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Search Results: 1 - 10 of 219597 matches for " C. Ruyer "
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Weibel instability-mediated collisionless shocks in laser-irradiated dense plasmas:Prevailing role of the electrons in the turbulence generation
C. Ruyer,L. Gremillet,G. Bonnaud
Physics , 2015, DOI: 10.1063/1.4928096
Abstract: We present a particle-in-cell simulation of the generation of a collisionless turbulent shock in a dense plasma driven by an ultra-high-intensity laser pulse. From the linear analysis, we highlight the crucial role of the laser-heated and return-current electrons in triggering a strong Weibel-like instability, giving rise to a magnetic turbulence able to isotropize the target ions.
Electromagnetic fluctuations and normal modes of a drifting relativistic plasma
C. Ruyer,L. Gremillet,D. Bénisti,G. Bonnaud
Physics , 2013, DOI: 10.1063/1.4829022
Abstract: We present an exact calculation of the power spectrum of the electromagnetic fluctuations in a relativistic equilibrium plasma described by Maxwell-J\"uttner distribution functions. We consider the cases of wave vectors parallel or normal to the plasma mean velocity. The relative contributions of the subluminal and supraluminal fluctuations are evaluated. Analytical expressions of the spatial fluctuation spectra are derived in each case. These theoretical results are compared to particle-in-cell simulations, showing a good reproduction of the subluminal fluctuation spectra.
Nonlinear dynamics of the ion Weibel-filamentation instability: an analytical model for the evolution of the plasma and spectral properties
C. Ruyer,L. Gremillet,A. Debayle,G. Bonnaud
Physics , 2015, DOI: 10.1063/1.4913651
Abstract: We present a predictive model of the nonlinear phase of the Weibel instability induced by two symmetric, counter-streaming ion beams in the non-relativistic regime. This self-consistent model combines the quasilinear kinetic theory of Davidson et al. [Phys. Fluids 15, 317 (1972)] with a simple description of current filament coalescence. It allows us to follow the evolution of the ion parameters up to a stage close to complete isotropization, and is thus of prime interest to understand the dynamics of collisionless shock formation. Its predictions are supported by 2-D and 3-D particle-in-cell simulations of the ion Weibel instability. The derived approximate analytical solutions reveal the various dependencies of the ion relaxation to isotropy. In particular, it is found that the influence of the electron screening can affect the results of simulations using an unphysical electron mass.
Collisionless shock formation, spontaneous electromagnetic fluctuations and streaming instabilities
A. Bret,A. Stockem,F. Fiuza,C. Ruyer,L. Gremillet,R. Narayan,L. O. Silva
Physics , 2013, DOI: 10.1063/1.4798541
Abstract: Collisionless shocks are ubiquitous in astrophysics and in the lab. Recent numerical simulations and experiments have shown how they can arise from the encounter of two collisionless plasma shells. When the shells interpenetrate, the overlapping region turns unstable, triggering the shock formation. As a first step towards a microscopic understanding of the process, we analyze here in detail the initial instability phase. On the one hand, 2D relativistic PIC simulations are performed where two symmetric initially cold pair plasmas collide. On the other hand, the instabilities at work are analyzed, as well as the field at saturation and the seed field which gets amplified. For mildly relativistic motions and onward, Weibel modes govern the linear phase. We derive an expression for the duration of the linear phase in good agreement with the simulations. This saturation time constitutes indeed a lower-bound for the shock formation time.
Probing the interstellar medium of NGC1569 with Herschel
Sophia Lianou,Pauline Barmby,Aurelie Remy-Ruyer,Suzanne C. Madden,Frederic Galliano,Vianney Lebouteiller
Physics , 2014, DOI: 10.1093/mnras/stu1770
Abstract: NGC1569 has some of the most vigorous star formation among nearby galaxies. It hosts two super star clusters (SSCs) and has a higher star formation rate (SFR) per unit area than other starburst dwarf galaxies. Extended emission beyond the galaxy's optical body is observed in warm and hot ionised and atomic hydrogen gas; a cavity surrounds the SSCs. We aim to understand the impact of the massive star formation on the surrounding interstellar medium in NGC1569 through a study of its stellar and dust properties. We use Herschel and ancillary multiwavelength observations, from the ultraviolet to the submillimeter regime, to construct its spectral energy distribution, which we model with magphys on ~300pc scales at the SPIRE250 {\mu}m resolution. The multiwavelength morphology shows low levels of dust emission in the cavity, and a concentration of several dust knots in its periphery. The extended emission seen in the ionised and neutral hydrogen observations is also present in the far-infrared emission. The dust mass is higher in the periphery of the cavity, driven by ongoing star formation and dust emission knots. The SFR is highest in the central region, while the specific SFR is more sensitive to the ongoing star formation. The region encompassing the cavity and SSCs contains only 12 per cent of the dust mass of the central starburst, in accord with other tracers of the interstellar medium. The gas-to-dust mass ratio is lower in the cavity and fluctuates to higher values in its periphery.
Wavy regimes of film flow down a fibre
Christian Ruyer-Quil,Serafim Kalliadasis
Physics , 2011, DOI: 10.1103/PhysRevE.85.046302
Abstract: We consider axisymmetric traveling waves propagating on the gravity-driven flow of a liquid down a vertical fibre. Our starting point is the two-equation model for the flow derived in the study by Ruyer-Quil \emph{et al.} [\emph{J. Fluid Mech.} {\bf 603}, 431 (2008)]. The speed, amplitude and shape of the traveling waves are obtained for a wide range of parameters by using asymptotic analysis and elements from dynamical systems theory. Four different regimes are identified corresponding to the predominance of four different physical effects: Advection by the flow, azimuthal curvature, inertia and viscous dispersion. Construction of the traveling-wave branches of solutions reveals complex transitions from one regime to another. A phase diagram of the different regimes in the parameter space is oferred.
Quantifying the Heating Sources for Mid-infrared Dust Emissions in Galaxies: The Case of M 81
Nanyao Lu,G. J. Bendo,A. Boselli,M. Baes,H. Wu.,S. C. Madden,I. De Looze,A. Rémy-Ruyer,M. Boquien,C. D. Wilson,M. Galametz,M. I. Lam,A. Cooray,L. Spinoglio,Y. Zhao
Physics , 2014, DOI: 10.1088/0004-637X/797/2/129
Abstract: With the newly available SPIRE images at 250 and 500 micron from Herschel Space Observatory, we study quantitative correlations over a sub-kpc scale among three distinct emission components in the interstellar medium of the nearby spiral galaxy M 81 (NGC 3031): (a) $I_{8}$ or $I_{24}$, the surface brightness of the mid-infrared emission observed in the Spitzer IRAC 8 or MIPS 24 micron band, with $I_8$ and $I_{24}$ being dominated by the emissions from Polycyclic Aromatic Hydrocarbons (PAHs) and very small grains (VSGs) of dust, respectively; (b) $I_{500}$, that of the cold dust continuum emission in the Herschel SPIRE 500 micron band, dominated by the emission from large dust grains heated by evolved stars, and (c) $I_{{\rm H}\alpha}$, a nominal surface brightness of the H$\alpha$ line emission, from gas ionized by newly formed massive stars. The results from our correlation study, free from any assumption on or modeling of dust emissivity law or dust temperatures, present solid evidence for significant heating of PAHs and VSGs by evolved stars. In the case of M 81, about 67% (48%) of the 8 micron (24 micron) emission derives its heating from evolved stars, with the remainder attributed to radiation heating associated with ionizing stars.
The molecular gas reservoir of 6 low-metallicity galaxies from the Herschel Dwarf Galaxy Survey: A ground-based follow-up survey of CO(1-0), CO(2-1), and CO(3-2)
D. Cormier,S. C. Madden,V. Lebouteiller,S. Hony,S. Aalto,F. Costagliola,A. Hughes,A. Rémy-Ruyer,N. Abel,E. Bayet,F. Bigiel,J. M. Cannon,R. J. Cumming,M. Galametz,F. Galliano,S. Viti,R. Wu
Physics , 2014, DOI: 10.1051/0004-6361/201322096
Abstract: We aim to quantify the molecular gas reservoir in a subset of 6 low-metallicity galaxies from the Herschel Dwarf Galaxy Survey with newly acquired CO data, and link this reservoir to the observed star formation activity. We present CO(1-0), CO(2-1), and CO(3-2) observations obtained at the ATNF Mopra 22-m, APEX, and IRAM 30-m telescopes, as well as [CII] 157um and [OI] 63um observations obtained with the Herschel/PACS spectrometer in the 6 galaxies: Haro11, Mrk1089, Mrk930, NGC4861, NGC625, and UM311. We derive molecular gas mass from several methods including the use of the CO-to-H2 conversion factor Xco (both Galactic and metallicity-scaled values) and of dust measurements. The molecular and atomic gas reservoirs are compared to the star formation activity. We also constrain the physical conditions of the molecular clouds using the non-LTE code RADEX and the spectral synthesis code Cloudy. We detect CO in 5 of the 6 galaxies, including first detections in Haro11 (Z~0.4 Zsun), Mrk930 (0.2 Zsun), and UM311 (0.5 Zsun), but CO remains undetected in NGC4861 (0.2 Zsun). The CO luminosities are low while [CII] is bright in these galaxies, resulting in [CII]/CO(1-0)>10000. Our dwarf galaxies are in relatively good agreement with the Schmidt-Kennicutt relation for total gas. They show short molecular depletion time scales, even when considering metallicity-scaled Xco factors. Those galaxies are dominated by their HI gas, except Haro11 which has high star formation efficiency and is dominated by ionized and molecular gas. We determine the mass of each ISM phase in Haro11 using Cloudy and estimate an equivalent Xco factor which is 10 times higher than the Galactic value. Overall, our results confirm the emerging picture that CO suffers from significant selective photodissociation in low-metallicity dwarf galaxies.
Asymptotic heat transfer model in thin liquid films
Marx Chhay,Denys Dutykh,Marguerite Gisclon,Christian Ruyer-Quil
Physics , 2015,
Abstract: In this article, we present a modelling of heat transfer occuring through a liquid film flowing down a vertical wall. This model is formally derived thanks to asymptotic developpment, by considering the physical ratio of typical length scales of the study. A new Nusselt thermal solution is proposed, taking into account the hydrodynamic free surface variations and the contributions of the higher order terms in the asymptotic model are numerically pointed out. The comparisons are provided against the resolution of the full Fourier equations in a steady state frame.
The Herschel Virgo Cluster Survey. XVIII. Star-forming dwarf galaxies in a cluster environment
M. Grossi,L. K. Hunt,S. C. Madden,T. M. Hughes,R. Auld,M. Baes,G. J. Bendo,S. Bianchi,L. Bizzocchi,M. Boquien,A. Boselli,M. Clemens,E. Corbelli,L. Cortese,J. Davies,I. De Looze,S. di Serego Alighieri,J. Fritz,C. Pappalardo,D. Pierini,A. Rémy-Ruyer,M. W. L. Smith,J. Verstappen,S. Viaene,C. Vlahakis
Physics , 2014, DOI: 10.1051/0004-6361/201424866
Abstract: To assess the effects of the cluster environment on the different components of the interstellar medium, we analyse the FIR-submm properties of a sample of star-forming dwarf (SFD) galaxies detected by the Herschel Virgo Cluster Survey (HeViCS). We determine dust masses and dust temperatures by fitting a modified black body (MBB) function to the spectral energy distributions (SEDs). Stellar and gas masses, star formation rates (SFRs), and metallicities are obtained from the analysis of a set of ancillary data. Dust is detected in 49 out of 140 optically identified dwarfs covered by the HeViCS field; considering only dwarfs brighter than $m_B$ = 18 mag, this gives a detection rate of 43%. After evaluating different emissivity indices, we find that the FIR-submm SEDs are best-fit by $\beta$=1.5, with a median dust temperature $T_d$ = 22.4 K. Assuming $\beta$=1.5, 67% of the 23 galaxies detected in all five Herschel bands show emission at 500 $\mu$m in excess of the MBB model. The excess is inversely correlated with SFR and stellar masses. To study the variations in the global properties of our sample due to environmental effects, we compare the Virgo SFDs to other Herschel surveys, such as KINGFISH, the Dwarf Galaxy Survey (DGS), and the HeViCS bright galaxy catalogue (BGC). We explore the relations between stellar mass and HI fraction, specific SFR, dust fraction, gas-to-dust ratio over a wide range of stellar masses. Highly HI-deficient Virgo dwarf galaxies are mostly characterised by quenched star formation activity and lower dust fractions giving hints for dust stripping in cluster dwarfs. However, we find that the fraction of dust removed has to be less than that of the HI component. Since the Virgo SFDs are likely to be crossing the cluster for the first time, a longer timescale might be necessary to strip the more centrally concentrated dust distribution.
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