peuvent figer ou faire osciller la structure de digitation dans certaines conditions.
- L'influence d'un champ électrique transverse sur l'instabilité diffusive et la digitation de densité de fronts autocatalytiques. Il a été montré que cette interaction peut donner lieu à des nouvelles structures et changer les propriétés du front.
En conclusion, nous avons montré que le couplage entre réactions chimiques et mouvements hydrodynamiques est capable de générer de nouvelles structures spatio-temporelles dont les propriétés dépendent entre autres des conditions imposées au système.
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In industrial reactors or in nature, fluid flows can be coupled to chemical reactions. In many cases, the result is the emergence of complex structures whose properties depend among others on the geometry of the system.
In this context, the purpose of our thesis was to study theoretically using simple models of reaction-diffusion-convection, the properties of dynamics resulting from the coupling between chemistry and hydrodynamics.
We focused on the hydrodynamic instabilities of viscous and density fingering that occur respectively when a dense fluid is placed above a less dense one in the gravity field and when a viscous fluid is displaced by a less viscous fluid in a porous medium.
In particular, we studied the following issues:
- The influence of a chemical reaction type A + B → C on viscous fingering. We have shown that the fingering patterns observed during this instability depends on whether the reactant A is injected into the reactant B or vice versa if they do not have identical diffusion coefficients or initial concentrations.
- The role of heat losses through the reactor walls on the density fingering of exothermic autocatalytic fronts. We have characterized the conditions of stability of fronts depending on heat losses and explained the appearance of unusually hot areas during this instability.
- The influence of the inhomogeneity of the medium on the density fingering of reactive solutions or not. We have shown that spatial variations of permeability of a porous medium may freeze or generate oscillating fingering pattern under certain conditions.
- The influence of a transverse electric field on the Rayleigh-Taylor and diffusive instabilities of autocatalytic fronts. It was shown that this interaction may lead to new structures and may change the properties of the front.
In conclusion, we showed that the coupling between chemical reactions and hydrodynamic motions can generate new space-time structures whose properties depend among others, on the conditions imposed on the system.
Doctorat en Sciences
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Hasan, Haider. "Nearshore hydrodynamical instabilities." Thesis, University of Nottingham, 2006. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.438557.
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Marant, Mathieu. "Contrôle en boucle ouverte d'un écoulement tridimensionnel décollé par perturbations optimales." Phd thesis, Toulouse, INPT, 2017. http://oatao.univ-toulouse.fr/19494/1/MARANT_Mathieu.pdf.
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On calcule les amplifications d’énergie optimales de structures quasi longitudinales dans le sillage d’un corps épais axisymétrique à culot droit et dans une couche de mélange parallèle. Les amplifications d'énergie sont seulement modérées dans le sillage du corps axisymétrique tandis qu'elles sont grandes dans la couche de mélange. Les amplifications maximales augmentent avec le nombre de Reynolds et lorsque le nombre d’onde transverse (azimutal) décroît. Les structures amplifiées optimalement sont des stries longitudinales. Lorsqu’elles sont forcées à amplitudes finies, les stries optimales réduisent considérablement l’instationnarité du sillage du corps épais axisymétrique. Pour des nombres de Reynolds modérés, l’instationnarité du sillage peut être complètement supprimée si le forçage optimal est combiné avec un soufflage au culot uniforme. Dans le cas de la couche de mélange 2D, le taux de croissance maximal de l'instabilité de KelvinHelmholtz et le ratio de vitesse critique d'apparition de l'instabilité absolue peuvent être soit réduits soit augmentés en fonction des symétries des stries forcées. Dans ce cas, on montre que la déformation non linéaire moyenne doit être incluse dans l'analyse de sensibilité de l'instabilité et que cela n'influe pas sur la dépendance quadratique par rapport à l'amplitude des stries.
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Li, Rui-Qing. "Hydrodynamic instabilities of cylindrical interfaces." Thesis, McGill University, 1992. http://digitool.Library.McGill.CA:80/R/?func=dbin-jump-full&object_id=39521.
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This thesis consists of two parts. In the first part of the thesis, the Rayleigh-Taylor and the Kelvin-Helmholtz instabilities of a cylindrical interface between two inviscid fluids or two viscous fluids are analyzed from first principles (momentum and continuity equations). Dispersion equations, relating wavenumber, k, to growth rate, G, were derived for various conditions. Application of the dispersion equations to film boiling on a cylindrical heater and to breakup of a liquid film around a cylindrical body led to the development of mathematical models for the prediction of the dominant wavelengths formed during these processes for both inviscid and viscous fluids.Experiments were carried out to measure the dominant unstable wavelength during the breakup of a liquid film around a cylindrical body. It was found that the dominant wavelength decreased with a decrease in the radius of the cylindrical body in agreement with the present theory and in contradiction to previously published work.
In another application of the present theory, the breakup of a cylindrical liquid-in-gas jet and a cylindrical gas-in-liquid jet was analyzed based on the Kelvin-Helmholtz instability. It was predicted that the dominant wavelength decreased rapidly with an increase in the jet velocity.
In the second part of the thesis, gas injection through a very narrow slot into a liquid is examined extensively. A modified bubble formation model is proposed taking into consideration the surface tension force and the inertial force.
When gas was injected into liquid through a very narrow slot (50-250$ mu$m), three different bubbling regimes were found as the flow rate of gas was increased. They were: regular bubble regime at low flow rates, coalescence bubble regime at medium flow rates, and gas globe regime at high flow rates. The gas-dispersion characteristics of each of the regimes were discussed and mathematically analyzed. In the regular bubble regime, the bubble formation was dominated by both surface tension force and inertial force. In the coalescence bubble regime, the formation of bubbles was dominated by inertial forces only. In the gas globe regime, due to the Rayleigh-Taylor instability, multiple bubbles were formed at separate nodes of a continuous gas blanket extending the length of the slot. The critical transition condition between the regular bubble formation regime and the coalescence bubble regime is given.
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Lebranchu, Yannick. "Étude d'ondes non linéaires hydrodynamiques : approches théorique et expérimentale." Thesis, Vandoeuvre-les-Nancy, INPL, 2008. http://www.theses.fr/2008INPL005N/document.
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Cette thèse est dédiée à l'étude d'ondes non linéaires dans des écoulements en rotation. Dans une première partie, je me suis intéressé aux ondes de Rossby apparaissant par instabilités de thermoconvection dans une coquille sphérique en rotation représentant un modèle simplifié de noyau planétaire tellurique, et ce pour deux types de forçage: un chauffage interne correspondant à une activité radioactive du noyau et un chauffage différentiel lié à la différence de température entre les frontières interne et externe. Selon le théorème de Proudman-Taylor, l'écoulement possède une faible dépendance en la coordonnée axiale à cause de la rotation rapide. Cela permet de simplifier les modèles 3D en des modèles quasi géostrophiques 2D reposant sur une intégration axiale. Cette thèse présente la première comparaison systématique entre modèles 2D et 3D (Simitev, U-Glasgow) concernant des ondes de Rossby faiblement non linéaires. En 2D l'équation de Landau régissant l'amplitude de l'onde critique est calculée; l'amplitude de la convection et celle des écoulements zonaux ainsi prédites se comparent assez bien aux résultats 3D. L'existence d'une bifurcation sous-critique est établie à très bas nombre d'Ekman en chauffage interne et en chauffage différentiel, à condition dans ce dernier cas que le nombre de Prandtl soit petit. La seconde partie est une étude expérimentale de l'écoulement d'eau et de ses premières instabilités dans un canal annulaire creusé dans un plateau éventuellement en rotation surmonté d'un couvercle tournant. Trois cas sont étudiés: le cisaillement pur correspondant à la rotation du couvercle seul, la corotation rapide et la contrarotation pure. Le seuil d'instabilité détecté par mesures globales (visualisations par caméra vidéo) et locales par Vélocimétrie Laser Doppler se caractérise par des ondes spiralées. Dans le cas de la contrarotation pure, des structures localisées dans l'espace-temps peuvent coexister avec les ondes. Une comparaison est effectuée avec des calculs numériques (Serre, CNRS-Marseille). Un accord relativement bon est obtenu pour l'écoulement de base (vitesse azimutale) et la première instabilité (nombre de Reynolds, nombre d'onde et fréquence angulaire critiques)A first part is devoted to the study of the Rossby waves that appear in a rotating spherical shell representing the core of a terrestrial planet by thermal instabilities for two heating types. Internal heating is driven by radioactive sources and differential heating is driven by a difference of temperature between the internal and external frontiers. According to the Proudman-Taylor theorem, the flow depends only weakly on the axial coordinate because of the high rotation rate. Thus the 3D models can be simplified into quasi-geostrophic 2D models \textit{via} an axial integration. I present the first systematic comparison between 2D and 3D models (Simitev, U-Glasgow) for weakly nonlinear Rossby waves. In 2D the Landau equation that controls the amplitude of the critical wave is calculated. Predicted convection' amplitude and zonal flows agree rather well with the 3D results. The existence of a subcritical bifurcation is established at very low Ekman numbers with internal and differential heating; in this latter case, the Prandtl number also has to be small for the bifurcation to be subcritical. The second part is an experimental study of water flows and its first instabilities in an annular channel digged in a plate which may rotate, and which is sheared by a rotating lid. Three cases are studied: a pure shear where only the lid turns, a rapid corotation and a pure contrarotation. The onset of instability is studied with global measurements (using a video camera) and local ones (Laser Doppler Anemometry) and is characterized by spiralling waves. In the case of contrarotation, patterns localized in space and time may coexist with the waves. The comparison of these results with numerical ones (Serre, CNRS-Marseille) is done and shows a rather good agreement for the basic azimutal flow and the first instability (critical Reynolds number, wavenumber and angular frequency)
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Roland, Caroline. "Formation de micro-jets depuis des défauts de surface dans des échantillons métalliques soumis à des chocs laser." Thesis, Chasseneuil-du-Poitou, Ecole nationale supérieure de mécanique et d'aérotechnique, 2017. http://www.theses.fr/2017ESMA0025/document.
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Lorsqu’un matériau solide est soumis à un chargement dynamique (par l’impact d’un projectile, la détonation d’un explosif ou l’irradiation par un laser intense), il se forme une onde de choc, qui se propage dans le matériau depuis la surface chargée. Si cette onde débouche sur une surface libre comportant des défauts géométriques tels que des rugosités, des rayures ou des cavités, son interaction avec ces défauts conduit à l’éjection, sous forme de jets de matière, de débris dont la taille caractéristique est de l’ordre du micromètre et dont la vitesse est typiquement de quelques km/s. La maîtrise de ce processus, appelé microjetting ou micro-éjection, est essentielle pour de nombreuses applications (conception de blindage, découpe pyrotechnique, usinage à très haute vitesse, expériences de Fusion par Confinement Inertiel…). Dans le cadre de cette thèse, menée en collaboration avec le centre CEA de Bruyères-le-Châtel, ce phénomène est étudié dans quatre métaux (Aluminium, Etain, Cuivre et Plomb) à partir de rainures calibrées de deux types : triangulaires isolées de demi-angles d’ouverture contrôlés (20°, 30° et 45°) ou sinusoïdales périodiques. Les influences du matériau, de la forme et de l’ouverture des défauts, de la pression de choc et de l’état du milieu (solide ou fondu sous choc ou en détente) sur les propriétés balistiques des éjectas (vitesses de jet, distribution en taille et densité surfacique des débris constituant les jets) sont évaluées via trois approches complémentaires : expérimentale, théorique et numérique.L’étude expérimentale comporte plusieurs campagnes de chocs laser, effectuées sur l’installation LULI2000 du Laboratoire pour l’Utilisation des Lasers Intenses (Ecole Polytechnique, Palaiseau), avec plusieurs techniques de diagnostic : Ombroscopie Transverse, Vélocimétrie Hétérodyne, radiographie X rapide in-situ, récupération d’éjectas dans des gels (analysés ensuite en microtomographie). Les résultats sont confrontés à des prédictions théoriques (hydrodynamique des chocs obliques et des charges creuses pour les rainures triangulaires, instabilités de Richtmyer-Meshkov pour les rainures sinusoïdales). Enfin, les simulations numériques réalisées avec le code Radioss utilisent deux approches complémentaires : les Eléments Finis Lagrangiens et la formulation SPH (Smoothed Particles Hydrodynamics), encore très peu appliquée au microjetting, plus empirique que la première mais mieux adaptée aux grandes déformations dans les jets et permettant d’accéder à des distributions de tailles de fragmentsWhen a dense material is subjected to a dynamic load (such as projectile impact, explosive detonation or irradiation by a high energy laser beam), a shock wave propagates from the loaded surface. If this shock wave interacts with a free surface with geometrical defects such as grooves, scratches or cavities, it can lead to the ejection of micrometric debris with typical velocities of a few km/s. Understanding this microjetting process is a key issue for many applications, including shielding design, pyrotechnics, high-speed machining and Inertial Confinement Fusion experiments.In this work in collaboration with the CEA-DIF at Bruyères-le-Châtel, this phenomenon is studied under laser-driven shock loading in four materials (Aluminum, Tin, Copper and Lead) with calibrated grooves of two types: isolated triangular profile with controlled aperture half-angles (20°, 30° and 45°) or periodic sinusoidal shape. The influences of the material, of the geometry of the defects, of the shock pressure and of the state of matter (solid or melted under shock or release wave) on the ballistic properties of the ejecta (jet velocity, size distribution and areal mass of the debris constituting the jet) are investigated with three complementary approaches: experimental, theoretical and numerical.The experimental study involves several campaigns performed at the LULI2000 facility of the Laboratoire pour l’Utilisation des Lasers Intenses (Ecole Polytechnique, Palaiseau) and complementary diagnostic techniques: Transverse Shadowgraphy, Heterodyne Velocimetry, fast in situ X-ray radiography, recovery of the ejecta in a gel followed by microtomography. The results are compared with theoretical predictions (2D shocks and shaped charges hydrodynamics for the triangular grooves, Richtmyer-Meshkov Instabilities for the sinusoidal grooves). Then, numerical simulations are performed with the Radioss code with two complementary approaches: the Lagrangian Finite Elements and the SPH (Smoothed Particles Hydrodynamics) formulation, still very scarcely applied to microjetting, more empirical than the first approach but more suitable to the high strains in the jets and allowing access to size distributions of the debris
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Lyra, Wladimir. "Turbulence-Assisted Planetary Growth : Hydrodynamical Simulations of Accretion Disks and Planet Formation." Doctoral thesis, Uppsala universitet, Institutionen för fysik och astronomi, 2009. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-9537.
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The current paradigm in planet formation theory is developed around a hierarquical growth of solid bodies, from interstellar dust grains to rocky planetary cores. A particularly difficult phase in the process is the growth from meter-size boulders to planetary embryos of the size of our Moon or Mars. Objects of this size are expected to drift extremely rapid in a protoplanetary disk, so that they would generally fall into the central star well before larger bodies can form. In this thesis, we used numerical simulations to find a physical mechanism that may retain solids in some parts of protoplanetary disks long enough to allow for the formation of planetary embryos. We found that such accumulation can happen at the borders of so-called dead zones. These dead zones would be regions where the coupling to the ambient magnetic field is weaker and the turbulence is less strong, or maybe even absent in some cases. We show by hydrodynamical simulations that material accumulating between the turbulent active and dead regions would be trapped into vortices to effectively form planetary embryos of Moon to Mars mass. We also show that in disks that already formed a giant planet, solid matter accumulates on the edges of the gap the planet carves, as well as at the stable Lagrangian points. The concentration is strong enough for the solids to clump together and form smaller, rocky planets like Earth. Outside our solar system, some gas giant planets have been detected in the habitable zone of their stars. Their wakes may harbour rocky, Earth-size worlds.
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Guha, Anirban. "Two dimensional hydrodynamic instabilities in shear flows." Thesis, University of British Columbia, 2013. http://hdl.handle.net/2429/44571.
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Hydrodynamic instabilities occurring in two dimensional shear flows have been investigated.
First, the process of resonant interaction between two progressive interfacial waves is studied. Such interaction produces exponentially growing instabilities in idealized, homogeneous or density stratified, inviscid shear layers. It is shown that two oppositely propagating interfacial waves, having arbitrary initial amplitudes
and phases, eventually phase-lock, provided they satisfy a particular condition. Three types of shear instabilities - Kelvin Helmholtz, Holmboe and Taylor have been studied. The above-mentioned condition provides a range of unstable wavenumbers for each instability type, and this range matches the predictions of the canonical normal-mode based linear stability theory.
The non-linear evolution of Kelvin-Helmholtz (KH) instability has been studied. The commonly known manifestation of KH is in the form of spiral billows. However, KH evolving from a piecewise linear shear layer is remarkably different; it is characterized by elliptical vortices of constant vorticity connected via thin braids. Using direct numerical simulation and contour dynamics, it is shown that the interaction between two counter-propagating vorticity waves is solely responsible for this KH formation. The oscillation of the vorticity wave amplitude, the rotation and nutation of the elliptical vortex, and straining of the braids have been investigated.
Finally, the linear stability of plane Couette-Poiseuille flow in the presence of a cross-flow is studied. The base flow is characterized by the cross flow Reynolds number, Reinj and the dimensionless wall velocity, k. Corresponding to each dimensionless wall velocity, k ∈ [0,1], two ranges of Reinj exist where unconditional stability is observed. In the lower range of Reinj , for modest k we have a stabilization of long wavelengths leading to a cut-off Reinj.
As Reinj is increased, we see first destabilization and then stabilization at very large Reinj. Analysis of the eigenspectrum suggests the cause of instability is due to resonant interactions of Tollmien-Schlichting waves.
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Mackerrell, O. S. "Some hydrodynamic instabilities of boundary layer flows." Thesis, University of Exeter, 1988. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.381355.
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Kaiser, Thomas. "Impact of Flow Rotation on Flame Dynamics and Hydrodynamic Stability." Thesis, Toulouse, INPT, 2019. http://oatao.univ-toulouse.fr/24115/1/Kaiser_Thomas.pdf.
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This thesis investigates large scale flow rotation in two configurations. In the first, the effect of flow rotation on a laminar flame is investigated. The flame is anchored in the wake of a cylindrical bluff body. The flow rotation is introduced by turning the cylinder along its axis. It is shown by Direct Numerical Simulation (DNS), that the cylinder rotation breaks the symmetry of both flame branches. Flame Transfer Function (FTF) measurements performed by the Wiener-Hopf Inversion suggest, that low rotation rates lead to deep gaps in the gain and the flame becomes almost insensitive to acoustic perturbation at a specific frequency. It furthermore is demonstrated that this decrease in gain of the FTF is due to destructive interference of the heat release signals caused by the two flame branches. The frequency at which the gain becomes almost zero can be adjusted by tuning the cylinder rotation rate. The study suggests that controlling the symmetry of the flame could be a tool of open-loop control of thermoacoustic instabilities.
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Kifonidis, Konstantinos. "Nucleosynthesis and hydrodynamic instabilities in core collapse supernovae." [S.l. : s.n.], 2000. http://deposit.ddb.de/cgi-bin/dokserv?idn=962128457.
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Forth, Shaun Anthony. "Morphological and hydrodynamic instabilities in undirectional alloy solidification." Thesis, University of Bristol, 1989. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.292481.
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D'Hernoncourt, Jessica. "Influence of thermal effects and electric fields on fingering of chemical fronts: a theoretical study." Doctoral thesis, Universite Libre de Bruxelles, 2007. http://hdl.handle.net/2013/ULB-DIPOT:oai:dipot.ulb.ac.be:2013/210607.
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Several types of instability can affect the interface between two fluids. For instance, a Rayleigh-Taylor instability (or density fingering) is encountered when a heavier fluid is placed upon a lighter one in the gravity field and double diffusive instabilities can be triggered by differential diffusivity of the different species present in the fluid. In this context our work aims to understand theoretically in which way a chemical reaction can induce and influence such instabilities in a fluid initially at rest.
To understand the dynamics resulting from the coupling between chemical reactions and hydrodynamical instabilities we use chemical fronts as model systems. These fronts result from the coupling between autocatalytical chemical reactions and diffusion and they allow to create a self-organized interface between the products and the reactants. As during a chemical reaction the density may vary due to solutal and thermal effects, the products and the reactants can have different densities which may trigger convection movements leading to the destabilization of the fronts.
We have in particular studied the influence of the exothermicity of the reaction on the fingering of chemical fronts, focusing first on the influence of heat losses through the walls of the set-up.
These leaks have a marked influence on the dynamics because they affect the temperature profiles and hence the density profiles too. We have also classified the various types of instabilities that may appear dues to solutal and thermal effects. We have found a new type of hydrodynamic instability of statically stable fronts induced by the chemical reaction.
We have furthermore analyzed an isothermal model with two chemical species. If they diffuse at different rates the front can be subject to diffusive instabilities as well. We have shown that the coupling between such a diffusive instability and fingering can trigger complex dynamics. We have eventually studied the influence of an external electric field on the diffusive instabilities and on fingering underlying the possibility to destabilize otherwise stable fronts./
Différents types d'instabilités hydrodynamiques peuvent affecter les interfaces entre deux fluides comme par exemple, une instabilité de Rayleigh-Taylor (ou digitation de densité) quand un fluide plus dense se trouve placé au-dessus d'un fluide moins dense dans le champ de gravité ou des instabilités de double diffusion induites par des différences entre les diffusivités d'un soluté et de la chaleur contenus dans les fluides. Dans ce contexte, notre thèse s'attache à comprendre de manière théorique comment une réaction chimique peut influencer ces instabilités voire les générer dans un fluide initialement au repos. Pour étudier les dynamiques résultant du couplage entre réactions chimiques et instabilités hydrodynamiques, nous utilisons des systèmes modèles: les fronts chimiques de conversion résultant de la compétition entre réactions chimiques autocatalytiques et diffusion créant une interface auto-organisée entre les réactifs et les produits. Comme au cours d'une réaction chimique la densité peut varier par des effets solutaux et thermiques, les produits et les réactifs de densités différentes peuvent générer des mouvements de convection qui conduisent à la déstabilisation des fronts.
Nous avons en particulier étudié l'influence de l'exothermicité de la réaction sur les instabilités de digitation de fronts chimiques, en nous focalisant dans un premier temps sur l'influence des pertes de chaleur par les parois du réacteur.
Ces fuites ont un effet marqué sur les instabilitités car elles affectent les profils de température et donc les profils de densité dans le système. Nous avons également classifié les différentes instabilités qui peuvent apparaître via des changements de densité dûs à des effets thermiques et solutaux et mis en évidence un nouveau type de déstabilisation hydrodynamique de fronts statiquement stables induit par une réaction chimique.
Nous avons ensuite analysé un modèle isotherme impliquant deux espèces chimiques. Si ces dernières diffusent a des vitesses différentes le front peut être sujet à une instabilité diffusive. Nous avons montré qu'un couplage entre une telle instabilité diffusive et de la digitation peut être à l'origine de dynamiques complexes. Nous avons ensuite considéré l'influence d'un champ électrique sur les instabilité diffusives et de digitation en soulignant la possibilié de déstabiliser via ce champ des fronts initialement stables.
Doctorat en Sciences
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Sandin, Christer. "A Study of Grain Drift in C Stars : Theoretical Modeling of Dust-Driven Winds in Carbon-Rich Pulsating Giant Stars." Doctoral thesis, Uppsala : Acta Universitatis Upsaliensis : Univ.-bibl. [distributör], 2003. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-3397.
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Marston, Jeremy Oliver. "Hydrodynamic assist, hysteresis and non-uniqueness of instabilities in curtain coating." Thesis, University of Birmingham, 2008. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.502201.
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Bridel-Bertomeu, Thibault. "Investigation of unsteady phenomena in rotor/stator cavities using Large Eddy Simulation." Thesis, Toulouse, INPT, 2016. http://oatao.univ-toulouse.fr/17867/1/BRIDEL_BERTOMEU.pdf.
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This thesis provides a numerical and theoretical investigation of transitional and turbulent enclosed rotating flows, with a focus on the formation of macroscopic coherent flow structures. The underlying processes are strongly threedimensional due to the presence of boundary layers on the discs and on the walls of the outer (resp. inner) cylindrical shroud (resp. shaft). The complexity of these flows poses a great challenge in fundamental research however the present work is also of importance for industrial rotating machinery, from hard-drives to space engines turbopumps - the design issues of the latter being behind the motivation for this thesis. The present work consists of two major investigations. First, industrial cavities are modeled by smooth rotor/stator cavities and therein the dominant flow dynamics is investigated. For the experimental campaigns on industrial machinery revealed dangerous unsteady phenomena within the cavities, the emphasis is put on the reproduction and monitoring of unsteady pressure fluctuations within the smooth cavities. Then, the LES of three configurations of real industrial turbines are conducted to study in situ the pressure fluctuations and apply the diagnostics already vetted on academic problems.
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Negretti, Maria Eletta. "Hydrodynamic instabilities and entrainment in two-layer stratified flows down a slope." Karlsruhe : Univ.-Verl. Karlsruhe, 2007. http://d-nb.info/985610263/34.
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Jones, Samuel Edward. "Symmetries in the kinematic dynamos and hydrodynamic instabilities of the ABC flows." Thesis, University of Exeter, 2013. http://hdl.handle.net/10871/14689.
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This thesis primarily concerns kinematic dynamo action by the 1:1:1 ABC flow, in the highly conducting limit of large magnetic Reynolds number Rm. The flow possesses 24 symmetries, with a symmetry group isomorphic to the group O24 of orientation-preserving transformations of a cube. These symmetries are exploited to break up the linear eigenvalue problem into five distinct symmetry classes, which we label I-V. The thesis discusses how to reduce the scale of the numerical problem to a subset of Fourier modes for a magnetic field in each class, which then may be solved independently to obtain distinct branches of eigenvalues and magnetic field eigenfunctions. Two numerical methods are employed: the first is to time step a magnetic field in a given symmetry class and obtain the growth rate and frequency by measuring the magnetic energy as a function of time. The second method involves a more direct determination of the eigenvalue using the eigenvalue solver ARPACK for sparse matrix systems, which employs an implicitly restarted Arnoldi method. The two methods are checked against each other, and compared for efficiency and reliability. Eigenvalue branches for each symmetry class are obtained for magnetic Reynolds numbers Rm up to 10^4 together with spectra and magnetic field visualisations. A sequence of branches emerges as Rm increases and the magnetic field structures in the different branches are discussed and compared. All symmetry classes are found to contain a dynamo, though dynamo effectiveness varies greatly between classes, suggesting that the symmetries play an important role in the field amplification mechanisms. A closely related problem, that of linear hydrodynamic stability, is also explored in the limit of large Reynolds number Re. As the same symmetry considerations apply, the five symmetry classes of the linear instability can be resolved independently, reducing the size of the problem and allowing exploration of the effects of the symmetries on instability growth rate. Results and visualisations are obtained for all five classes for Re up to 10^3, with comparisons drawn between the structures seen in each class and with those found in the analogous magnetic problem. For increasing Re, multiple mode crossings are observed within each class, with remarkably similar growth rates seen in all classes at Re=10^3, highlighting a lack of dependence on the symmetries of the instability, in contrast with the magnetic problem. This thesis also investigates the problem of large-scale magnetic fields in the 1:1:1 ABC flow through the introduction of Bloch waves that modify the periodicity of the magnetic field relative to the flow. Results are found for a field with increased periodicity in a single direction for Rm up to 10^3; it is established that the optimal scale for dynamo action varies as Rm increases, settling on a consistent scale for large Rm. The emerging field structures are studied and linked with those of the original dynamo problem. On contrasting this method with a previous study in which the flow is instead rescaled, it is shown that the use of Bloch waves drastically increases the range of possible scales, whilst cutting required computing time. Through a multiple-scale analysis, the contribution from the alpha-effect is calculated for the 1:1:1 ABC flow and is seen in growth rates for Rm << 1.
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Junk, Veronika. "Hydrodynamical instabilities and the trace of dark energy within the CMB." Diss., lmu, 2010. http://nbn-resolving.de/urn:nbn:de:bvb:19-133349.
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Paré, Gounséti Nimonoka. "Création et éjection des gouttes de l'atomisation." Thesis, Paris 6, 2015. http://www.theses.fr/2015PA066318/document.
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Cette thèse traite des instabilités hydrodynamiques survenant dans les ligaments liquides en présence d’écoulement axial, afin de comprendre la formation des gouttes lors des processus d’atomisation. Il a été montré par des études précédentes que tout processus d’atomisation passe par l’étape de la formation des ligaments, qui se déstabilisent en gouttelettes. Le processus de fragmentation des ligaments est régi par deux instabilités : l’instabilité de Rayleigh-Plateau lorsque le ligament est infini, le phénomène du « end pinching », lorsque le ligament est semi-infini. Dans les deux cas le mécanisme responsable du pincement du ligament est la capillarité. Dans cette thèse, nous avons montré que, sous certaines conditions, le pincement du ligament peut être retardé ou évité : c’est le phénomène d’évitement de l’étranglement. Une exploration détaillée de la zone de constriction du ligament (là où le rayon est minimal), révèle des effets non linéaires liés à la viscosité du fluide : la couche visqueuse se développe, s’enroule puis décolle de l’interface sous forme de jet, en aval du cou avec formation d’anneau tourbillonnaire. L’écoulement dans cette zone du ligament est soumis à une accélération axiale correspondant à une baisse de la pression : c’est l’effet Venturi. Ce type d’écoulement a été étudié à travers l’instabilité du pont capillaire entre deux tubes, soumis à un écoulement axial. Tout au long de ces travaux, deux approches ont été utilisées : les simulations numériques et des observations expérimentales. L’essentiel des résultats présentés a fait l’objet de publication ou d’une soumission d’articleThis thesis deals with the hydrodynamic instabilities which occur in a liquid ligament in presence of axial flow. We investigate the formation of drops during the atomization process. Previous studies highlighted a common step to all types of atomization processes: the initial formation of the ligament which later evolves into droplets. The ligaments fragmentation process is governed by two possible instabilities: the “Rayleigh-Plateau” instability which is characteristic of an infinite ligament and the “end-pinching” phenomenon, which occurs in semi-infinite ligaments. In both cases, capillarity is the driving mechanism underlying the ligament segmentation. In this thesis we show that, under certain conditions, the liquid ligament can surprisingly escape from pinch-off through creation of a vortex ring (“escape phenomenon”). A detailed analysis of the constriction zone (neck of the ligament) during the “escape phenomenon” suggested that nonlinear effects associated to fluid viscosity might play an important role in the escape process. Both our experimental observations and numerical results confirmed the occurrence of the detachment of the viscous layer into a jet downstream of the neck through creation of a vortex ring, when fluid viscosity exceeds a threshold. Accordingly, the fluid in the constriction zone undergoes an axial acceleration associated to a decrease in the pressure: this is the so-called “Venturi effect”. This type of flow is characteristic of the instability which emerges at the capillary bridge between two tubes subjected to axial flow. Part of the results obtained were the subject of a publication or article submission
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Pagani, Bruno. "Explosion asymétrique des supernovæ gravitationnelles." Thesis, Université Paris-Saclay (ComUE), 2019. http://www.theses.fr/2019SACLS244.
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L’histoire de l’observation des supernovæ remonte à plusieurs millénaires, mais cela fait moins de cent ans que l’on sait que certaines d’entre elles marquent la fin de vie des étoiles massives. L’effondrement gravitationnel du cœur de fer de ces étoiles peut conduire à la formation d’une étoile à neutrons et au déclenchement d’une de ces explosions spectaculaires, ainsi appelées supernovæ gravitationnelles. Les mécanismes à l’œuvre dans la région la plus interne de l’étoile durant les quelques centaines de millisecondes suivant l’effondrement initial jouent un rôle clé dans le succès ou non de l’explosion. En particulier, les instabilités multi-dimensionnelles telles que l’instabilité du choc d’accrétion stationnaire (SASI) ou la convection induite par les neutrinos sont susceptibles d’augmenter efficacement le chauffage de la matière par les neutrinos émis depuis la proto-étoile à neutrons et de donner lieu à des explosions fortement asymétriques.Dans cette thèse, ces phénomènes sont étudiés à l’aide de simulations numériques d’un modèle simplifié à deux dimensions. Cela permet une vaste exploration de l’espace des paramètres qui serait inaccessible pour les modèles plus réalistes.La frontière entre explosion et effondrement en trou noir est déterminée dans un espace à trois paramètres que sont la rotation stellaire, le chauffage par les neutrinos et le taux d’accrétion — qui est relié à la masse du progéniteur. La surface critique ainsi définie permet de caractériser l’impact des instabilités multi-dimensionnelles sur le seuil d’explosion. Les effets de la rotation sont importants pour les modèles présentant un faible taux d’accrétion. Ces résultats permettent de réconcilier ceux de différents modèles réalistes. Le caractère stochastique des résultats à proximité de la transition est mis en évidence ; celui-ci est d’autant plus important que la rotation et le taux d’accrétion sont faibles. Les différents chemins vers l’explosion observés dans nos simulations sont décrits et illustrés par l’analyse d’un échantillon emblématique de modèles. Les rôles respectifs des différentes instabilités et leurs signatures sont discutés.L’ensemble des ∼600 simulations réalisées constitue une base offrant de nombreuses perspectives d’analyses futuresThe observational history of supernovæ dates back to several millennia, but it has been less than one hundred years since we know that some of them mark the death of massive stars. The gravitational collapse of the iron core at the centre of those stars can lead to the birth of a neutron star and the onset of one of those spectacular explosions, thus called core-collapse supernovæ. The mechanisms at work in the innermost part of the star during the first few hundred milliseconds after the initial collapse play a key role in the success or the failure of the explosion. In particular, multi-dimensional instabilities like the standing accretion shock instability (SASI) or the neutrino-driven convection are likely to increase efficiently the matter heating by neutrinos emitted from the proto-neutron star and yield highly asymmetric explosions.In this thesis, those phenomena are studied with the help of numerical simulations of a simplified two dimensional model. This allows for a vast exploration of the parameter space that would be unreachable for more realistic models.The boundary between explosion and collapse into a black hole is established in a three parameter space, namely the stellar rotation, the neutrino heating and the accretion rate —which relates to the progenitor mass. The critical surface so defined allows us to characterise the impact of multi-dimensional instabilities on the explosion threshold. The effects of rotation are important for models with a low accretion rate. These results allow us to reinterpret the seemingly contradictory results of more realistic models. The stochasticity of the results near the explosion threshold is highlighted. This effect is more pronounced for low rotation and accretion rates. The different paths to explosion observed in our simulations are described and illustrated with the analysis of a representative sample of models. The respective roles of the different instabilities and their signatures are discussed.The set of ∼600 simulations constitutes a database offering numerous perspectives for future analysis
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Kokkonen, Toni. "CFD analysis of stepped planing vessels." Thesis, KTH, Mekanik, 2018. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-250023.
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High speed planing hulls are currently widely used for example in recreational and emergency vessel applications. However, very little CFD research has been done for planing vessels, especially for those with stepped hulls. A validated CFD method for planing stepped hulls could be a valuable improvement for the design phase of such hulls. In this thesis, a CFD method for stepped hulls, with a primary focus on two-step hulls, is developed using STAR-CCM+. As a secondary objective, porpoising instability of two-step hulls is investigated. The simulations are divided into two parts: In the first part a method is developed and validated with existing experimental and numerical data for a simple model scale planing hull with one step. In the second part the method is applied for two two-step hulls provided with Hydrolift AS. A maximum two degrees of freedom, trim and heave, are used, as well as RANS based k-w SST turbulence model and Volume of Fluid (VOF) as a free surface model. The results for the one-step hull mostly corresponded well with the validation data. For the two-step hulls, validation data did not exists and they were first simulated with a fixed trim and sinkage and compered between each other. In the simulations with free trim and heave both hulls experienced unstable porpoising behavior.
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Gandikota, Vs Gurunath. "Instabilités d'interfaces fluides en apesanteur spatiale lors d'un changement brutal ou périodique d'accélération." Thesis, Grenoble, 2013. http://www.theses.fr/2013GRENY036/document.
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L'étude du comportement d'un fluide proche de son point critique et soumis à des vibrations ou une variation rapide de gravité/acceleration est un sujet extrêmement intéressant. Les phénomènes physiques impliqués sont d'un grand intérêt non seulement pour la physique fondamentale mais aussi pour l'industrie spatiale. Dans cette thèse, trois problèmes sont principalement trait&s: (i) Etude de l'interaction de vibrations harmoniques avec une couche limite thermique dans un fluide supercritique en absence de gravité, (ii) Etude de l'interaction de vibrations avec une interface liquide/vapeur d'un fluide sous−critique sous plusieurs niveaux de gravité (les instabilités de Faraday et d'onde gelée, l'équilibre dynamique d'une interface) et (iii) Etude du phénomène de geyser à l'intérieur d'un réservoir partiellement rempli d'oxygène lorsqu'il est soumis à une variation rapide de la gravité (ou accélération). La thèse comporte une partie expérimentale et une partie numérique. Des expériences ont été réalisées sur les installations HYLDE et OLGA du CEA Grenoble utilisant respectivement les fluides H2 et O2 dans la zone sous−critique. Des simulations numériques sont réalisées pour étudier la stabilité d'une couche limite thermique et la dynamique d'une interface fluide soumise à une variation rapide de la gravité en utilisant des codes numériques basées sur le méthode volumes finis utilisant les algorithmes SIMPLER et VOF−PLIC respectivement. Plusieurs résultats intéressants ont été obtenus. Différents phénomènes ont été étudiés et quantifiés, comme l'instabilité de Faraday et l'instabilité d'onde gelée dans le domaine sous−critique et l'instabilité parametrique et l'instabilité Rayleigh−vibrationnelle dans le domaine supercritique. Les expériences ont permis de bien comprendre les raisons de la transition de l'instabilité de Faraday vers une structuration en bandes verticales très près du point critique. Les expériences et les simulations numériques sur le phénomène de geyser ont aidé à développer des corrélations empiriques pour les vitesses de la bulle et du geyser en prenant en compte les effets des paroisThe behavior of a near-critical fluid subjected to vibration or a rapid variation of acceleration is an extremely interesting topic of research. The resulting physical phenomena are of great interest in view of the fundamental physics involved and have great relevance to the space industry. The thesis addresses mainly three problems: (i) study of the interaction of harmonic vibration with a thermal boundary layer of a supercritical fluid under the absence of gravity, (ii) study of the inter- action of vibration with the liquid−vapor interface of a near−critical fluid under various gravity levels (Faraday and frozen wave instabili- ties, dynamic equilibrium of the interface) (iii) study of the geysering phenomenon inside a reservoir partially filled with a liquid when it is subjected to a rapid variation of gravity. Experiments are conducted onboard the zero−g installations HYLDE and OLGA developed by CEA Grenoble using H2 and O2 as the work- ing fluids. Numerical simulations are carried out using finite volume codes based on SIMPLER (for the problem involving the supercriti- cal fluid) and VOF−PLIC (for the interface dynamics problem under rapid variation of gravity). New and interesting results have been obtained. Various phenom- ena like the Faraday instability and the frozen wave instability in the sub−critical region and the parametric instability and the Rayleigh−vibrational instability in the supercritical region have been quantified. The experiments have successfully explained the reason behind the transition of the Faraday instability into vertical band pattern very close to the critical point. Experiments and numerical simulation of the geysering phenomenon have helped to evolve empir- ical correlations for the bubble rise and geyser edge velocities taking into account the effect of walls on these velocities
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McGlinchey, Kristopher. "Radiation-hydrodynamic simulations of the impact of instabilities and asymmetries on inertial confinement fusion." Thesis, Imperial College London, 2017. http://hdl.handle.net/10044/1/57027.
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In recent years, there has been significant progress towards achieving ignition from controlled thermonuclear fusion. Recent experiments at the National Ignition Facility have come close to achieving this, but the performance of experiments were compromised by perturbations affecting the implosion's symmetry. This thesis presents the implementation of a multigroup radiation transport algorithm into an existing hydrodynamics code, Chimera, and its application to Inertial Confinement Fusion (ICF) to investigate these perturbations. An idealised 1-dimensional implosion was simulated to explore how the shock timing and final drive affected the stagnation conditions of a capsule's implosion. The timing of the shocks played a critical role in controlling the adiabat of the implosion, with the initial shock being most important by setting the mass that enters the forming hotspot. Multidimensional simulations then evaluated how perturbations affected an implosion's performance. Hydrodynamic instabilities from harmonic and natural roughness seeds were imaged, and the requirements of a next generation imaging system derived. It was found that a new system will require a 10keV backlighter at a < 10 micron spatial and a < 20 ps temporal resolution. The radiation from the forming hot spot played an important role in fire polishing incoming instabilities, leading to a denser, cooler hot spot which lowered the yield by 50%. Large-scale asymmetries caused by radiation asymmetries prematurely ended the hotspot confinement due to imploding lobes of cold dense material, reducing the yield by 50%. Neutron detectors found a 10% variation in inferred ion temperature due to the residual flows induced. The tent scar had a small influence on the performance of a capsule, being confined largely to the surface. The combination of the tent and radiation asymmetries produced a highly perturbed implosion that performed better than the radiation asymmetry, but worse than the tent.
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Tun, Yarzar. "Nonmodal Analysis of Temporal Transverse Shear Instabilities in Shallow Flows." Thesis, Université d'Ottawa / University of Ottawa, 2017. http://hdl.handle.net/10393/36886.
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Shallow flows are those whose width is significantly larger than their depth. In these types of flows, two dimensional coherent structures can be generated and can influence the flow greatly by the lateral transfer of mass and momentum. The development of coherent structures as a result of flow instabilities has been a topic of interest for environmental fluid mechanics for decades. Studies on the use of linear modal stability analysis is commonly found in literature. However, the relatively recent development in the field of hydrodynamic stability suggests that the traditional linear modal stability analysis does not describe the behaviour of the perturbations in finite time. The discrepancy between asymptotic behaviour and finite time behaviour is particularly large in shear driven flows and it is most likely to be the case for shallow flows. This study aims to provide a better understanding of finite time growth of perturbation energy in shallow flows. The three cases of shallow flows evaluated are the mixing layer, jet and wake. The critical cases are obtained through the linear modal analysis and nonmodal analysis was conducted to show the transient behaviour in finite time for what is so-called marginally stable. Finally, the thesis concludes by generalizing the finite time energy growth in the S-k space.
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Surville, Clément. "Morphologie et évolution des tourbillons de Rossby bidimensionnels dans les disques protoplanétaires." Thesis, Aix-Marseille, 2013. http://www.theses.fr/2013AIXM4784/document.
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Le rôle des tourbillons anticycloniques dans l'évolution des disques protoplanétaires et, en particulier, dans les mécanismes de formation des planétésimaux, est au coeur des défis actuels de l'astrophysique moderne. C'est pourquoi une étude approfondie de leur structure et de leur dynamique est primordiale.Grâce à un outil numérique spécifiquement développé pour l'étude des disques, nous avons revisité l'Instabilité en Ondes de Rossby dans le régime non linéaire, et découvert l'existence d'une cascade des modes de perturbation qui permet de mieux comprendre la formation des tourbillons par cette instabilité.Leur structure à été décrite par un modèle gaussien innovant, remarquablement en accord avec les résultats numériques. Grâce à un échantillon de près de 300 tourbillons, nous avons borné le domaine des dimensions radiales, azimutales et de la vorticité. Deux familles de tourbillons possibles ont été distinguées : (i) les tourbillons incompressibles, stables et quasi-stationnaires; (ii) les tourbillons compressibles, très mobiles et associés à l'émission d'ondes de densité. Leur persistance sur plus de 1000 rotations confirme l'observabilité de tous ces tourbillons. Enfin, nous avons caractérisé leur migration vers l'étoile en fonction de leur géométrie, du gradient de pression et de l'échelle de hauteur du disque. Pour la première fois, une expression analytique permet d'estimer le taux de migration en fonction de ces paramètres; l'échelle de temps pour tomber sur étoile peut aller de 10^6 à 100 rotations. Suivant un modèle de viscosité alpha, la perte de moment cinétique pourrait être suffisante pour maintenir un taux d'accrétion significatif dans la zone morteThe role of anticyclonic vortices in the protoplanetary disk evolution and in how do planetesimals form are among the most important chalenges of the modern astrophysics. That is why an exhaustive study of the structure and the evolution of these vortices is necessary.Thanks to a numerical code specificly designed for the study of these disks, we have revisited the Rossby Wave Instability in the nonlinear regime, and have discovered that a cascade of the perturbation modes can explain the formation of the vortices created by this instability.We have described the structure of these Rossby vortices with a new gaussian vortex model, which accurately fits the numerical results. A sample of 300 different vortices led us to define the bondaries of the radial and azimuthal extent as well as the vorticity of the vortices. We have distinguished two main families : (i) the incompressible family, which is stable and quasi stationnary ; (ii) the compressible family, moving and exciting density waves. We found them surviving more than 1000 orbits, a clear confirmation of their observability.Finaly, we have caracterized the inward migration of the vortices as a fonction of their shape, their vorticity, but also of the pressure gradient and the scale height of the disk. For the first time, we exhibit a equation relating the migration rate to these parameters. The time scale of the migration ranges from 10^6 to just 100 rotations of the disk. Extremely steep pressure gradients are needed to reverse the migration to an outward regime. Following the alpha viscosity approch, the loss of kinetic momentum due to this migration would be sufficient to sustain the accretion in the dead zone
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Lorenzani, Silvia. "Fluid instabilities in precessing ellipsoidal shells." [S.l. : s.n.], 2001. http://deposit.ddb.de/cgi-bin/dokserv?idn=964398702.
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Keiser, Ludovic. "Formation et déplacement de gouttes confinées : Instabilités et dynamiques." Thesis, Sorbonne Paris Cité, 2018. http://www.theses.fr/2018USPCC080/document.
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Les écoulements biphasiques en milieux poreux sont généralement accompagnés par des phénomènes d'émulsification d'une phase dans l'autre. Les causes peuvent être nombreuses, de la digitation visqueuse aux instabilités purement capillaires. Cette thèse expérimentale a pour objet l'étude d'un mécanisme particulier d'émulsification de l'huile en milieu poreux, ainsi que le transport des gouttes produites dans des milieux confinés. Dans la première partie de cette thèse, l'instabilité gravito-capillaire de Rayleigh-Taylor est revisitée dans un coin formé entre deux plaques de verre centimétriques. La présence d'un gradient de confinement introduit une force capillaire supplémentaire à cette instabilité canonique, susceptible de stabiliser une couche de liquide suspendue au-dessus du vide. Le seuil de stabilité, les longueurs d'onde caractéristiques et les taux de croissance sont bien modélisés par une analyse de stabilité linéaire de l'interface. La caractérisation de cette force capillaire induite par le gradient de confinement nous amène par la suite à l'étude d'une instabilité purement capillaire se produisant lorsqu'un fluide en mouillage très favorable migre vers les régions les plus confinées d'un coin, occupées initialement par un fluide en mouillage moins favorable. Le gradient de confinement introduit alors une force déstabilisante, aboutissant à l'inversion de la position respective des deux phases. Le liquide le moins mouillant est complètement émulsifié et transporté vers les régions les moins confinées sous la forme de gouttelettes. Une analyse de stabilité linéaire de l'interface permet, là encore, de prédire cette sélection de taille. Les taux de croissance mesurés ne sont en revanche pas en accord avec la modélisation, basée sur la loi de Darcy. Leur valeur suggère une localisation de la dissipation visqueuse dans les lignes de contact déplacées durant le développement de l'instabilité, ainsi que dans les films de lubrification également déposés. Ces dynamiques "non-darciennes" nous ont amenés dans une seconde partie de la thèse à l'étude du transport de gouttes d'huile très visqueuses confinées dans de l'eau en mouillage total. Dans cette configuration, la présence de films de lubrification d'eau entre la goutte et le substrat assure la localisation de la dissipation dans les films peu visqueux, favorisant ainsi la mobilité des gouttes. Nous montrons également que la présence de rugosités sur les parois du confinement induit un ralentissement significatif de la vitesse des gouttes, lié à l'amincissement du film de lubrification par ces rugosités. L'interdépendance subtile entre friction visqueuse à l'avant de la goutte et dans son volume est notamment mise en lumière. Dans une dernière partie, nous étudions l'instabilité capillaire se produisant lorsqu'une goutte binaire d'eau et d'alcool est déposée à la surface d'un bain d'huile. L'évaporation majoritaire de l'alcool à la surface de la goutte induit des variations locales de la tension de surface. Des écoulements interfaciaux de Marangoni se produisent, et aboutissent à la déstabilisation spectaculaire de la goutte en étalementBiphasic flows in porous media generally lead to the emulsification of one phase into the other. This may be due to several phenomena, such as viscous fingering or pure capillary instabilities. In this experimental thesis, we study a particular emulsifying phenomenon of oil in a model porous medium, as well as the transport of the produced droplets in confined regions. In the first part of the manuscript, the Rayleigh-Taylor instability is revisited in a wedge formed between two centimetric glass plates. The gradient of confinement leads to a capillary force not present in the canonical Rayleigh-Taylor instability. This new force can stabilize liquid layer above air submitted to gravity. The threshold of the instability, the characteristic wavelength and the growth rate are captured by a linear stability analysis of the interface. This characterization of the confinement-induced capillary force drove us to the study of a pure capillary instability occurring when a wetting liquid migrates toward the most confined regions of a wedge, initially filled with a less wetting liquid. The gradient of confinement generates a destabilizing force, leading to the complete inversion of the position of both phases. The less wetting liquid is fully emulsified and the produced droplets are convected towards the less confined regions. A linear stability analysis of the interface here again predicts the characteristic size of the droplets. However, the measured growth rates are not in agreement with the model, based on the Darcy law. This suggests a localization of viscous dissipation in the contact lines displaced during the development of the instability. Another source of viscous dissipation can be in the deposited lubrication films. Those "non-Darcian" dynamics motivated the second part of this thesis, which focuses on the motion of very viscous and non-wetting droplets confined in water. In this configuration, the lubrication film of water between the drop and the substrate ensures the localization of viscous dissipation in those films of low viscosity. This favors the extremely high mobility of the droplets. We also show that wall roughness may induce a thinning of these lubrication films. We shed light on the intricate coupling between viscous friction at the front of the drop and in its bulk. In a last part of this work, we study the capillary instability occurring when a binary droplet of water and alcohol is deposited at the surface of a vegetable oil bath. The dominant evaporation of alcohol at the surface of the drop induces local variations of surface tension. Interfacial Marangoni flows are thus observed, leading to the spectacular destabilization of the spreading droplet
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Lamberts-Marcade, Astrid. "Simulations numériques de collisions de vents dans les systèmes binaires." Thesis, Grenoble, 2012. http://www.theses.fr/2012GRENY038/document.
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L'objectif de cette thèse est de comprendre la structure des binaires gamma, binaires à collision de vents composées d'une étoile massive et d'un pulsar jeune. Ces binaires possèdent probablement une structure similaire aux binaires à collision de vents composées de deux étoiles massives, avec des particularités liées à la nature relativiste du vent de pulsar. L'interaction de deux vents supersoniques d'étoiles massives crée une structure choquée qui présente des signatures observationnelles du domaine radio aux rayons X. Plusieurs instabilités ainsi que le mouvement orbital des étoiles influent sur la structure choquée. Afin de comprendre leur impact, j'ai effectué des simulations à haute résolution de binaires à collision de vents à l'aide du code hydrodynamique RAMSES. Ces simulations sont numériquement coûteuses à réaliser, surtout lorsque un des vents domine fortement l'autre. A petite échelle, les simulations soulignent l'importance de l'instabilité de couche mince non-linéaire dans les collisions isothermes alors que l'instabilité de Kelvin-Helmholtz peut fortement modifier la structure choquée dans une collision adiabatique. A plus grande échelle, cette instabilité peut parfois détruire la structure spirale à laquelle on s'attend si la différence de vitesse entre les vents est trop importante. WR 104 est une binaire dont on observe la structure spirale grâce à l'émission de poussières. Les simulations de ce système montrent un bon accord avec la structure observée et indiquent que des processus de refroidissement du gaz sont nécessaires à la formation de poussières. Pour modéliser les vents de pulsar dans les binaires gamma, RAMSES a été étendu à l'hydrodynamique relativiste. J'utilise ce nouveau code pour réaliser des simulations préliminaires de binaires gamma. Elles montrent effectivement une structure similaire aux binaires stellaires, avec de légères corrections relativistes . Ce code est adapté à l'étude de divers systèmes astrophysiques tels que les jets relativistes, les sursauts gamma ou les nébuleuses de pulsar et fera partie de la prochaine version de RAMSES qui sera rendue publiqueThe aim of this thesis is to understand the structure of colliding wind binaries composed of a massive star and a young pulsar, called gamma-ray binaries. They are expected to display a similar structure to colliding wind binaries composed of massive stars, with some particularities due to the relativistic nature of the pulsar wind. The interaction of the supersonic winds from massive stars creates a shocked structure with observational signatures from the radio domain to the X-rays. The structure is affected by various instabilities and by the orbital motion of the stars. To understand their impact, I carried out high resolution simulations of colliding wind binaries with the hydrodynamical code RAMSES. They are computationally demanding, especially when one of the winds strongly dominates the other one. Small scale simulations highlight the importance of the Non-linear Thin Shell Instability in isothermal collisions while the Kelvin-Helmholtz instability may strongly impact the dynamics of adiabatic collisions. I found that, at larger scales, this instability can destroy the expected large scale spiral structure when there is an important velocity gradient between the winds. WR 104 is a system that displays a spiral structure with important dust emission. The simulation of this system shows a good agreement with the observed structure and indicates cooling processes are necessary to enable dust formation. To model the pulsar wind in gamma-ray binaries, an extension of RAMSES has been developed, that incorporates relativistic hydrodynamics. I used this new relativistic code to perform preliminary simulations of gamma-ray binaries. They display a similar structure to colliding wind binaries with small relativistic corrections. We expect to use this code to perform large scale simulations of gamma-ray binaries. It will be part of the next public release of RAMSES and is suited for the study of many astrophysical problems such as relativistic jets, pulsar wind nebulae or gamma-ray bursts
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Negretti, Maria Eletta [Verfasser]. "Hydrodynamic instabilities and entrainment in two-layer stratified flows down a slope / von Maria Eletta Negretti." Karlsruhe : Univ.-Verl. Karlsruhe, 2007. http://d-nb.info/985610263/34.
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Negretti, Maria Eletta. "Hydrodynamic instabilities and entrainment processes in two-layer density-stratified exchange flows over a submerged sill." [S.l. : s.n.], 2007. http://digbib.ubka.uni-karlsruhe.de/volltexte/1000006966.
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Paquier, Anna. "Génération et croissance des vagues à la surface d’un liquide visqueux sous l’effet du vent." Thesis, Université Paris-Saclay (ComUE), 2016. http://www.theses.fr/2016SACLS183/document.
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Bien qu'ayant suscité de nombreuses études sur le sujet, un certain nombre de questions à propos de la formation des vagues sous l'effet du vent restent sans réponse précise. Dans ma thèse, j'aborde ce problème selon une approche peu explorée : l'étude expérimentale de la déformation sous l'effet du vent de la surface d'un liquide fortement visqueux. En effet, contrairement à la majeure partie de la littérature sur le sujet, le liquide que j'utilise n'est pas de l'eau mais un liquide sensiblement plus visqueux. Indépendamment des questions fondamentales sous-jacentes, cela a en pratique l'avantage de simplifier le problème. En effet, du fait de la forte viscosité du liquide, l'écoulement dans le liquide reste laminaire et les perturbations de l'interface qui ne sont pas amplifiées ne peuvent se propager que sur une distance limitée. Pour observer ces déformations de l'interface liquide-air, j'ai développé un nouveau montage expérimental sur lequel a été mise en œuvre la méthode de visualisation Free Surface Synthetic Schlieren. Cette technique non intrusive a permis de mesurer avec une résolution micrométrique les amplitudes de déformations de la surface et d'accéder aux premières déformations à faible vitesse de vent. Dans un premier temps, les expériences furent conduites sur un liquide trente fois plus visqueux que l'eau. Grâce aux données expérimentales obtenues par FS-SS, deux régimes de déformation de l'interface liquide-air ont été mis en évidence. A vitesse de vent faible, l'interface est recouverte de "wrinkles", des perturbations de faible amplitude désorganisées spatialement et globalement alignées dans le sens de l'écoulement. Ces wrinkles peuvent être interprétés comme l'effet sur l'interface des fluctuations de pression de l'écoulement turbulent d'air. A plus forte vitesse, au-dessus d'une vitesse critique, apparaissent des vagues transverses quasi-parallèles entre elles et perpendiculaire à la direction du vent. Les distinctions entre les deux régimes ont été détaillées et les non-linéarités émergeant au-dessus du seuil ont aussi été étudiées. Par la suite, la viscosité du liquide a été changée sur une large gamme. Il ressort des expériences que les deux régimes de déformation de l'interface sous l'effet du vent peuvent être identifiés pour l'ensemble des viscosités parcourues. Suite à ces résultats, un modèle décrivant l'évolution de l'amplitude des wrinkles en fonction du vent et de la viscosité du liquide a été développéDespite numerous studies on the subject, the development of waves under the action of wind still retains a certain number of open questions. In my PhD, I approach this problem through a fairly uncommon angle: the experimental study of the deformation by wind of the surface of a highly viscous liquid. Indeed, contrary to the major part of the literature on the matter, the liquid I used is not water but a significantly more viscous liquid. Regardless of the fundamental underlying questions, this has the practical advantage of simplifying the problem. Indeed, due to the high viscosity of the liquid, the flow in the liquid stays laminar and the unamplified perturbations of the interface can only propagate over a limited distance. To observe these deformations at the liquid-air interface, I have developed a new experimental set-up upon which the Free Surface Synthetic Schlieren method of visualization was implemented. This non-intrusive technique allowed to measure with a micrometric accuracy the amplitude of the surface deformation and to access the first deformations at low wind velocity. First, experiments were conducted over a liquid thirty times more viscous than water. The experimental data obtained by FS-SS show two regimes of deformation of the liquid-air interface. At low wind velocity, the interface is populated with ``wrinkles'', small-amplitude streamwise spatially disorganized perturbations. These wrinkles can be interpreted as the effect on the interface of the pressure fluctuations in the turbulent wind. At higher windspeed, above a critical velocity, transverse waves appear with quasi-parallel crests perpendicular to the wind direction. The distinctions between the two regimes have been detailed and the nonlinearities emerging above the threshold have also been studied. Then, the viscosity of the liquid has been changed over a large range. It results from the experiments that the two regimes of surface deformation by wind can be identified for all the viscosities explored. Following these results, a model was developed to account for the evolution of the wrinkles' amplitude both with wind velocity and with viscosity
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Junk, Veronika [Verfasser], and Andreas [Akademischer Betreuer] Burkert. "Hydrodynamical instabilities and the trace of dark energy within the CMB / Veronika Junk. Betreuer: Andreas Burkert." München : Universitätsbibliothek der Ludwig-Maximilians-Universität, 2010. http://d-nb.info/1015131158/34.
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